Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México

Alvarez-Meraz, R.; Nagel, E.; Rendon, F.; Barragan, O. PLANETARY INFLUENCE IN THE GAP OF A PROTOPLANETARY DISK: STRUCTURE FORMATION AND AN APPLICATION TO V1247 ORI Revista Mexicana de Astronomía y Astrofísica, vol. 53, núm. 2, octubre, 2017, pp. 275- 307 Instituto de Astronomía Distrito Federal, México

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How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México eit eiaad srnmı Astrof´ısica Astronom´ıa y de Mexicana Revista t,Gaaut,Go320 M´exico. 36240, Gto Guanajuato, ato, ,115Trn,Italy. Torino, 10125 1, iktpsso asaceinrt notestar Both the onto 2012). rate al. accretion about mass et hot of a Nagel show from 2005; types emission al. disk thin et (Calvet their optically dust in with al. holes well- parts et have the Kim which inner to 2010; disks, complementary star transitional 2007, are known al. the disks These et near (Espaillat dust 2013). gap hot a show thick and they optically disks; of pre-transitional emission as classified been LNTR NLEC NTEGPO RTPAEAYDISK: PROTOPLANETARY A OF GAP THE IN INFLUENCE PLANETARY 1 2 eetyanwtp fpoolntr ik has disks protoplanetary of type new a Recently eatmnod srnmı,Uiesddd Guanaju- de Astronom´ıa, Universidad de Departamento iatmnod iia nvri´ iTrn,vaP Giuria P. via Universit´a Torino, Fisica, di di Dipartimento TUTR OMTO N NAPIAINT 14 ORI V1247 TO APPLICATION AN AND FORMATION STRUCTURE ≈ 10 − τ h ik hi assadszs ihnotcldphrange depth optical within dus sizes, of and number the masses extract their to disk, order the in disk protoplanetary a in y elsetutrsd ov nitrao epouddd´op profundidad de intervalos en polvo de el estructuras extraer para las protoplanetario, de disco un en embebidos rios SE the explains which structures. system of planetary observations a interferometric st of with the model of a i information to the available evolutio of leading the ranges faster using depth run a optical was different allows simulation the planets for of radius optica number Hill for the the effects in time structur increase slower massive an to of corresponds rate creation accretion the mass in increase an implies o nsseapaeai u xlc aSDycnuracnl con concuerda y Words: SED Key la no explica que que Ori, planetario interferom´etricas. V1247 sistema estelar un sistema con el para plan simulaci´on los ad-hoc el ´opticas de profundidades en el de intervalos estructuras en distintos efec las incremento evoluci´on m´as a r´apida de una un e corresponde permite creaci´on (3) de planetaria de masa ´opticamente delgadas; tasa acreci´on de estructuras la baja en una incremento (2) un implica planetas de 10 ≥ .INTRODUCTION 1. τ .Tesuyo h tutrssos 1 nices ntenu the in increase an (1) shows: structures the of study The 2. ≥ o10 to .E sui elsetutrsmetaqe 1 nincremen un (1) que: muestra estructuras las de estudio El 2. epeetasto yrdnmclmdl fapaeaysyst planetary a of models hydrodynamical of set a present We rsnao ncnut emdlshdoi´mcspr si hidrodin´amicos para modelos de conjunto un Presentamos − .Alvarez-Meraz R. 8 M crto,aceindss—hdoyais—paesadsa and disks planets protoplanetary — — hydrodynamics formation — disks accretion accretion, ⊙ / eevdOtbr1 06 cetdJn 92017 29 June accepted 2016; 11 October Received r(avte l 2002, al. et (Calvet yr 1 .Nagel E. , , 53 ABSTRACT RESUMEN 7–0 (2017) 275–307 , 1 .Rendon F. , u otepeec fpaesi h ne regions inner the in planets of presence the these to that due perturbations gravitational suggest by produced observations are patterns Their disk transitional 100546. the HD of patterns spiral multiple show ta.20;Lgag ta.21) htmti ob- Photometric 2010). (Chauvin al. with disks et servations in Lagrange 2005; gas al. and et dust through the is of formation observations of mechanisms possible their or al. et Quanz 2011; 2010; al. al. et gaps et 2013). Espaillat (Andrews or 2009; AU holes al. of et with 2008; Brown tens regions 2007, around and al. sizes 2007), et with al. Espaillat et 2014; al. Najita et Close 2005; nidrc a oifrtepeec fplanets of presence the infer to way indirect An 1 n .Barragan O. and , tsitro.S corri´o una Se internos. etas s 2 oe planetary lower a (2) es; nrpaes nad-hoc An planets. nner ´ mr,ms tama˜no y n´umero, masa s la ytmV27Ori, V1247 system ellar l hnsrcue;(3) structures; thin lly tica ai eHl aalos para Hill de radio τ Gemini tutrsfre in formed structures t ftesrcue in structures the of n ≤ ´ mr eplanetas de n´umero lv nmodelo un a lleva s o ´slno para m´as lentos tos tutrsmasivas; structuras n sconsistent is and D 0 τ . ,0 5, ≤ sobservaciones as oe ln´umero el en to tmsplaneta- stemas bro planets of mber 0 . membedded em . yBcaet ta.(2013) al. et Boccaletti by ,0 5, 5 1,2 τ< < . 5 tellites: τ< < and 2 2 275 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México h neato ftepaesi h ika h re- the as disk the propose in and planets cavities the the of in interaction material the hidden of lem gas. and dust restrict well-coupled which consider (2011), al. to same et us the Zhu use we as algorithm, conditions our initial test To cavity. the structure each in for the (SED) calculate distribution for to energy able area spectral is and algorithm Our density ex- mass, structure. each of we contribution simulations, hydrody- the the in tract From ranges depths simulations. optical namical protoplanetary set several the a in for run structures we disks detect planets, to immersed models in to of and, due in- material disk disk of the the configuration side the of describe regions to thick general, optically in terial disk hide can regions sug- material. thick environment, optically thin the optically that an struc- gesting in gap live thick can optically tures the Particularly, thin optically thick. be or can currents Salyk the & that optically showed Dodson-Robinson (2011) structures an disk. and These inner filaments) residual thick (like gap. for- currents the the of in induces consist structures system of planetary mation con- the they that hole; studied the cluded inside (2011) structures Jupiter Salyk of 2 formation & of the order Dodson-Robinson the of mass masses. inside a material with by asymmetry explained the be the directions. can of (20%), azimuthal component emission asymmetrical and the radial that found the They as in described sur- Gaussian vortex mass a steady-state variable a al. with a density, They et including face 21. cavity Perez SR the and 206462 modelled SAO planets. disks by transitional the in cleared asymmetries point- cavity found and (2014) a photoevaporation, to gas ing by cannot behaviour explained this be that suggesting with cavities, 48 dust IRS Ophiuchus of ALMA cavity the cavity.servationally the of existence 1:100, the explain value, to standard order of the in orders than 3 be smaller con- must magnitude ratio who dust-to-gas (2011), was the al. that problem et cluded This Zhu by addressed accretion. disks previously planetary pre-transitional and through cav- transitional is the explain in to way region hypothetical feasible ity A by gap. perturbed the Ori, is in V1247 planets gas of the region suggest gap which the in asymmetries solved South 7 LAE-EA,E AL. ET ALVAREZ-MERAZ, the Using ferometer disk. the of 276 umrzn,i hswr eadesteprob- the address we work this in Summarizing, ma- hidden of problem the address to order In ob- resolved (2014) al. et Bruderer recently, More and , hyfudgssrcue niete2 AU 20 the inside structures gas found They . the , IRTF ekInterferometer Keck ru ta.(03 ptal re- spatially (2013) al. et Kraus , eyLreTlsoeInter- Telescope Large Very ALMA , Keck-II bevtosof observations , Gemini In eso h eut.In results. the show we yaia oefrpaeaymigration planetary for code dynamical step of first modelling. a analysis their as detailed face systems a observed to of in structure and handy disk the gap, very the shows the become in clearly will immersed that it structures study the of preliminary all richness of a However, sample is small system. the this a for just configurations is possible set the spectrum. this and that mass realize size, We char- their that system: information the the planetary acterizes obtain embedded to an aiming with system, disk of protoplanetary simulations hydrodynamical a initial of the set present a we for section, counter- conditions this a In have SED. not the in do part they kind when this even inside extract structures, hidden of is to that able material of is amount From the one spectrum. material simulation the this hydrodynamical to that contribution a sense a the have in not dust, does and able is gas structure hide thick thick- to optically optical surroundings. an its particular its in by ness; to characterized lower is respect clearly A structure with a Each structure. with density of region larger lot a or a as planets, with defined the is produced of structure is proximity gap the larger of a overlap- because are there gaps when al. ping that et each hypothesize Crida We around 1986; Papaloizou 2006). gap & a (Lin creates orbit planetary disk protoplanetary a in tla ytmV27Oi(ru ta.21) In 2013). the al. et of (Kraus SED Ori a V1247 the and system explain model stellar to disk these a configuration to describe propose planetary associated we we spectrum Finally, Also, a structures. extract factor. to filling masses method the their a structures, and of sizes, number and the simula- formed as the each such inside gap, For structures the characterize we system. tion planetary with embedded disk an protoplanetary a of simulations dynamical odto sawy aifid nobtladvection orbital An satisfied. time-step always the (CFL) is Courant-Friedrichs-Lewy in increase condition the centre to radius, order with each In upwind mesh at Leer primary. staggered van fixed 2D a a a uses on code algorithm This 2000). (Masset follows: as organized is In creating paper This and gaps inside. structures opening for mechanism sponsible asadsrcue.In structures. and gaps 3 § § u iuain r eeoe ytehydro- the by developed are simulations Our embedded system planetary a of presence The http://fargo.in2p3.fr epitotteconclusions. the out point we 5 eitouetepoolntr ik with disks protoplanetary the introduce we 1 .METHODOLOGY 2. § § epeettediscussion. the present we 4 epeetasto hydro- of set a present we 2 FARGO § 3 3 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México asadteds icst.Teeprmtr are criteria: parameters general These following the viscosity. in planetary disk included the the thickness, disk and to affect the mass that According are parameters shapes main gap (2011). the the the al. (2006), choose al. et we et Zhu done, Crida in be analysed can carved system cases gap a planetary inside a structures by of formation the of sis fastest the (2005)). is al. FARGO et codes, Val-Borro the de among SPH (see that and note equations We based (34) 1992). and grid Norman (33) & the Stone (see of order second viscos- of artificial ity an contains the uses in The and code implemented equations is The Navier-Stokes auto-gravity. which tensor 0.5. to stress at viscous subject the fixed not is is number gas Courant central The a of are star. potential planets gravitational and the Navier- by Disk influenced the disk protoplanets. solves Keplerian embedded a code with for equations The continuity and Stokes one magnitude. by of time order required This the manual. decreases Objects’ implementation Gaseous Rotating Ad- in ‘Fast numerical vection FARGO the follows procedure reduce The to diffusivity. implemented ra- been each has at velocity dius azimuthal average the on scheme ei Atmwc ta.19) ntefis term, first the In cri- 1994). viscous-gravitational al. H a et is is (Artymowicz term term teria 1997), left left al. second first et (Ward the the criteria where thermal-gravitational formation, a gap the for lntpsto,and position, planet ai ewe h lntr n tla as and mass, stellar and planetary ℜ the between ratio ohmcaim.Fo h iuain eextract we of simulations contribution the the by From the shaped mechanisms. close is both to gap tries the viscosity Then, disk gap. the However, planetary the the around orbit. with region the interaction sweeps gravitational material disk its the form because to planetary necessary gap, parameter The relevant the opening. is mass gap mech- two the the influencing the affect anisms think and strongly We parameters planets planets. these the of that by accreted number matter the of amount are simulations of eimjrai,Ω axis, semi-major term, second the in while planet, the of dius = stetikeso h ikand disk the of thickness the is nodrt en e fcssi hc nanaly- an which in cases of set a define to order In h w anprmtr hnigi h set the in changing parameters main two The a 2 Ω p 2.1.1 /ν steRyod ubr(where number Reynolds the is yrdnmclSimulations Hydrodynamical . 2.1 4 3 p R H ν h Models The . H steaglrvlct tthe at velocity angular the is steknmtcviscosity). kinematic the is TUTR OMTO NPOOLNTR IK 277 DISKS PROTOPLANETARY IN FORMATION STRUCTURE + q 50 ℜ ∼ < 1 , R H h ilRa- Hill the a q sthe is sthe is (1) opouedee as eol osdrmodels consider order only we in gaps, (8) the (7) deeper zero; code; produce is the to in eccentricity time used N- any planetary order at Runge-Kutta initial fifth of are the solver orbits Body with their calculated and influ- consistently other planets planets the each with resonance), ence configuration 2:1 approximately stable in a with migration (initially planetary for allowing respectively, AU case, 5/7.5/12.5/20 each and 7.5/12.5/20 12.5/20, axis M where dΣ respectively) rate planet, the a of at axis semi-major the and 0 ih2 ,ad4paesaecniee ihan with considered are 0 planets of 4 mass and initial 3, 2, with § rto sprmtie ytedmninesaccre- dimensionless parameter the timescale by tion parametrized is cretion 0,frwihtemtra fteds sdepleted is disk ( the radii of Hill material 0.45 the inside which for 100, where uye 93,wt naceinselrrate stellar accretion an with 10 1973), Sunyaev & ag rm07 o20A,rsligi asof mass a in resulting AU, 200 to 0.025 0.75 from range sume a aso 1 of mass lar ial steml is isothermal) tically ltosae 1 h iksraedniyprofile density surface disk 178( the = (1) Σ are: ulations of efficiency time code. the computa- the decreases more terms and implies more resources solution tional when their code included, the are by solved equations the h ikapc ai is ratio aspect disk the ie o oicuete.Ti ilb commented be will de- This we in them. Thus, below include gap. to the not about cided in conclusions behaviour the structures’ change that the not found we will However, inclusion must mesh. the star the of the center which the for at frame, be acceler- reference an the causes of inclusion ation the Their in simulations. included of not set are cells) and be- gravitational planets/star interaction the tween gravitational Zhu of by emulate terms (produced indirect to potential the order (2011), In al. in et Ori. Finally, V1247 system planet. stellar closest the relationship of § their position and the gap, or with merger the their into structures, the fragmentation of mass, spectra the size, of radial behaviour typical the about information . 45 .. eso na-o iuae oe o the for model simulated ad-hoc an show we 2.1.6 p nZue l 01.()paeaysystems planetary (6) 2011). al. et Zhu in 3 − , h aaeesdfiigtestpfrtesim- the for setup the defining parameters The 8 − M M α M 0 ∗ T h ⊙ 0 = . p ⊙ and 75 § yr stehih cl;()tepaeayac- planetary the (5) scale; height the is 3 h ailtmeauepol (ver- profile temperature radial the (3) ; r/ stepro ttepae oiin(see position planet the at period the is ..Fo h ueia on fve of view of point numerical the From 3.4. − . R 1frtevsoiyprmtr(Shakura parameter viscosity the for 01 AU) 1 r H / p d nsed tt,adacnrlstel- central a and state, steady in r h lntms,teselrmass stellar the mass, planet the are t tart dΣ rate a at − M = . 1 1 (0 ⊙ M − 2 h ikhsaradial a has disk the (2) ; . J 2 01 R T n niiilsemi-major initial an and , π/ H /α f (f 221( = ( = h/r cm g ) T ihtevle ,1 and 10 1, values the with p Σ n nterange the in and )Σ, M / 0 = p d / r/ t − 3 M AU) 2 = . hr eas- we where , 029( ∗ − ) 1 − 2 / π/ 1 3 r/ / r 2 (3f p AU) where , ;(4) K; T p 0 )Σ, . 25 , © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México 7 LAE-EA,E AL. ET ALVAREZ-MERAZ, resolution used The (9) (N is accretion; planetary with 278 norcs,we ehv elfre a,the (0 gap, Radii well-formed Hill a the have inside cells we of when planet. number the case, to our close distribution In characteri- matter fully the a of require Benitez- zation process we of the when of relevant version modelling highly 3D 3D in is A new Now, is (2016). the al. version et FARGO that Llambay model. 2D faster 2D the times the efficiency, 7 time in of structures neglected terms the plan- be the in can for changes that model produces 3D last accretion a the etary than including smaller that magnitude such scale of value a order in an occur least process dynamics accretion at the The changes process. that the (that of height), direction is the vertical there on the latter depends in the in component and velocity mid-plane velocity a the radial the all specific in a former accreted at the and in concentrated is that plan- mass is 3D few models and a 2D accretion of between etary gap difference main a The in formed AUs. we structures because in effects interested 3D account are into take not does tion dis- logarithmically spaces radial of tributed. number N the and is distributed, arithmetically spaces azimuthal ac) rais(bnac 0 (abundance organics dance), ldt h a.Teds scomposed is where dust The orthopyroxeno, + (olivine gas. silicates 0 the of to pled amount. small some a of by shape only exact planetary the structures ac- another change planetary will including This model where Thus, accretion AUs. value few the occurs. a than cretion of larger disk order is the the value of with scales structures interaction spatial of planetary over description the the is by paper formed Summarizing, the of resolution. aim higher the rele- of circum- be disks of could simulations planetary 22-24) in applications Figures resolution future the for the vant (like with paper Radii this Hill the of of the estimate in an mass However, relevantaccreting description. not 3D is a plane- it use Thus, the to included. on not are impinge produced surface material the tary by the heating when dust radiation as such phys- of Besides, processes scale occurs. ical spatial accretion typical the where the simulations region describe the the to of enough resolution not the is Thus, quantification area). the the for of procedure numerical the state we 20 tween . 06 0 + 00264 h aaerzdagrtmfrpaeayaccre- planetary for algorithm parametrized The h uti sue ob elcou- well be to assumed is dust The φ , N r − (384 = ) 2.1.2 . 0frteue eouin(in resolution used the for 40 07 0 = 00077 hrceitc fDust of Characteristics . , 5) hr N where 256), . 04i h oa abun- total the is 0034 . φ 0)adtriolite and 001) stenme of number the is . 7 § R ..,we 2.1.5, H sbe- is ) r hc eieo h itr fds n a.Note 10 gas. at and opacity dust the of take mixture we the that of regime thick consider We and respectively. τ intermediate emission, thin, thick optically optically to corresponding a.Ormdlcniessalds riswt a with grains the dust to small size considers relative minimum model abundance Our 0.005168 gas. a to amounts audne0 (abundance soitdt ieetrne fotcldph(see depth optical structures of the 1). ranges find way.Figure different to iterative to used an are associated in steps structures following the The find to proceed the proceeds. and spectrum structures the of of search calculation the how reference. show as we do wavelength Below another conclusions use main we Our if change depth. not optical dust the for tutrs a h ffc fcagn h physical the changing of thick effect optically the the has (particularly structures) material distri- new of uniform the bution an However, with parameter. simulation viscosity alpha a from come algorithm r Mti ta.17) hc orsod oamean a to corresponds which 1977), opacity al. et (Mathis ic MN ri iedsrbto d distribution size grain (MRN) sieck pia depth: optical d .W nls h egbuho fflge cells. flagged of neighbourhood the analyse We 3. a with identified is cell hydrodynamical Each of 2. output specific a choose We Selection. Case 1. .W rn h tutrsit niiulfie in files individual into structures the print We 5. cells contiguous the all for 3 Step repeat We 4. , sacnevtv rniint h optically the to transition conservative a as 2 = max neteds pia et scaatrzd we characterized, is depth optical dust the Once entc httesrcue on sn this using found structures the that notice We ecluaeteds mso ihnarneof range a within emision dust the calculate We fanihorcl a h aernein range same the has cell neighbour a If interme- thin, optically structure. thick an or of diate member a as flag simulation. hydrodynamical the re ocutte n oka rprislike properties mass. at and look size and radial them count to order the of structures ‘the name will of disk’. blocks we form op- that procedure three cells This the for bins. cells, depth pro- unflagged tical the the repeat all we same for Next cess the depth. share optical which in structure range forming the of structure. a of member a as flagged be will it 0 = κ ≈ 2.1.3 . 25 9 . µ . cm 6 078 Plake l 94.This 1994). al. et (Pollack 000768) r h erho Structures. of Search The . ,wt ahs up n Nord- and Rumpl Mathis, a with m, τ d , min ≤ 2 0 g 0 = . − ,0 5, 1 . t10 at 005 . 5 < τ < µ n aiu size maximum and m µ µ m. sorreference our as m 2 . n/ and 0 d r d ∝ τ τ ≥ r then − 2 3 . . 0 5 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México software/radmc-3d/ ot al aitv rnfrcode transfer radiative Carlo Monte in)frec tutr dnie ytealgorithm the by in identified described structure each for tions) viscosity. al. reduced et a (Martin embed- to zones’ to due ‘dead 2012) (due means become formed can This structures planets) ded the turbulence. of created some the that viscos- insta- to non-homogeneous rotational related a magneto ionization ity define the of will (MRI) degree and bility the places change these will in This heat- the reduce rate. will ing cases some in which conditions, ulmn oii 04.W rce sfollows: as proceed We 2004). in Dominik & based Dullemond is which prep, in (Dullemond i.1 iga o h trtv erho structures. of search iterative the for Diagram 1. Fig. .W hneclswt ufc est Dt a to 2D density surface a with cells change We 1. 4 nodrt e pcrm(rmte2 simula- 2D the (from spectrum a get to order In http://www.ita.uni-heidelberg.de/ ob sdby used be to ukdensity bulk Σ( density sur- face from conversion The 3D. density volumetric oigses is,w loaetebl density bulk the allocate we First, steps. lowing 2.1.4 § ..,w opeteagrtmwt the with algorithm the couple we 2.1.3, h tutr Spectrum Structure The . ρ RADMC-3D ( ,φ R, ,θ φ θ, r, TUTR OMTO NPOOLNTR IK 279 DISKS PROTOPLANETARY IN FORMATION STRUCTURE n2 oa oriae to coordinates polar 2D in ) nshrclcoordinates spherical in ) smd ytefol- the by made is ~ dullemond/ RADMC-3D RADMC-2D 4 hl h lntpsto is position planet the while vlae ihthe with evaluated the of borders where iue 22)b pia et ag acrigto (according range depth § (see optical contribution After by mass 22-24) Radii. their Figures Hill determine can the we inside that, areas grid the calculate r we h elpsto n h lnt h mean The be- planet. distance the the is: and is position position cell inequality cell the the of tween part left The etk h u ftemasses the of sum the take we enposition mean ij 2.1.5 med r .W soit h tutrs(rvosyfound, (previously structures the associate We 4. .W aclt h ikeiso fc n i.e., on, (face emission disk the calculate We a 3. using by temperature disk the calculate We 2. 2.1.2). ne ntepae egbuho uhta their that such neighbourhood planet the in index ij o sn h odto ie neuto ,we 4, equation in given condition the using Now oetmt h asisd h ilRadius Hill the inside mass the estimate To ,i nteds ln,i.e. plane, disk the in where imation etclyiohra itiuinteequation is the distribution isothermal Considering vertically a midplane. the above density the for steds egt h egtsaei self- is simula- scale hydrodynamical height i.e., The the tions, with height. consistent disk the is urdb h supino etclyisother- (see vertically disk a mal of assumption the by quired ecie in described the in array an as file a space in pixel it save and lengths, 0 RADMC-3D. in routine pcr soito a ese nFgr 6. Figure in seen be A can spectra. association respective spectra their with them associate ( = siaeo h asIsd h ilRadius Hill the Inside Mass the of Estimate . ◦ ( = r nlnto)i h ieo ih o l wave- all for sight of line the in inclination) ij x ij r and y , i h +1 ij ρ stehih cl and scale height the is ( = ) r ( − r ij ,θ φ θ, r, ij i xy ρ h +1 r § ( | el h nl ln h el is cells the along angle The cell. satisfies: § ,π/ r, i 0 = r . j j ) ..)i ie pc,i re to order in space, pixel in 2.1.3) r ij 2.1.1). / med ne as index r h ne n ue radial outer and inner the are sterda endistance, mean radial the is 2 = ) − . 029( 2 ,i φ , r p cos( ρ θ | ( = ) r/ ,π/ r, R < = φ AU) φ π/ r j (2 j Σ( m p ) H 2 (( = r , π ,wt h approx- the with 2, φ , . ij 1 ,θ R, ( = ) med . 1 25 ) fteclswith cells the of / e j 2 hc sre- is which , − ) ,i h +0 x 2 z sin( , z p h 2 y , 2 . = 5) , φ p /N .The ). j r )) cos( φ , )2 R (5) (3) (4) (2) φ H π ) . , © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México el n h ra vlto ftegi rawti 0.7 within area grid the Right: of evolution planet. area, (inner) the outer and the cells of evolution the represent ftopaes sn he rdresolutions grid three using 3 planets, (until axis (N two semi-major the of of tion online. viewed be can figure color The resolution. grid by area n (448 and htti orei ebro the of member found a (2008) is Solano source & this Caballero sys- that stellar Ori. the V1247 of structures tem disk the analyze to tions nti gr otisteds assoni the in shown mass 22. area Figure dust the of the particular, plot contains In top-left figure used. this when is in in- change resolution appreciably area not better and do a axis reason- radius is Hill semi-major mass the the larger dust side that the is Notice of radius area. estimate Hill able. the the the and so inside 20, cells cells than of of number number the The of evolution the itneo 385 of distance a raisd h ilRadius the Hill of the check convergence inside a area presented is plot right the ta.21) sn h r-ansqec evolu- pre-main-sequence Kraus the 2003; re- Using al. been et has (Vieira 2013). it star A5III al. recently F0V an et a be 1971); as to al. thought classified et was (Schild it star Originally Myr. 10 i.2 et eimjrai vlto utl3 (until evolution axis Semi-major Left: 2. Fig. AL. ET ALVAREZ-MERAZ, 280 φ 2.1.6 h etpo nFgr hw h evolu- the shows 2 Figure in plot left The eapytemto ecie npeiu sec- previous in described method the apply We , N r yrdnmclMdlfrSrcue in Structures for Model Hydrodynamical . (384 = ) , 8) o o rd,itreit gen n ih(le re (blue) high and (green) intermediate (red), low for 384), , 5) (384 256), ± 5p n iha g f5- of age an with and pc 15 14 Ori V1247 , R 8)ad(448 and 384) H o hs ae,with cases, these for . ǫ 2 lse at Cluster × , . 8) In 384). 2 10 × 5 10 yrs) 5 r)frsvrlgi eouin;( resolutions; grid several for yrs) R H oprsnbtenaltersltosfrtenme of number the for resolutions the all between Comparison fteitro lnt n h ubro el ntegrid the in cells of number the and planet, interior the of etk aaeeso h rtpaeayds as disk protoplanetary the of 2008). Caballero parameters the 2007; to take al. distance et We (Terrell a pc assume 385 We of (2013). source al. et Kraus by hyas on htteds a niciainan- inclination an has disk around the gle that found also They asadage, and mass rbto nscales dis- on brightness tribution centro-symmetric a with consistent is uepae esrdby measured phases sure inr rcsfo rsa ta.(2012, as al. mass et the Bressan SEC from tracks tionary h netite of uncertainties the rmo h ik hc nldsa pial thin optically an includes spec- range which the the in disk, modeled gap the they of MIR, to trum NIR from obser- vations spectroscopic 2013). and al. interferometric et (Kraus Combining asymmetric disk the of inside evidence besides structures is because, density there method SED, sampled our well with a study a for quate ly sn pruemsigosrain nthe in observations masking aperture using ally, t K’ rgtesdsrbto nsae of scales on distribution brightness ∗ and , 7 = normdl eaottecluaino stellar of calculation the adopt we model, our In hsojc spriual neetn n ade- and interesting particularly is object This . ees 10,Kase l 21)estimate (2013) al. et Kraus V1.0), release 4 ouin epciey h pe lwr curves (lower) upper The respectively. solution, L’ ± 0 i ad,te bevdaymtisi the in asymmetries observed they bands, . Myr. 4 31 = M M ∗ ∗ ≈ 1 = ◦ 1 = .. ls oface-on. to close i.e., , < 0 ∼ . . 3 86 0ms( mas 30 . 87 5 − N ◦ ± φ 4A.Te on h clo- the found They AU. 44 AMBER M seterFgr ) which 2), Figure their (see N , 0 . ⊙ 02 r (384 = ) and < r M ⊙ 2A) Addition- AU). 12 t ∗ n h g as age the and , ob eowithin zero be to 7 = ≈ , 5) (384 256), 15 . 4 − × 10 0AU. 40 PAR- 6 , 384) yrs, H , © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México follows: 08) h ufc est lp ssteult one, to al. equal 104(AU set = et is Σ (Beckford slope i.e., density WL16 surface disk The resolved 2008)). the to up to 2013) similar al. et (Kraus AU a ≈ and 0.18 disk), from Tauri range T classical radial typical a from mass the sflos h ne ikmass disk disk the inner of the mass for total follows: condition pre- the as initial self-consistent divide we a an simulation make as the to model, order disk In structures the transitional the of gap. analyse to the degeneracy is in innate aim our the Here, planetary break observa- modeling. embedded to detailed the and constrain more system to require interpretation order We the in for tions object. scenario this possible of one formation just gap for the is parameters to the associated that system model out planetary the point consistent We number a pre- Ori. large obtain V1247 a to not for order run is in to simulations need system of would (2013). the we al. and of et Kraus dictable, evolution by Ori the V1247 gap, of However, formed model well the a in untilas maintaining disk and ‘seed’ the opening mass in finally small migrates and a matter as accretes would starts which scheme planet consistent each more that A imply formed. already is ikmass disk h oa aso h planets the of mass total the asis mass nteinrds ftesmltos,teotrdisk outer the simulations), the is of mass disk seen inner as magnitude the of in orders two by disk this depleted is τ odro U(5A) h asls yaClas- disk a pre-transitional by a lost (outer) become mass to inner is The disk AU). Tauri an (55 T has AU sical gap 2 of pre-formed border The sider). ensraedniyΣ=10 with = initially Σ density thin, surface optically mean the considered a planets, be with can simulations gap numerical to cording l ecnie htteselracee asand mass accreted are mod- stellar mass for these the planet effects In that total other consider considered. no we are by i.e., els material accreted star, the is the losing mass and depleted planets the the that assume We M pdi hswr.Tema tla crto rate accretion stellar mean The work. is devel- this simulations in hydrodynamical oped the with sistent aesmlfidt osatselraceinrate, accretion stellar constant a to simplified have gap p 0 U(ossetwt orespectroscopically source a with (consistent AU 500 h M M , M soriiilcniin easm httegap the that assume we condition, initial our As tot ˙ depleted gap 0 = acc 0 = M , M ∗ M 10 = . o h ri opsto htw con- we that composition grain the for 1 i disk M disk disk . = 9 = disk , in , − M M in 0 = M 2 2 = , acc depleted out π /r 2 = disk ((55AU) . cm g ) , h asi h gap the in mass the , π 2M 02 ∗ /t R − π 55AU system 100AU TUTR OMTO NPOOLNTR IK 281 DISKS PROTOPLANETARY IN FORMATION STRUCTURE R epciey hc scon- is which respectively, , M M 0 2AU ∗ . − acc 18AU disk 2 wihi ossetwith consistent is (which 2 . − , Σ ∗ ≈ , M in r (Σ ((2AU) − 0 = d p 10 − 2 r , / M tot n h a mass gap the and , cm g − 100) M . disk 10 h ne disk inner The . 1 gap 2 M M r , − cm g ) in d 2 − depleted ⊙ r h outer the , uhthat such , M yr M w have (we gap − − disk 1 2 We . and , , (ac- and out . nyrpeet2 ftettl oee,w ar- we However, total. the of % 23 represent only ihsm-ao axes semi-major with t ntetbewt eimjraxes semi-major with plan- nine table The the radii. in larger ets at planets that exist indicates normally pc) could rela- 7.7 a of at distance and short method tively image the by (detected AU 115 h bevtoso tr ihntems range, mass that the Note within stars gap. relaxed 1 of the AU) observations cover 41.9 the to to 2.6 required (from are planets (2:1) resonant tually in npriua,sbin tr ntems range mass the in stars 1 subgiant classifica- particular, last the In to tion. belong would Ori V1247 giants; rm05 o25 to 0.53 from ag nodrt rdc eae pial thin this optically choose relaxed we a (where produce AU from 55 to gap to order 2 in gap from range initial size The a exoplanets.eu). has systems in multiplanetary database the the to (see in belong planets asymmetries detected the creating ≈ for responsible Ori. like-V1247 stars around common be could aspae n atcewihi etre after 5 Jupiter perturbed is a is which between particle planet 10 a distance (last) and minimum planet first (outer) mass the the inner is and the This between border separation gap initial The n tr aea1 a have stars low-mass that M found and They with K which formation mass. (2007), planetary stellar of al. increasing efficiency et larger Johnson a by show studies by tivated al. et (Zhu resonances these 2011). in mutual located planets interactions show 2:1 planet-planet and simulations by planet-disk hydrodynamical including separated longer the are resonances; planets remaining tr n 8 and stars ec aecmae o4 to compared rate rence M Ori. the V1247 of of variability rate allow accretion 2013) stellar al. et (Kraus although hr the where n atpae,rsetvl.Wt hsi id we mind, relation in linear this a With assume respectively. planet, last and efida prxmt eainbtentemass as the defined between planets, relation neighbour approximate of an the find f=10 to parameter we for planetary inner simulations accretion the intermediate hydrodynamic an the (from From planets one). of outer number the bels . . 7 7 p 6 0A a fV27Oi culy 2 fthe of 22% Actually, Ori. V1247 of gap AU 40 , M h al hw htFmlatb(3 b Fomalhaut that shows table The epooeta utpaeaysse is system multiplanetary a that propose We h utpaeaycoc o 14 r smo- is Ori V1247 for choice multiplanetary The h oa aso l h lnt is planets the all of mass total The M tot r Ddo-oisn&Slk21) The 2011). Salyk & (Dodson-Robinson yrs ⊙ ⊙ = < < P ≈ α M M i N i to 2 . =1 9% aevle rm07t .,frtefirst the for 0.9, to 0.7 from values have < < m 1 ≈ ± . 1 M p,i 95 . 95 5A,atr10 after AU, 45 J 2 where , etikta agrplanets larger that think We . M . %frtehge assub- mass higher the for 9% M > a ⊙ ⊙ α hwnn asv planets massive nine show . aepaeswt masses with planets have 2% 2 i . 8% . 0 = U(e al 1). Table (see AU 5 i ± ± . 0 + 7 1 = . α %pae occur- planet 1% %frsolar-mass for 7% 4 i r) ee mu- Seven yrs). ≈ i (0 , 2 m . > a 2) N , . . . , p,i / ( /m N M 2 . p,i J − AU 5 at ) R +1 2). la- H . , © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México asrne .2ad1.76 simi- and the 1.72 noting stellar ranges and the mass between mind, frequency planetary in observed this lar and velocity With (radial diffi- star methods the transit). the successful from to distances most large the i.e., at by planets radii, bias find observational larger to culty to at due detection is against depletion this that gue AL. ET ALVAREZ-MERAZ, 282 n 1.91 and r ee lnt ntegp rmteinrto inner the are: From masses initial 0 and AU, gap. positions 2.6 their the there one, outer in that the planets found we seven above, are mentioned masses and be- is goal. issue present This our migration. yond (outer) inner bodies induce planetesimal whole can because the cover range, not can axes planets are semi-major the simulations how these show to However, enough model Ori. disk V1247 protoplanetary for the in embedded several with planets motivated simulations This hydrodynamic Kepler- develop 2011). 2016); to al. us al. et Lissauer et planets, Buchhave planets, (six 11 2012; (six Kepler-20 al. 2013); et al. Gautier planets, et et (seven Tuomi Mayor planets, 2009; Kepler-90 (six plan- al. 40307 plan- HD 2017); 2014); (seven (seven al. al. et TRAPPIST-1 219134 Schmitt et 2015); HD Gillon al. ets, 2011); et al. Vogt plan- ets, (seven et 10180 Lovis HD stars: ets, type around discovered late been and the have Sun-like Although the they uncertain, inside cases. is systems model real gaps multiplanet in of our exist process for formation do required Ori the range V1247 that radial for conclude the we de- in masses) planet planets stellar against low bias at observational tection the of spite in 04A,0 AU, 10.4 D153 . 2.28 4.6 b 145934 HD EIMJRAXIS SEMI-MAJOR D145 .62.58 5.36 c 154857 HD oahu 1 3 115 b Fomalhaut I 39 021 20 b 73990 HIP I 73 .520 2.55 [ Mass [AU] b axis 97233 HIP Semi-major name Planet I 39 222 32 c 73990 HIP eaPcb1.87 13.18 b Pic Beta D43 . 2.37 4.6 c 4732 HD pligtecniin o h lntresonance planet the for conditions the Applying FPAESHSE YSASWITH STARS BY HOSTED PLANETS OF 1Eib1 7 14 b Eri 51 M . ASSFO 1 FROM MASSES 2 ⊙ . M 53 smlrosre lntr frequency planetary observed (similar J . U 0 AU, 4.1 ; M J 66A,0 AU, 16.6 ; AL 1 TABLE > a . 31 2 M . . UADMASSES AND AU 5 7 M ⊙ − n ewe 1.90 between and , J . . U 0 AU, 6.6 ; 1 65 . 95 M M J ⊙ 64AU, 26.4 ; . 40 M M J ] J ; ayaccretion. tary mle httelte hneterobtlparame- orbital their change ters. planets latter the the is and that fact gas implies the the noteworthy between of interaction A evolution the that dynamical system. the planetary by inside immersed shaped formed gap structures the the physi- of and characterization geometrical cal the for relevant information ae h a lwymgae oad h tr For star. the towards three migrates the slowly In gap respectively. the disk, cases the in embedded ets ayb enfco f07/.509 uigthe during 0.79/0.85/0.92 3 of (until factor axes simulation mean semi-major a the by material; vary to disk due the move to with free torques radially sim- are the planets of The physics included ulations. the take in we account structures; leave into of them will formation effects the appreciably; These in imprints not below. their explained but be changes will planets this the the eccen- of to the simulation, joined tricity the is During gap longer planets. The time migrating timescale. a viscous over the star than the towards migrates slowly ltosdsrbdin described ulations optically an and gap. disk, an thin outer with and code, inner transfer thick radiative optically the in ran model we static simulations, a hydrodynamical the to mentary 0 21) ial eue qain n ocreate to the 2 and with 1 spectra equations al. the used et we Osorio in Finally 169142 HD (2014). of models the with patible xd h ytmi eae fe h rt10 first the after relaxed is system The fixed. rsrpinb h ta.21 iha accretion an with 2011 f=1) al. et parameter Zhu the by (with allowed prescription is accretion planetary Afterwards, r fti orei Devrnet eextrapo- we as environment, scale 3D height a the in lated source this of tra re- spaces, distributed, azimuthal spectively). arithmetically 256 and and radial logarithmically 256 in (with formation gap structure the possible because in AU, interested 100 were to 1 we from scale radial only the mesh considered hydrodynamical The FARGO). with of version simulations the ran FARGO3D we advantage putational . 76 5 fe h a omto,tepaeaysystem planetary the formation, gap the After nti eto epeetterslsfrtesim- the for results the present we section this In nodrt nls h oeldsrcue spec- structures modelled the analyse to order In h revrinof version free The 3.1 M h e fHdoyaia Simulations Hydrodynamical of Set The . J 19A,0 AU, 41.9 ; nis2 eu t eebeteold the resemble (to setup 2D its in , 5 ihagahccr o com- for card graphic a With . . 5 .RESULTS 3. . 85 FARGO-3D × RADMC-3D § M 10 .I atclr eshow we particular, In 2. J h 5 h eimjrae are axes semi-major The . r) o ,3ad4plan- 4 and 3 2, for yrs), 0 = . osnticueplane- include not does 5 r 1 . 3 hc scom- is which , oe Comple- code. 4 yrs. © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México h te ae where cases other the curve, solid planet the 4 and respectively. to dash-dotted, 3 and 2, correspond dashed for rate which accretion mass configurations, Stellar 3. Fig. f epciey oieta tti tg ftesimula- with the cases the of for stage only this tions, 0.5/0.75/0.9, at and that 0.62/0.8/0.93 Notice of respectively. factor mean a by ofiuaino ,3ad4paesadteaccretion the and planets 4 and 3 2, of configuration into 0.17. taking is simulations, planets, the the all for account eccentricity final mean . fudfrte4pae aewith case is 4-planet eccentricity the the for of value (found planetary largest 0.3 mean The lower planetary lower ei- a migration. a that imply or show parameter we planets of of (2011), accretion scope number al. larger the et dur- a Zhu beyond evolution ther in is As the disk fo- paper. a disk; the without work a stage This with the stage ing some the system. of on planetary escape cuses the the scat- in of planet resulting members work) the occur, this of in could included clearing tering into not the stage trapped During (a are disk planets resonances. all mutual most time 2:1 Over simulation simula- produced. the the not of of is span scattering time the planet by During tions, diminishes 0.78. cases axis of For semi-major factor mean a the environment. gap, thin a optically with an have not 0 (until 100 = iue3sosteselraceinrt o a for rate accretion stellar the shows 3 Figure × 10 6 r) h eimjrae vary axes semi-major the yrs), f TUTR OMTO NPOOLNTR IK 283 DISKS PROTOPLANETARY IN FORMATION STRUCTURE 0(ni 4 (until 10 = f 0 h aiydoes cavity the 100 = . 5 × f 10 ) the 1); = 5 r)and yrs) ufc est o h he agso pia depth optical of ranges three considered: the for density variation. surface any magnitude, suffer not of does orders disk external four the by and decreases region gap a.Tedniyo h ne ikdcessb two by decreases 3 disk at magnitude inner of the deeper orders of a density produces The planets of gap. number lower parame- a accretion and planetary the ter lower that a show of simulations combination the because example this 0 lntr parameter planetary online. viewed be can figure color The (2011). al. et Zhu o rd,rsetvl,fra crto lntr param- planetary dash-dot-dot- accretion eter an and (purple), for respectively, (green), dotted (red), dot (black), dash-dotted curve (blue), solid dashed the to correspond o h w-lntcs with case two-planet the for planets. the disk the restricts inner between the gap planets to the outer of through the number from circulation large This material a smaller. because order magnitude is order the an of is value configurations a reaches 10 system of 2-planet a for i.4 zmta engsdniya times at density gas mean Azimuthal 4. Fig. tla asaceinrt ihalwrnme of number lower a 3 with Until rate planets. accretion mass stellar ie 5 times al hc msin epciey ntecs ftwo of case 3 the at In planets respectively. opti- emission, and thick intermediate cally thin, optically to responding . 5 × iue5sosa xml fteaiuhlmean azimuthal the of example an shows 5 Figure iue4sostema zmta a density gas azimuthal mean the shows 4 Figure f − 10 10 ,ad2paes iia gr ssonin shown is figure similar A planets. 2 and 1, = × 5 1 , M 10 . ⊙ 0 4 × τ 1 , yr × 10 ≤ − 10 × 5 × 1 0 5 hl hto h -ad4-planet and 3- the of that while , 10 . r,w on httegpdensity gap the that found we yrs, 2 , ,0 5, 10 5 . 2 , 5 0 f . 5 r,teselraceinrate accretion stellar the yrs, × × .W aclt larger a calculate We 1. = < τ < 10 × 10 5 10 5 n 3 and , n 3 and 5 f r,wieta fthe of that while yrs, 2 tevolutionary at 1 = . and 0 . × 0 × 10 10 5 τ 5 r;w use we yrs; ≥ r,which yrs, 2 . t cor- 0 0, = © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México eil hl nytemtra fteinradouter and thick. inner optically the is of material disks the ma- only intermediate while and terial, thin optically by dominated is The online. viewed respectively. be can ranges, optically figure thick color to and dashed correspond intermediate (blue), (red), curve thin, solid dash-dotted The and in (green) depth. separated optical density surface of azimuthal ranges mean The 5. Fig. AL. ET ALVAREZ-MERAZ, 284 o lntr crto aaee qa o1at 1 to equal spectrum parameter the accretion the to 3 planetary contribution planets, their a two and for the disk structures of complex the of case in emission Fig- the the spectra, between for relation their shows, and 6 structures ure the of geometry it tutr ihamxmmvlei t SED its in value maximum interme- a of optically with an domi- structure found outer) We see and diate (inner can spectrum. disks We the the nate plus spectrum. star struc- the respective the that match their structures colors with The thick tures optically gap. the thick and inside optically disks, present two an con- the that gap, region nects op- intermediate a optically an an disk, has disk, outer which inner disk, thick pre-transitional tically a of ample ihamxmmof maximum a with w pial hnsrcue ihamxmmof maximum a with structures ≈ thin optically two lgtylre asde o ec aiu value maximum a 10 reach of not does mass larger slightly hs w pial hnsrcue aeads mass dust a have structures of thin optically two these × ≈ ≈ 10 nodrt iulz h eainbtenthe between relation the visualize to order In 10 − − 10 10 13 13 5 3.2 − − 11 r cm erg 4 r.W hwti aea odex- good a as case this show We yrs. r cm erg h ope tutr Emission Structure Complex The . M r cm erg ⊕ notclytiksrcuewt a with structure thick optically an ; − − 2 − 2 nisSED. its in 2 s s − ≈ − 1 1 ewl e in see will We . 8 notclyti structure thin optically an , × 10 − 12 r cm erg − § 2 s . that 3.5 − 1 and , a n nse tteetra odro h disk. the of border external the at the finishes inside in and begins lying structure gap structures eighth the seven finally the gap; to the one inner second the the to range disk; corresponds thick structure optically first the the For (crosses): show structures. figure small this very on colors) (and symbols overlapping oisn&Slk(01,wofudta planet 5 a to that 4 found Dodson- open who by can (2011), considered Salyk & distance half Robinson interaction approximately is the This of planet. (outer) inner the uniissc stems n enpsto fthe other of position obtain mean We see and structure, mass size. structure, the radial each as their such for quantities estimate edge obtain to radial can as we outer so disk, and the inner on the blocks cell by metrically t,adapaeayaceinprmtreulto equal parameter 3 accretion plan- at planetary 2 1 for a considered and depth optical ets, of ranges the in pciey ent htteinr(ue)bre is border re- (outer) gap, inner at the the of located that borders note outer We and spectively. inner the are lines n nsigwt au f00 t3 at 0.01 of value a with finishing and hnrgos n t3 at and regions; thin ehv endtegpfo ninrt nouter an with to material inner is there an that from such gap radius the defined have We tuigafiln atro 0 of good factor a filling obtaining 44, a DoAr using and model fit Aur They GM of (2011). SEDs Salyk SEDs, the & observed Dodson-Robinson to models g. adjust e. to gap filling thick the optically of mean factor a use authors Some gions. ligfco sdmntdb pial intermediate 2 optically at by regions; dominated is factor filling o-ih n otm epciey t10 At respectively. 3 2, bottom, 1, and times at top-right equal planets, 2 parameter and accretion 1, planetary to a fill- for radial azimuthal factor mean ing complex 2014). a al. shows et 7 Perez Figure spectra 2011; simulations Salyk disk hydrodynamical & from (Dodson-Robinson protoplanetary data model the authors without to by used desire commonly who of is necessity quantity the This without un- details. structure to disk us area. the allows total derstand quantity the geometric and important area This thick optically the between ihtm,satn ihavleo . t1 at 0.1 of value a with starting time, with factor filling thick τ = netesrcue r elcaatrzdgeo- characterized well are structures the Once iue8sosterda ie ftestructures the of sizes radial the shows 8 Figure h ligfco fargo sdfie steratio the as defined is region a of factor filling The h Σ × i κ 10 10 3.4 ≈ µ 5 3.3 m × h ieo h Structures the of Size The . r.Telwraduprhorizontal upper and lower The yrs. ecnseta h enoptically mean the that see can We . 3 § 10 h a iln Factor Filling Gap The . . and 3.5 R 5 R H r,b pial nemdaeand intermediate optically by yrs, h H f ( gap ≈ asin gaps × i 10 § 2 = .,respectively. 3.6, R 5 . A r,b pial hnre- thin optically by yrs, H 3ad0 and 03 gap rmtelcto of location the from ) ≈ ,τ> 10 × 5 2 10 /A . r.Tesame The yrs. ,respectively. 1, 5 × gap τ r,top-left, yrs, 10 ≤ 5 × decreases 5 ,where 2, r,the yrs, yrs. 10 5 yrs © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México i.6 nphta 3 at Snapshot 6. Fig. o et est oa Dmpfo o10A.TpRgt h 2 The (bl Right: thin Top optically AU. 100 depth: to optical 1 of from range map respective 2D their polar Density Left: Top pial hnoe aeamxmmflxi E of SED in the flux dominates c maximum disk dotted a (outer) have The ones inner pc. thin thick 140 optically optically at target The the star). with SEDs Simulated Bottom: h ltbcueterSD aeamxmmflux maximum a have SEDs their because plot the in wt agrnme fpaes,tegeneral the planets), configura- of planetary number other larger the a lie For (with structures tions fifth the gap. and at the fourth located inside the is border; structure gap third lies inner the structure second gap; For the the border; structure across gap first border. inner the the gap at lies (triangles): external struc- ranges the small thin at seventh optically the located and inside sixth are lay the tures structures finally small and border; fifth gap; third gap and inner and fourth the second in the the located are gap; structures the small across first lies the structure (squares): ranges intermediate optically For thi optically online. structures viewed to correspond (red), dash-dotted ht ie hwrdiweetema pia depth optical mean the where radii show lines white × 10 TUTR OMTO NPOOLNTR IK 285 DISKS PROTOPLANETARY IN FORMATION STRUCTURE 5 r.Cneto ewe h tutrsfudi agso opt of ranges in found structures the between Connection yrs. < h > τ 10 ( r 10 ) e,itreit gen n hc rd tutrs Hori structures. (red) thick and (green) intermediate ue), − ,itreit n hc,rsetvl.Teclrfiuecan figure color The respectively. thick, and intermediate n, i − 13 .Tesalcoe ie hw h ilrdio h planets the of radii Hill the shows lines closed small The 2. = 13 r cm erg pcrm notclyitreit tutr n three and structure intermediate optically An spectrum. r cm erg eairo h lntpsto essterneigh- their in versus presented is position structures planet the bour of the description of detailed three behavior A the regimes. sharing in center depth similar, located gap optical the are is of which structures surroundings structures the the small the of for size except the of description em hshpesbcueteetra at of parts external the because optically happens indirect of This the number of term. inclusion the the without than the structures thick in larger structures becomes intermediate gap of number equa- the hydrodynamic tions, the in included is term potential re(lc)sostettlsetu srcue + (structures spectrum total the shows (black) urve o oprsn ent htwe h indirect the when that note we comparison, For − − 2 oa a hr h tutrsaesoe with showed are structures the where map polar D 2 s − s − 1 h oi uvs(le,dse gen and (green) dashed (blue), curves solid The . 1 h eto h tutrsd o perin appear not do structures the of rest The cldph n hi SEDs. their and depths ical § 3.6. zontal be . © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México h a eini h enfiln atro pial hc ma thick optically of factor filling mean d a the optical intermediate is of thin, region range optically gap by the to factor correspond filling (red), azimuthal dotted mean The 7. Fig. AL. ET ALVAREZ-MERAZ, 286 that em,tegpocr talre radius. larger a at the occurs including that gap structure Note the our terms, details. on the influence on terms just significant indirect analysis, a the have formation, not structure do Then, of terms structures. the op- in intermediate of of optically increase cleared of easily the number is allowing gap structures, the thick struc- i.e., tically of gap, evolution the in faster slower tures a a to allowing due density, rate, surface migration lower a have disk the online. viewed τ = h Σ( r ) i κ 10 µ m o et 1 left: Top . × 10 5 r.Tprgt 2 right: Top yrs. dtikrgos epciey h ahdhrzna line horizontal dashed The respectively. regions, thick nd × eil hr h a sdfie o any for defined is gap the where terial, r hs o hc h ut(a)ms saoeof above is mass (gas) dust the 10 which structures for Massive those non-massive. are or massive as tures tr crto aaee qa o1 n plan- 2 and 1, 3 to plan- at equal a ets, for parameter range accretion depth optical etary and mass dust tures’ ph h oi uvs(le,dse gen n dash- and (green) dashed (blue), curves solid The epth. 10 − 5 iue9sostecnrbto ftestruc- the of contribution the shows 9 Figure 3 r.Bto:3 Bottom: yrs. M ⊕ × 3.5 (0 10 . 1 h asso h Structures the of Masses The . M 5 r.Hratr ecasf h struc- the classify we Hereafter, yrs. ⊕ ,wietennmsiestructures non-massive the while ), × 10 5 r.Teclrfiuecnbe can figure color The yrs. r with τ ≤ such 2 in © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México i.8 ailsz fsrcue a 3 (at structures of size Radial 8. Fig. zna iecrepnst h ne otr odrof border (outer) inner hor- (bottom) the cavity, top to the solid corresponds to The line correspond borders. izontal symbols (outer) (outer) inner the inner structures, thick The and (blue), intermediate bor- respectively. triangles thin, the The optically to of correspond ders (red), structure. crosses the and (green) of squares edge outer and tutrshv aiu u nterSDabove SED their in νF flux massive maximum These a have gap. structures the op- defines an inter- structure finally thin and optically tically gap; first the the crosses disk; structure struc- mediate outer thick the optically eighth defines the ture disk; inner de- the approximately which fines region opti- thick inner- The optically the most encompasses value. structure this massive below thick mass cally a having those are h ue aeflxsblwti value. this below fluxes have tures ytmwt orpaesadapaeayaccretion planetary a planetary and the planets for four picture number planet, with the the each system present than around structures 10-12 structures complex description Figures of neighbour more real here. is The a presented process semi-major accretion; this mean of planetary planet. the the the around affect of structures ones neighbour axis the neigh- by the mean planet; in the we each time how of in present evolves bourhood we structures Here of number information. of amount τ ( 3.6 ν r h iuain oti noverwhelming an contain simulations The ) ∼ i tutrsi h lntr Neighbourhood Planetary the in Structures . .Teclrfiuecnb iwdonline. viewed be can figure color The 2. = 10 − r 13 gap r cm erg , in and − r 2 gap TUTR OMTO NPOOLNTR IK 287 DISKS PROTOPLANETARY IN FORMATION STRUCTURE s − , out 1 h o-asv struc- non-massive The . epciey ..where i.e. respectively. , × 10 5 r) rinner or yrs), hs o ahpae h itiuino structures planet. of structure the distribution thick the to planet optically linked each physically for the Thus, necessarily position i.e., not spatial same planet, is the the the have of not as neighbourhood opti- do the Two the planet in to third region. structures due thick thick planets, optically cally outer the and to inner transition the thin to optically structures related an intermediate with optically gap some the environment in find we 12) (Figure lnt.A 2 intermediate At outer optically the of of time, planets. start neighbourhood same of the the the dominate environment structures At is thin optically it gap. the the planets; of neigh- inner formation the the the in emerge of to bourhood starting are structures thin 5 At planet. hr h a sesl n ucl omd We such are formed. gap quickly the of and limits that the easily that is remember should gap the where h oiino h hr lnt t3 At planet. third at the located is of structure position thick thin the optically optically An by dominated material. that gap structure a larger forms a eventually form to merge structures thin eeec oFgr 3 h otdhrzna iecorre- line horizontal 10 dotted to the sponds 13, Figure Fo to respectively. reference structures, thick optically and to intermediate correspond thin, (red), crosses and (green) squares h o-asv tutrs h oo gr a be parameter can figure color The online. viewed structures. non-massive the i.9 utms itiue nsrcue a 3 (at structures in distributed mass Dust 9. Fig. fwl ie iiaeds,ognc n riie within 0 troilite; of and range organics size dust, a silicate mixed well of h τ ( r ) i f − nie(usd)teinr(outer) inner the (outside) inside 2 = 3 × ,ta orsod oascenario a to corresponds that 1, = × M . 10 005 ⊕ 10 4 hc eaae h asv from massive the separates which , 5 r Fgr 0,saloptically small 10), (Figure yrs − r Fgr 1,teoptically the 11), (Figure yrs 0 . 15 µ .Tetinls(blue), triangles The m. . 5 × × 10 10 5 5 yrs) yrs r © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México odro h a vle nodro magnitude of inner order rate mean the an a evolves that (with gap see faster the can of we planetary border Also, the reso- for spatial available neighbourhood. high are when observations useful planet. lution be the will that of results location accretion and These planetary time on a depends in strongly resulting different, is ca figure color The planets. the of by axis size radial semimajor the the with are correspondence lines the shows plot bottom oprdwt h ue a odr(ihamean a (with border gap outer rate the with compared h pe ih,lf n oe lt orsodt h system the to correspond plots lower and left right, upper The irto aeo lnt is planets of rate migration ihntesm re fmgiue hs the but Thus, rate, magnitude. border of gap order outer same the the than within faster i.e., h lntnme:1frteinrad4frteotrpae.E planet. colo outer red the and for green 4 blue, and to inner corresponding the structures, for thick 1 number: planet the fteotcldphfrtehdoyaia iuain t5 at simulations ea hydrodynamical around the structures for of depth number optical the the of of evolution Time 10. Fig. AL. ET ALVAREZ-MERAZ, 288 ≈ 3 . 7 × 10 − 6 Uyr AU − 1 ≈ .Hwvr h mean the However, ). ≈ 1 5 . . 4 2 × × 10 10 − − 5 6 Uyr AU Uyr AU − − 1 1 ), ) s epciey h etclai stenme fstructur of number the is axis vertical The respectively. rs, × hpae.Tetplf ltrpeet h oa Dimage 2D polar the represents plot left top The planet. ch 10 tutrs(ssoni iue8.Tehrzna dashed horizontal The 8). Figure in shown (as structures h asv tutrsa hs oemsiethan massive more define those we as range, 5 depth structures the massive optical dominate each the which in structures In spectra the disk). disk detect outer and opti- to inner two order (the by structures dominated thick was cally spectrum the that saw ue a odrvlct ol eemn h mean the rate. determine migration could planetary velocity border gap outer evee online. viewed be n t5 at c eto sdvddit ,frti,itreit and intermediate thin, for 3, into divided is section ach 4 × r.I h o ih lt h oiotlai indicates axis horizontal the plot, right top the In yrs. 3.7 ntesaso fFgr t3 at 5 Figure of snapshot the In 10 × − h vlto fteNme fMassive of Number the of Evolution The . 10 3 4 M 2 , ⊕ × hc orsodt notclythin optically an to correspond which , 10 5 n 3 and Structures . 5 × 10 5 r. epciey The respectively. yrs., × 10 5 r,we yrs, es. © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México tutr ntesm gr,wt aiu flux maximum a of with SED figure, the same in the in structure online. viewed be can figure i.1.Sm sFgr 0bta 2 at but 10 Figure as Same 11. Fig. rto aaee qa o1utl3 until ac- 1 of planetary to number a equal the and parameter planets for cretion 2 evolution for time structures the massive shows 13 ure 5 × 10 4 r,tefis pial nemdaestructure intermediate optically first the yrs, νF ν ≈ 8 TUTR OMTO NPOOLNTR IK 289 DISKS PROTOPLANETARY IN FORMATION STRUCTURE × 10 − 12 r cm erg × 10 . 5 5 × r.Tecolor The yrs. − 10 2 s 5 − r.At yrs. 1 Fig- . as fterpo otiuint h oa spectra. total be- the to quantified contribution not poor are their of structures begins. cause massive disk hydro- non pre-transitional a of a The relevance for the time model Fi- this dynamical at disk. i.e., gap, outer the and in inner 2 the at of nally emergence the see rssi h ik fe ht t7 at that, After disk. the in arises online. viewed be can figure color i.1.Sm htFgr 0bta 3 at but 10 Figure that Same 12. Fig. × 10 5 r h pial hnsrcue arise structures thin optically the yrs × . 5 10 × 4 10 r,w can we yrs, 5 r.The yrs. © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México i.1.Teeouino h ubro tutrsmore structures of number the 5 than of massive evolution The 13. Fig. AL. ET ALVAREZ-MERAZ, 290 o ntne t3 at instance, For online. viewed be struc- can thick figure color and The cor- intermediate respectively. (red), tures, thin, crosses optically and to (green) respond squares (blue), triangles ie o xml,t ecieteeouino their of evolution the in followed describe emission. easily to be are example, can for structures they time, that massive so the number, in that few optically A is the respectively. fact for ranges, noteworthy 2:6 thick and and 1:6 intermediate 1:5, thin, are massive non to n h iapaac ftesrcue ntegap. the in structures the evolution of SED the disappearance pa- follow the can accretion We and planetary 1. a to and equal rameter planets 2 with model omteinradotrds.Fo 2 From disk. outer and inner the form remains one 1 only at but structures, intermediate cally nraetereiso otiuina h iein- structures time 5 Both the from as gap. creases: contribution emission the their inside increase intermedi- lie optically structures and ate thin optically massive two 3 o h pia hnsrcue n rm8 from and structure, thin optical the for 1 tutr.Hwvr sw ilsein see will we as However, structure. 3.8 × × o xml,a 5 at example, For a of SED the of evolution the shows 14 Figure 10 10 vlto fteSDfrteGpStructures Gap the for SED the of Evolution . × 5 − 10 11 r,i diint h ne n ue disks, outer and inner the to addition in yrs, 5 r cm erg r.A hstm h iksprtsto separates disk the time this At yrs. × 10 × − − 10 3 2 × M s − − × 10 ⊕ 12 1 10 5 nds,utl3 until dust, in o h pia intermediate optical the for o8 to 4 r,terto fmassive of ratios the yrs, r,teeaetreopti- three are there yrs, × 10 − 12 § . 5 r cm erg .1 tthese at 3.11, × 10 × 5 × 10 r.The yrs. − 10 − 2 12 5 s − to to 1 r n ue ikcnrbto.I atclr h peak the particular, 20 In inner at contribution. the disk surpassing outer the SED and is the to structure contributor intermediate largest optically This bands. ikta h lp fteSDfo 0t 100 to 10 from SED the pre-transitional of a slope the of the in example that bands this silicate disk in the note explain We to SED. gap ma- et thin the Espaillat optically in that of terial emission Note the cavity. required larger (2010) al. a open man- to planets is of ages result number This greater a bands. because silicate reasonable the is in emission one thin dominant optically the the increases, planets of ber fsrcue stenme fpaesicessfor increases planets of number f the as structures of otr lnt tteiiiltm,tems between mass the time, initial r the At planet. (outer) sicesdi h a,wieta o h optically be- the discussed be for will low. that This while decreased. structures gap, is thin intermediate the optically in for increased factor is filling the times al nemdaesrcuecnb eni h range the in opti- seen an 10 be planets, can four structure with intermediate case cally the In to contribution spectrum. opti- the the two dominate by which mainly disks, thick separated cally was disk the planets, r loicess eefe,ti aswl ereferred mass. be initial will the mass as this to Hereafter, increases. also at asunits, mass earth negligible. but is observed, spectrum is the increases to parts. contribution planets two structures their of of in number large number separated the the not as be in is to increment time an disk simulation However, the The for planets. enough ( 4 accretion and cases planetary 3 shows smaller (bottom) a 15 with optically Figure an within environment. in- gap thin optically the exist in there structures that termediate means that negative; is ag:0.005-0.25 range: ndb h enotcldpheult ,i.e. 2, to equal de- depth boundaries optical the mean between h the consider is We by mass fined gap studied. here the depth that optical of ranges 3.9 τ gap p p ,a 3 at 1, = , , ( in in − r iue1 tp hw nices ntenumber the in increase an shows (top) 15 Figure iue 61 hwtems vlto (in evolution mass the show 16-18 Figures h Eso h tutrswieVrigthe Varying while Structures the of SEDs The . , ) in and i 50 ( µ r = = 2 = spoue yti tutr.I h num- the If structure. this by produced is m p µ , out r < r r ,ie,i h ag nldn h silicate the including range the in i.e., m, p 3.10 × , stesm-ao xso h inner the of axis semi-major the is ) out 10 p h a asEvolution Mass Gap The . h 5 , sicesdi h ubro planets of number the if increased is Σ( in r.I h ae ihtoadthree and two with cases the In yrs. r and ubro Planets of Number M ) µ i )i h a o h three the for gap the in m) κ ⊕ 10 ,o ml utgan (size grains dust small of ), r gap µ m , hshpesa radii at happens This . out = r > r f 0 o 2, for 10) = p , out where , µ m © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México 2 aso h 14 r oe fKase al. Fig- as et in defined curves Kraus is dashed mass of the This by model shown gap 16-18. Ori is ures thin It V1247 optically the the (2013). plot of we mass simulations, of set inter thin, online. (st optically viewed spectra to be total correspond can the show (red), (black) dash-dotted curves and dotted The 9. Figure Σ i.1.Seta nrydsrbto aito uigthe during variation distribution energy Spectral 14. Fig. mle yafco f07 hntevlew found we value the in than is model 0.72 value our of this in factor However, a only by they grains. smaller which dust in carbon model, include spectral Ori V1247 their 9 parameter oeta h aso h pial hnmtra in material thin is optically the gap of the We mass of the material. mass that intermediate the note optically time, by this its dominated At from magnitude value. of been orders initial has two 16) almost Figure by the inner gap in reduced the an curve that solid shows into (the 13), mass separated Figure total see has disk, outer disk an the and which (in yrs . × 0 gap 10 × ln h vlto ftegpms o our for mass gap the of evolution the Along h aewt lnt n lntr accretion planetary and planets 2 with case The , Kraus − 10 6 5 cm g 2 , × f . 5 π − tplf nFgr 6 t8 at 16) Figure in (top-left 1 = × ( 2 r hr h atvlei h etfi to fit best the is value last the where , 10 gap § 5 3.13. , n 3 and , out 2 TUTR OMTO NPOOLNTR IK 291 DISKS PROTOPLANETARY IN FORMATION STRUCTURE − r . 0 gap × , in 10 2 5 ,wt Σ with ), r) hw r h pcr ftesrcue on bv h h the above found structures the of spectra the are Shown yrs). M gap gap , , Kraus Kraus × 10 = = 4 eit n hc tutrs epciey h oo figur color The respectively. structures, thick and mediate vlto.(..frtms5 times for (i.e. evolution. utrs+sa) h oi uvs(le,dse (green) dashed (blue), curves solid The star). + ructures aewt lnt,teotclyti ru mass Kraus thin optically the planets, M 2 with case eoeotclytikr rud9 cases Around latter the thicker. 4 in and optically structures 3 become gap with the cases that the in so than in planets, planets faster 2 is with case accretion This the planetary behaviour. the 17, same because Figure the happens in show bottom not and do for (top-right respectively) cases planets The 4 structures. and thick the 3 optically to the equal of is mass structures intermediate optically the h a is gap the iue1)at 17) Figure ffcsaefse hni h aeo planets. 2 of case the 16) in opening than Figure gap faster in the are planets, (top-right 16) effects 3 Figure in of (bottom cases 4 and the in For contained factor mass the gap. optical filling to the of related the ranges directly the not 19, is for depth gap Figure the in in material see between mass. we comparable a as has However range depth optical each for gap h aewt lnt and planets 2 with case The , Kraus M seult h aso h pial thin optically the of mass the to equal is gap ≈ , Kraus 4 × 10 fe 2 After . 5 r hw httems of mass the that shows yrs × 10 × 4 1 , 10 f . 0 5 0(o-etin (top-left 10 = r,tematerial the yrs, × × rzna iein line orizontal 10 10 5 5 1 , r nthe in yrs . 5 × 10 5 e , © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México o osdrdi h oe fV27Oib Kraus by Ori V1247 structures (2013). of inside al. model et is the material in the considered not of structures, of most thin lot hence non-optically a in and because located important is is and material This thick optically structures. optically thin the the over of dominates structures mass intermediate gap simulations. the hydrodynamic However, our in detected material solid The struc thick star). and + intermediate (structures thin, optically spectra to total correspond the show (black) 10 it tutrsa 7 interme- at optically structures of diate appearance the observe we ever trmassalraceinb h planets). the by accretion param- the smaller accretion of means planetary mass larger eter a larger that a accre- (notice planetary to gap larger corresponds a parameter (2011), al. tion et gap; Zhu the of in mass like larger (2) a generates planets of number number the on depends turn in planets. which of respectively. on size depends planets, gap structures 4 the intermediate and of presence 3 The 2, considering when i.1.TeSDbhvorfrtopaeayaceinparame accretion planetary two for behaviour SED The 15. Fig. AL. ET ALVAREZ-MERAZ, 292 6 h ae with cases The h anrslso u nlssae 1 larger a (1) are: analysis our of results main The r,d o hwotclyti tutrs How- structures. thin optically show not do yrs, f 0 Fgr 8,aaye for analysed 18), (Figure 100 = × 10 5 6 , × 10 5 n 5 and × 10 5 yrs, ue,rsetvl.Teclrfiuecnb iwdonline. viewed be can figure color The respectively. tures, a oiae yotclyti aeilsatn at starting material 2 thin optically by dominated gap al hnmtra,tefiln atro h optically approximately 0 the is regions of thick factor and intermediate filling thin, the material, thin cally eosrei iue1 httegpms fopti- of mass gap the that 16 time, Figure same the in At observe of material. we thick factor and filling thin the optically between difference magnitude of n atro h a.Tecsswt (top-left), 2 and with planets cases (bottom) The 4 and gap. (top-right) the 3 of factor ing 3.11 a sdmntdb pial nemdaematerial, 5 intermediate from optically by dominated is gap 0.1. to equal best with material the factor thick that filling optically of found filament They a of required 44. fit model DoAr by their of obtained dis- in spectrum region the (2011) we gap Salyk line the & dashed of Dodson-Robinson factor horizontal filling an the As play here. shown . × uvs(le,dse gen n ahdte (red), dash-dotted and (green) dashed (blue), curves ,0 7, es( ters t3 At iue1 hw h vlto ftema fill- mean the of evolution the shows 19 Figure h aewt lnt hw h tg hnthe when stage the shows planets 2 with case The 10 h vlto fteFligFco fteGap the of Factor Filling the of Evolution The . . 5ad0 and 25 5 × f yrs. × ,top; 1, = 10 10 4 5 r o2 to yrs . r,wt h a oiae yopti- by dominated gap the with yrs, 5 epciey .. hr sa order an is there i.e., respectively, 05, f 0 utm.Tedte curves dotted The buttom). 10, = × 10 5 r,adtesaeo the of stage the and yrs, f are 1 = © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México al hnadtikmtra a oprbevalues, comparable has ≈ material thick and thin cally online. cusltrta ntecs ih2planets. 2 with case the material in thin dom- than optically the by later but factor planets, occurs filling 4 the and of 3 with inance cases the for gap i.1.Teds aseouini h a i at asunit mass earth (in gap the in evolution mass dust The 16. Fig. osdrn N iedsrbto.Tecsswt ,3ad4 and 3 2, with cases The distribution. size MNR a considering utms.Frrfrne eso h oe fKase l (201 al. et Kraus Σ of of model cavity the the ca show in thick we density and surface reference, For intermediate thin, mass. respectiv optically dust bottom, the and to top-right correspond top-left, from ordered are 10 − 2 M ⊕ iia eaiu sosre nthe in observed is behaviour similar A . TUTR OMTO NPOOLNTR IK 293 DISKS PROTOPLANETARY IN FORMATION STRUCTURE gap , Kraus 9 = × 10 − 6 cm g − l.Tetinls(le,surs(re)adcoss(red) crosses and (green) squares (blue), triangles The ely. 2 e,rsetvl.Tesldcrecrepnst h total the to corresponds curve solid The respectively. ses, e eal nthe in details see , adffrneo tlattoodr fmgiuebe- magnitude of orders two least spectrum at the of the to difference contribution to (a small contribute a gap have but the op- mass, small in the structures where thick 9, and tically 6 Figures in shown results s lnt n h mletaceinprmtr( parameter accretion smallest the and planets M )o h aswti h a,dse uv wt a (with curve dashed gap, the within mass the of 3) o h aeo lnt,ti scnitn with consistent is this planets, 2 of case the For ⊕ ,frds risi h ierne0 range size the in grains dust for ), § .0.Teclrfiuecnb viewed be can figure color The 3.10). . 005 − 0 . f 25 1), = µ m, , © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México 9 LAE-EA,E AL. ET ALVAREZ-MERAZ, 294 we pial hnadtiksrcue ntegap, the in structures ≈ thick and thin optically tween ≈ atbcmsrlvn hnfitn h a spectrum gap This the fitting structures. when thin relevant optically becomes the fact hide of only mass the can twice structures structures. intermediate thin mag- optically optically of The than order material one more hide nitude could regions that means thick This optically would spectrum. latter the the dominate and to continue structures, thin mass the optically to struc- the compared thick of magnitude of optically order the an by of tures mass the increase could i.1.Sm sFgr 6 u ihmdl crto paramet accretion middle with but 16, Figure as Same 17. Fig. 8 5 × × 10 10 − − 12 3 and and < ≈ 10 2 − × 13 10 r cm erg − 4 M ⊕ − epciey We respectively. , 2 s − 1 ihmasses with , otn,i re oetmt h muto material im- structures. of these amount is by the emission ranges hidden estimate of depth to order study optical in the several portant, why in reason structures the of the is of time, This factor same filling the factor a 0.85. At filling has 44. the material DoAr intermediate to of optically equal region is gap planets the 2 of of case the for ae h muto aeili h gap. the in fit underesti- material a of clearly amount words, material the other thin mates In optically only material. with thin optically with r( er entc htat that notice We f 0.Teclrfiuecnb iwdonline. viewed be can figure color The 10). = ≈ 8 × 10 4 r h ligfactor filling the yrs © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México i.1.Sm sFgr 6 u ihtelretaceinpar accretion largest the with but 16, Figure as Same 18. Fig. atro h a o h ae ih2(o-et,3 (top-left), 2 with and cases planets the (bottom) 4 for and gap (top-right) the of factor tg hntegpi oiae yotclyinter- 3 optically at by starts dominated material is mediate gap the when stage tprgt n bto)paes and planets, (bottom) 4 and (top-right) ae h ligfco ftegputlteedo the of end the until 4 gap at the domi- simulation, of always factor material filling the thick nates optically the planets, 4 10 6 iue2 hw h vlto ftema filling mean the of evolution the shows 20 Figure iue2 hw h ae ih2(o-et,3 (top-left), 2 with cases the shows 21 Figure r fsmlto ie tti ieteoptically the time this At time. simulation of yrs . 5 × 10 5 TUTR OMTO NPOOLNTR IK 295 DISKS PROTOPLANETARY IN FORMATION STRUCTURE yrs. . 5 × 10 5 r.Fr3and 3 For yrs. f f 0 The 10. = 0,at 100, = mtr( ameter eed nteeouinr tt ftesystem. the of state evolutionary strongly the gap the on the in that factor) depends note filling to (or important mass is estimated It dominant. always is pial nemdaemtra vnulybecomes for eventually dominant; material intermediate optically hntenme fpaesi ml;for small; is planets of number predominate the material when thin optically and termediate u anrslsae for are: results main our t tutrsapa t8 at appear intermedi- structures optically ate Some dominates. material thick umrzn,a ie rae hn3 than greater times at Summarizing, f 0) h oo gr a evee online. viewed be can figure color The 100). = f 0,teotclytikmaterial thick optically the 100, = f × 10 0 h pial in- optically the 10, = 5 yrs. f × ,the 1, = 10 5 yrs, © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México hte ti osbet omstlie nteneigh- know planets. the massive in us the satellites lets of form to it bourhood possible because is it important, whether highly is hood a modelling when system. account into particular taken be should This online. viewed Do be disk can pre-transitional figure the color The for fit 5). Figure best their the produce to value i.1.Ma ligfco vlto ntegp h triangl The resp gap. structures, the thick in and intermediate evolution thin, factor optically filling to Mean 19. Fig. AL. ET ALVAREZ-MERAZ, 296 3.12 h ecito fteinrpae neighbour- planet inner the of description The vlto fteDs asit h Hill the into Mass Dust the of Evolution . aisfrteInrotPlanet Innermost the for Radius ciey o oprsn h oiotldse ieshows line dashed horizontal the comparison, For ectively. r4 eue yDdo-oisn&Slk(01 (see (2011) Salyk & Dodson-Robinson by deduced 44 Ar s(le,surs(re)adcoss(e) correspond (red), crosses and (green) squares (blue), es hsi og nlss eas ed o include not do we because analysis, rough a is this is hs hsgvsu esnbeetmt fthe (see of region estimate this reasonable ra- inside a Hill us mass gives the this inside work. thus, contained because dius; this completely radius Hill are in the cells of developed all fraction simulations 0.7 the of choose We set the for nlnrms units planet innermost mass the lunar for radius in Hill 0.7 within mass iue 2t 4so h vlto ftedust the of evolution the show 24 to 22 Figures M L (1 M § L ..) ent that note We 2.1.5). 7 = . 3477 × 10 25 the g) © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México ihhge resolution. higher simulations ini- with disks better circumplanetary a for establish However, conditions to tial useful (2008). Ayliffe be al. in could et should as exercise Machida we this cells and nested analysis, (2009) on Bate better gas & based a the approach For in an present use planet. physics the the for near model detailed a lto ieo 3 of time ulation aisdcessfo niiilvle(10 value initial an from decreases radius i.2.Sm sFgr 9 u ihmdl au o h accre the for value middle with but 19, Figure as Same 20. Fig. nsmltoswith simulations In . 5 × 10 5 TUTR OMTO NPOOLNTR IK 297 DISKS PROTOPLANETARY IN FORMATION STRUCTURE f r,tems ihnteHill the within mass the yrs, Fgr 2 n sim- a and 22) (Figure 1 = − 1 M L to ) vrteotclyti as umrzn,i all in Summarizing, with mass. cases dominates the thin planet dust planets, optically 4 intermediate the with optically over case the the optical of in the mass Finally, thick over optically mass. dominates the thin of dust the mass In intermediate the and planets, ranges. 3 thin with and that case intermediate the over optical planets, dominates the dust 2 thick of with optically case the of the mass In respectively. cases, 10 inprmtr h oo gr a evee online. viewed be can figure color The parameter. tion − 2 10 , − 3 n 10 and f − 4 ,i la hta increase an that clear is 1, = M L o h ,3ad4planet 4 and 3 2, the for © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México nieteHl aisfrteinrplanets. inner the for radius depth Hill optical of of the evolution ranges inside different faster the a in allows structures planets the of number the in AL. ET ALVAREZ-MERAZ, 298 lto ierahs4 reaches time ulation h ilrdu erae nodro antd,from magnitude, of order 10 an decreases radius Hill the rsn ssihl mle ihicesn planet increasing with smaller number. slightly is present − ncsswith cases In 1 i.2.Sm sFgr 9 u ihtelretaceinpar accretion largest the with but 19, Figure as Same 21. Fig. M L o10 to − f 2 0(iue2) hr h sim- the where 23), (Figure 10 = M L . 5 efudta h mass the that found We . × 10 5 r,tems within mass the yrs, h uti iil nternefo .0 o0 to 0.005 of from range 20% the in that visible 2011) is dust consider Salyk the we & if Dodson-Robinson Now, (like to disk. case) circumplanetary each the in rate form constant nearly a (with material radius. Hill the within mass the 10 oercsadpaeeia ois hntevalues be- the then could bodies, size planetesimal millimetric and above rocks come 80% other the and 6 rlmnr ocuini htteei enough is there that is conclusion preliminary A with simulations In mtr h oo gr a evee online. viewed be can figure color The ameter. r,w ontosreasgicn eraeof decrease significant a observe not do we yrs, f 0 Fgr 4,at 24), (Figure 100 = . 25 µ m, © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México 21) nbt ae,w n odfi oteob- the to con- fit case good non-hydrodynamic a The find we spectrum. cases, served both al. In et interfero- Kraus system with (2013). by observations consistent stellar photometric are and latter the metric the for Ori; V1247 models hydrodynamic and the beyond multiplied are work. be formation this moon must of of scope radius details The Hill 5. the by within mass of o in planet thin, inner optically online. the to viewed for correspond be Radii (red), Hill crosses the and inside (green) mass Dust 22. Fig. nti eto epeetnnhydrodynamic non present we section this In 3.13 h 14 r Case Ori V1247 The . TUTR OMTO NPOOLNTR IK 299 DISKS PROTOPLANETARY IN FORMATION STRUCTURE emdaeadtikcss epciey h oo gr c figure color The respectively. cases, thick and termediate h orsodn ytm h rage bu) squares (blue), triangles The system. corresponding the f eew osdrol mrhu abnfrthe compar- for a make carbon to disk, amorphous the of only composition chemical consider we here reality. a the find how to to of closer required configuration examples system is as information cases observational both this new by present explained We be cannot 2013) model. observa- al. interferometric et (Kraus the tions the by hence, found structures; asymmetries density axisymmetric of sists iue2 hw oeldSDo 14 Ori; V1247 of SED modelled a shows 25 Figure 3.13.1 o-yrdnmcCase Non-Hydrodynamic . an © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México 0 LAE-EA,E AL. ET ALVAREZ-MERAZ, 300 ue ik aeotclytikmtra ihasur- a and with inner material thick the optically where have AU), disks optically (45-120 outer an disk and outer AU), by (0.26-45 followed thick gap AU), thin (0.16-0.26 optically op- disk an an inner considering thick model, tically spec- axisimmetric the the of fit op- of the an trum produce as We outer gap structure. and the thin and inner tically structures, the individual model consider as the we disks separate opti- i.e., we order the structures, regions, In by by thick (2013). contributions and al. thin emission et cally the Kraus extract by model to the to ison i.2.Sm sFgr 2btwt h ideaceinparam accretion middle the with but 22 Figure as Same 23. Fig. ne ik oepantedffrnebtentetwo the the between difference over the MIR gap explain To to the NIR disk. model, inner from (2013). (2013) spectrum al. al. the et et dominates Kraus Kraus by the to proposed Contrary gap the than 1.38 sa pial hnrgo ihacntn density constant the a with explain region to gap thin 1 disk The optically outer wavelengths. an to the longer is extended at of we emission size but observed (2013), the al. AU the with et 120 consistent Kraus are by disks outer model and inner the for aedniypol fslope of profile density face . 25 × tr h oo gr a evee online. viewed be can figure color The eter. 10 − 5 cm g − 2 hc sdne yafco of factor a by denser is which , − .Teesailranges spatial These 1. © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México nwihtepooso h eincnitrc and interact gap. can thicker region a the code, from of transfer escape photons radiative the 3D which the disk, in in the of required thickness is the which consider to need we models i ie3 time a til oiin nteds sedtiso h nta model initial the of different details at (see in disk fixed the and in embedded positions been have planets § esatwt r-omdgp hr seven where gap, pre-formed a with start We ..) u yrdnmcsmlto srnun- run is simulation hydrodynamic Our 2.1.6). i.2.Sm sFgr 2btwt h ags crto para accretion largest the with but 22 Figure as Same 24. Fig. × 3.13.2 10 4 r srahd h ytmrelaxes system The reached. is yrs yrdnmcCase Hydrodynamic . TUTR OMTO NPOOLNTR IK 301 DISKS PROTOPLANETARY IN FORMATION STRUCTURE uino h zmta endniysrae at surface, density mean azimuthal 1 the of lution allowed. is accretion 1 first the during n .5cmae ot hi nta aus It values. initial 1.78 their 0.94, to 0.52, to 0.34, compared out) 0.22, inside 5.05 0.26, (from and to planets value. two the increased initial value of has the a fraction than mass reaches smaller The disk magnitude inner of the orders of density face e n ue te de ftegphv been have gap the of edges 1 steep at smoothed outer and ner × ntetppnlo iue2 eso h evo- the show we 26 Figure of panel top the In 10 ee.Teclrfiuecnb iwdonline. viewed be can figure color The meter. 4 2 , × 10 × 4 × 10 n 3 and 10 4 4 r.A 3 At yrs. r.Atrti ie planetary time, this After yrs. × 10 4 r.Teiiilin- initial The yrs. × 10 4 r,tesur- the yrs, © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México n eodpae,10 planet, second and orhpae,10 planet, fourth ae hc seult 10 to accretion (in- equal maximum in- the planet is find which each the we rate, of to Radii), neighbourhood closer Hill the the is side disk. In it outer because disk. mass one the ner more second from accretes the planet coming more than inner is accreting first mass the are Moreover, This planets outer mass. the that view be follows can figure color The yellow). (i (in diamonds ( squares 2MASS, the spectrum base): IRAS, total data red); the respective in is their thick (black) from optically (taken curve the solid of is the spectra (black) the contribution; curve V1247 are dotted of blue) The (light distribution profile. curves energy density static spectral a the for for depth Model 25. Fig. AL. ET ALVAREZ-MERAZ, 302 lnt 10 planet, rtmcclrsae n pia et isocontours depth optical and ( log- a scale) (in color coordinates polar arithmic in map density the of shot utpoete of properties dust eini endbetween defined is region h a tezn ihotcldepth optical with zone find (the We gap region. the intermediate im- optically are the radii) in Hill mersed their by (specified planets external setelf lti h gr) hs tutrsare structures These figure). the between in located sub-range plot left each the for (see found are structures asymmetric uefrtetosbrne fotcldph the depth, optical of sub-ranges two 0 the for ture (2013). al. et Kraus in region the emdaerne,and range), termediate τ . 5 10 = ntebto ae fFgr 6w hwasnap- a show we 26 Figure of panel bottom the In iue2 hw h ieadms fec struc- each of mass and size the shows 27 Figure < τ < − 2 − , < 10 10 n 1 and 1 − 6A,smlrt h eindescribed region the to similar AU, 46 M 1 , ⊙ − ≈ 0 . § 11 5 yr 0and 20 ...Orotclyintermediate optically Our 2.1.2. , M 1 − < τ < − , 1 )a 3 at 2) ⊙ 12 > τ o h eet planet. seventh the for M − yr τ ≈ 13 ⊙ − teotrds) Two disk). outer (the 2 0 = 6A,a rdce by predicted as AU, 46 × i h pial in- optically the (in 2 1 M yr 10 o h fhadsixth and fifth the for ⊙ − . and 5 4 1 r,asmn the assuming yrs, yr o h hr and third the for − < τ 1 τ o h first the for .Two 2. = )within 2) e n ue ik;tedse uv bak stettldisk total the is (black) curve dashed the disks; outer and ner ik+sa) o oprsn eso h bevddata observed the show we comparison, For star). + disk h pcrmo pial hngpmtra;tedot-dashed the material; gap thin optically of spectrum the le;WS,tinls(nbon;Sizr oi ie(in line solid Spitzer, brown); (in triangles WISE, blue); n r,rpeetn ahrgo endb agso optical of ranges by defined region each representing Ori, ru ta.(03,weete rps asymmetric propose they between where structures (2013), al. et Kraus ne ikfo .6A o02 U(ihasurface a (with AU 0.22 slope of to thick profile AU region density optically 0.16 outer an from need the We disk and AU). inner 110 AU, in- to 1 (the AU to 100 regions from 0.16 simulated from non region two ner and AU AU) 1 100 (from to region with simulated obtained radial is hydrodynamically a AU, 110 the with and AU spectrum 0.16 between modelled range total tele- the The several and of scopes. structure data by each composed of spectrum observed spectrum the Ori, V1247 figure). the in iepaes h asspeitdb hs struc- these by predicted around masses are mas- tures The resonant two planets. by sive reproduced be asymmetric can the structures model, multiplanetary our with that egh h msino h pial hc ue disk outer thick optically ( the wave- of longer At emission the disk. inner lengths thick emis- optically the the over of dominates sion it Particularly, MIR. the (from of region at to gap the AU slope of 0.22 emission profile the The density AU). of (100 AU surface AU values 1 mean (100 simulation a AU the and on 1 density based and AU) the AU 110 in 0.22 and density between the range extrapolate We radial region. inner the ∼ > donline. ed 6A)dmntsoe h msino h two the of emission the over dominates AU) 46 iue2 hw h oa oeldsetu of spectrum modelled total the shows 28 Figure ≈ 6A)dmntsfo I opart to NIR from dominates AU) 46 ≈ 10 ≈ − 5and 15 − 5 − )t oe h pcrmof spectrum the model to 1) 10 − ≈ 2 M 0A.Ti means This AU. 40 ⊕ setelf plot left the (see © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México i.2.Tp enaiuhlgsdniywt pre- a with time density initial gas at azimuthal gap Mean formed Top: 26. Fig. asv nso h a ( gap most the the of are ones These structures massive intermediate gap. optically the two of structures intermediate optically online. viewed be can figure color The overplotted. ae ewe 0ad4 Ua eni iue27. Figure in seen as AU 46 and 20 between cated ltl endb h yrdnmclitrcinof interaction hydrodynamical the by defined pletely ry,05(le,ad10(zr) n 2 and (azure), 1.0 and (blue), 0.5 gray), 2 oiin r elietfidb hi ilrdi h op- The 0 radii. Hill isocontours: their depth by tical identified well are positions 3 in otm nphto ufc est ngcm g loca- in density axis surface of semi-major Snapshot correspondent Bottom: their dot- tion. the vertical at as of lines shown locations are ted planets initial resonant seven mutually 2:1 The dashed (red) respectively. (black), dash-dot-dot-dot and curves, solid (green), the dash-dotted to (blue), correspond which ulation, . . 0 0 × h tutrsaaye nti okaecom- are work this in analysed structures The × 10 10 4 4 , r,wt oaihi cl oo.Teplanet The color. scale logarithmic a with yrs, n 3 and . 0 .DISCUSSION 4. × 10 TUTR OMTO NPOOLNTR IK 303 DISKS PROTOPLANETARY IN FORMATION STRUCTURE 4 . r fhdoyaia sim- hydrodynamical of yrs 1(akga) . (neutral 0.1 gray), (dark 01 t ≈ ,adatr1 after and 0, = 10 − 2 M ⊕ ,adaelo- are and ), . ca)are (cyan) 0 . 0 × − 10 2 at 4 , tutrsfrainare: formation structures interactions. planet-disk to could which related However, structures, be the structures. for call origins other we are that there disk These the of disk. in concentrations the matter of in formation inter- gas the gravitational the allow with the interactions planets and the itself of with action gas disk the • • lentv xlntosfrtefrainof formation the for explanations Alternative rgigi h nlsso tutrsfrthe for structures dust of ( include simulations analysis a to long-term the In planning in are dragging same. we the the work, remain in future should dust qual- the picture of but itative details distribution the in vary the could structures Thus, struc- the between zones tures. transition oc- these of changes in opacity size cur the and because mass structures, number, the This the regions. changes intermediate slightly or op- thin between work, thick, boundaries this tically the of modifies pro- context effect in the this grains In dis- large spatial disks. and toplanetary different et small the a Garufi for show by tribution which made (2013), resolution This al. high obser- of polarimetric homogeneous. vations by be supported the is not that mechanism will means opacity distribution dust and space small et grain the Zhu between and large 2006; difference The disk, al. et 2012). the al. (Paardekooper in through- disk gap distributed the dust remain out grains a smaller grains open the larger to mi- the they able Thus, then are star. and can the edge, grains towards gap Small grate the disk. through the pass massive by in formed inmersed edge of planet gap maximum the as local such a density pref- in are grains accumulated large due the erentially gas then mechanism forces; the drag physical of the decoupled to a are grains is large this where filtration: Dust hr h R satvtdb h ihtemper- high the ( by ature activated zone, is inner located MRI an are the between where zones places: These intermediate 1998). at Hawley (Bal- & created bus turbulence a the to defines related mechanism viscosity MRI this operate 1996); not (Gammie does magne- (MRI) the instability where regions torotational are these zones: Dead prep.). ntr eed nteecec fteheating the of efficiency the the on which of depends ionization, turn of importance in degree cos- The the on by depends relevant. (meanly MRI is ionization nonthermal rays) the disk mic where the zone, of outer source an and als, > T 10 3 )wihinzsteakl met- alkali the ionizes which K) lae-ea ta.in al. et Alvarez-Meraz ´ © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México ihnasz ag f0 of range size a within r tutrs et ailsz ftesrcue rinrand to inner solid The or border. structure, (outer) the inner of to size corresponds structure Radial Left: structures. > τ hwtorne:teotclyitreit:0 intermediate: optically the ranges: two show hw h euto h oe o h tla msin h co The emission. stellar the for model dashed-d the and of contributio (blue) result The dashed the (black), shows emission. dotted the modelled to total correspond the is curve black i.2.SDmdlatr3 after model SED 28. Fig. in and gap, the in structures intermediate Optically 27. Fig. AL. ET ALVAREZ-MERAZ, 304 gap , out ca) iei iue8 h qae n rse correspond crosses and squares the 8, Figure in Like (cyan). 2 where , h τ ( r ) i .Rgt utms itiue nsrcue fwl ie s mixed well of structures in distributed mass Dust Right: 2. = . 005 − × 0 . 15 10 4 µ r ftesmlto,wt h aeosrainldt fFig of data observational same the with simulation, the of yrs .Teclrfiuecnb iwdonline. viewed be can figure color The m. . 5 < τ < bu) n hc:1 thick: and (blue), 1 oiotlln orsod oteotrbre ftecavit the of border outer the to corresponds line horizontal p ue deo h tutr.Inr(ue)smo feach, of symbol (outer) Inner structure. the of edge outer so h pial hn nemdaeadtikstructures thick and intermediate thin, optically the of ns te ca)cre,rsetvl.Tedse ie(green) line dashed The respectively. curves, (cyan) otted o gr a evee online. viewed be can figure lor h pial hc ue ik fe 3 after disk, outer thick optically the otebreso pial nemdaeadthick and intermediate optically of borders the to < τ < lct ut raisadtroilite; and organics dust, ilicate aue.Teotrds has disk outer The (azure). 2 r 5 h solid The 25. ure × 10 4 r.We yrs. y © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México lnto h oe fti ae ( paper this of model the outer the of than planet away farther planet perturbing a quire uhosre tutrs oepanteextended 108 the (to explain explain disk to To planets outer of structures. number observed a smaller such in a results disk with require which model will photoevaporation, source by re- this gap for dispersion the models to Better sensitive is gion. which mid-IR, the cluding e h oeln rsne ee hc smainly is emission. which MIR al- here, the not on presented into will focused take but modelling should gap, the the modelling ter outside new region The the account prep.). in al. oe lost tteSDu o20 to up SED the the fit of to degeneracy the allows However, model 2013). al. et (Kraus xsmercsrcue between structures axisimmetric hoc .W eeo ehdt nls h utstruc- dust the analyse to method a develop We 1. • esmaieorcnlsosa follows. as conclusions our summarize We h utpaeaymdlfrV27Oii an is Ori V1247 for model multiplanetary The ± oe,bcueo h ag a n h non- the and gap large the of because model, ol iems nodro antd larger magnitude of order an mass gap?. hide structures the intermediate could and in thick structures optically optically The in intermediate hidden or is material thick ques- much the how answer these to of tion: us SED allows the which estimate structures, also other We into fragmented structures. are know or can We grow Structures they identified. whether well cell. are gap structures hydrodynamical the detect a within to as able small is as method The simula- hydrodynamical ranges tions. using several depth, at optical disks of protoplanetary of tures rnpr ytruec snteetv)hv a have effective) density not surface is turbulence momenta by angular transport the (where in- places such termediate that show (1996) Gammie mechanisms. i aaozu(00,Zue l 21) Zhu (2014), (2014)). al. Stone et & Zhu (2010), Papaloizou & Lin gas-pressure (e.g., vortexes steep anticyclonic in produce resulting gradients can Planets Terquem 2006; 2008). Tagger (Varni`ere & of zones border dead found outer of been gradients have gas-pressure steep structures in These Regaly (2012). (1999); al. al. et et Lovelace in- wave (RWI); Rossby the stability by produced are with- planets formed out Structures with planets. produced any without are or they vortexes: of Anticyclonic models viscosity the in work. found this not are zones 5A Ot ta.21)temdlwl re- will model the 2016) al. et (Ohta AU 35 ≈ .CONCLUSIONS 5. 0 U iha r mso at emision arc an with AU) 300 P TUTR OMTO NPOOLNTR IK 305 DISKS PROTOPLANETARY IN FORMATION STRUCTURE > 0 rcm gr 100 ≈ lae-ea et Alvarez-Meraz ´ 5and 15 − 2 uhdense Such . µ ,ie in- i.e. m, ≈ 0AU 40 ad .Tehdoyaia iuain rsne in presented simulations hydrodynamical The 4. an that shows scales radii Hill the of analysis An 3. the in increase an shows analysis structure The 2. rct ilhv iteeeto h omto of formation the eccen- on the effect Thus, little have 0.05. will in tricity around structures reaches thick gap optically the happens of this factor When filling 0.17. the to up initially increases zero, which During is eccentricity, the position. simulations planetary neces- the the not posi- to is the linked structure thick sarily op- gap, optically an an the In of of tion gap. environment the thin the in tically between material the position relative and planets the the de- on mainly pends formation structure because inside gap, structures the of not formation does the displacement affect dur- strongly This appreciably simulation. change the the not ing that does means the location This of gap but magnitude. planets, of the order the same of than rate smaller opti- is migration the border mean gap of 0.78. outer rate of thick migration cally factor orbits mean a planetary by the However changes mean the simulations The of the in axis star. semi-major the towards final move to the containing planets gap the allows which star, central § of part is it However, and work. analysis, future planets. further outer requires and sys- this inner moon the of there masses of that the tems speculate between difference we a Thus, is change 2006). (Canup Ward will formation & this moon sure, for condition For initial disks the planets. circumplanetary inner the the material to of of arrive amount the could limits that the This to system, compared ones. planetary material means outer of a This inflow in lower a planets, have planets. inner of the number accre- that mass the planetary inner and the the tion by to limited outer is the regions from inner influx the because material behaviour, of the reasonable a radii is Hill This the planets. of inside ranges depth different of optical faster structures a the allows of planets evolution of number the in increase system. the obser- in of asymmetry some interpretation requires the vations when important, is instance, This with for for parameter. structures accretion scale thin small time optically a larger of a formation planets find the of we number Also, the increases. as structures of number to compared respectively, structures. thin mass optically the twice and .. osdrpaeaymgaintwrsthe towards migration planetary consider 2.1.1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México 0 LAE-EA,E AL. ET ALVAREZ-MERAZ, 306 ryoiz .&Lbw .19,AJ 2,651 421, ApJ, 1994, S. Lubow, 2011, & al. P. et Artymowicz, C., Espaillat, J., D. Wilner, M., S. Andrews, research project. this his of of beginning server the the at run- in group, for simulations Torres-Papaqui some Pablo code. ning Juan RADMC-3D P. thank the Cornelis also of and We release code the FARGO for the Dullemond of release Masset the Frederic for acknowledge number gratefully grant We CONACYT by 365146. supported O. been 246335. has number B. been grant has CONACYT R. by Tecnolog´ıa F. supported y 329762. Ciencia number de grant (CONACYT) Fellowship Nacional Ph.D. Consejo a the by from supported been has Doctor- and de juato Programa Guana- the (Astrof´ısica), de of Ciencias Universidad en student ado Ph.D. paper. a this is of A. presentation R. the improve to us allowed .W etorpoeuet erhsrcue in structures search to procedure our test We 5. p,72 42 732, ApJ, etakteaoyosrfre hs report whose referee, anonymous the thank We and a.Ti oe sal oepanteob- of the formation explain between the to structures shows intermediate able also optically it is and model open SED This served could planets gap. resonant case, a 7 hydrodynamic that the suggest In we (2013). in al. presented This et model the the Kraus disk. with while outer consistent the spectrum, is by model the dominated and is of band band band FIR NIR MIR the of in part gap emission the an AU); the and (45-120 dominates AU), disk (0.26-45 outer gap thick followed opti- optically thin AU), optically an (0.16-0.26 an by disk by represented inner thick be cally can case, spectrum non-hydrodynamic the spectrum, the hydro- In the and cases. on non-hydrodynamic dynamic gap the influence the analyse the in compare we structures to the order of In star the Ori. surrounding V1247 disk circumplanetary the do we as account, work. into this taken in is planets gas the the and between interaction when physical present Note correct is eccentricity the on. in goes increase time the as that gap the inside structures .2t 6A n notclytikotrdisk outer AU. thick 110 optically to an 46 and from from AU from gap 46 a to AU, thick 0.22 0.22 to optically 0.16 from an disk modelled inner contributors: The three (2013). has al. 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