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PoS(BASH2015)004 http://pos.sissa.it/ † ∗ [email protected] Speaker. Hubble Fellow Finding young in protoplanetary disks iscess essential and for constraining understanding the long-term formation evolution pro- ofetary planetary disks systems. with Transitional gaps disks, and protoplan- holes, arerecent great near-IR candidates polarization for harboring imaging these (e.g. young SEEDS,vations planets. have VLT) However, posed and several submm puzzles (e.g. on transitional SMA,in disks. ALMA) these Such obser- disks as, dust and and the gasalso seems decoupling discovered to can in decouple these occur disks. non-axisymmetrically In indisks. this disks. Then chapter, I I Spiral will will patterns present first theoretical are in summarize developments observations disks: on on three gaps, transitional indirect large signatures scalewith of asymmetric observations, young we structures, planets have constrained and protoplanetary spiral disk properties arms.of and planet revealed the By formation. early comparing stage Finally, such observational strategies theories etary to disks directly has find young been planets discussedkey in and to protoplan- detect I young suggest planets directly. that Currentsome accreting direct circumplanetary imaging circumplanetary disk observations disks candidates may have and could already there be found are the more to come. ∗ † Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). BASH 2015 18 - 20 October, 2015 The University of Texas at Austin, USA Zhaohuan Zhu Observational Signatures of Young Planets in Disks Princeton University E-mail: PoS(BASH2015)004 Zhaohuan Zhu Space Telescope has found that more Sptizer 2 spacecraft, more than 1800 have been discovered. Kepler The direct imaging technique is more promising to find young planets in protoplanetary disks A much easier way to find young planets is studying the imprints left by the planet on pro- On the other hand, eventually we would like to confirm the existence of these young planets in In this chapter, I will first summarize transitional disk observations. Then, I will discuss three Thanks largely to the On the other hand, the structure of protoplanetary disks has also been revealed over the last Thus, a missing link in planet formation studies is finding young forming planets in disks. and it has discoveredmethod several requires planets/planet using candidates 10 inYoung meter planetary protoplanetary systems class disks. are telescopes far to away However,parison, get (>100 the such pc HR enough away), 8799 photons system and where from normally 4 obscured the planets by have young dust. been planet. directly For imaged com- is onlytoplanetary 40 disks. away. The gravity fromspiral a patterns young and planet gaps. can Itstructures. perturb can the These also protoplanetary lead large disk, to scale inducing largeprotoplanetary features scale in disks disk disks with instabilities, are causing gaps muchhundreds asymmetric and easier of disk to holes transitional disks be [3], have detected. been are discovered. Transitional great disks, candidates to harbor youngdisks. planets Directly detecting and young planetsbigger in and disks is hotter still than possible mature consideringitself planets. young with Furthermore, planets less when may be a extinction. youngcircumplanetary disk. planet The opens The young a process planet gap, cancircumplanetary can it release disks an exposes continue can observable to amount be of directly grow energy, found and through by these the direct imaging accretion techniques. of the indirect observational signatures left byhow the they planet: can explain gaps, some spiral ofin arms, the detecting transitional asymmetric young disk structures, planets: observations. and observing Finally, accretion I signatures will of discuss circumplanetary the disks. frontier than half of the protostars show[2]. variablities, from Such 0.05 large to variability 0.2 dominates magnitude, the on variability a signal variety induced of by timescales the planet. decade by studying their spectralsolve energy protoplanetary disks distributions either (SEDs). through optical/near-IR Recently,submm/mm telescopes we (e.g. interferometer start Subaru, (e.g. VLT, to Gemini) ALMA, or spatiallywill EVLA). re- reveal In the detailed the disk near structure future, which especially will provide with the ALMA, initial we condition for planetIf formation. we find young planetswhich in will disks, put we stringent knowplanets constraints when, that on where, planet and around formation how protostarsmainly young through theories. because either planets their the form Unfortunately, host radial in finding velocity disks, young are or highly transit variable. method is difficult Young Planets 1. Introduction With such large number of exoplanets,[1], the architecture and of now exo-planetary we systems has knowmost been that of revealed on these planets average are every billions starprotoplanetary of disks has years within roughly old. their one first We planet several have million limited within years constraints 1 lifetime. on AU. how However, they formed in PoS(BASH2015)004 Zhaohuan Zhu m appears to be due µ 10 . 50 AU [9; 5; 7]. ∼ [20]) onto their central stars (e.g. 1 − 5 to yr ∼

M 8 − m, while showing significantly reduced fluxes 10 µ ∼ 3 10 & A young planet can induce spiral arms and gap in protoplanetary disks. A circumplanetary disk Recently, thanks to high contrast NIR polarization imaging (e.g. SEEDS, [10]) and submm- Recent ALMA observations have revealed non-axisymmetric dust distributions in some tran- Surprisingly, despite the wide dust gaps, most transitional disks exhibit gas accretion rates To summarize the observations, transitional disks normally have: 1) moderate accretion rates, Transitional disks are protoplanetary disks with gaps and holes. They were first identified interferometric techniques [11; 12; 13],NIR these observations gaps/holes probe have the been distributionobservations resolved of spatially probe small (Figure larger dust 1). dust particlesobservations particles at reveal the at completely disk different the structures, surface, disk suggestingrelative while to midplane. that submm each small other and In in big protoplanetary many dust disks grains disks, [14]. drift NIR and submm sitional disks [15; 16;crescent-shaped 17]. dust structure between In 45dust the and structure 80 extreme AU is case from at the of leastSpiral . Oph 130 patterns The times IRS have peak stronger also emission 48, than from beendisks there this the (e.g. revealed is upper [18]). by limit a NIR of direct highly the imaging asymmetric opposite observations side in of some theclose transitional to disk. the averaged T Tauri disk accretion rate ( 2) wide dust gaps up to several tens of AU, and in some transitional disks we see: 3) large scale [5; 7; 21]). Maintainingcavity, or this some accretion way requires of allowing either mass a from significant the outer mass disk reservoir to interior move past to the the cavity [22]. entirely to optically-thin dust [5;interpreted 8]. as being The due depletion to of evacuation near- of dust to to mid-infrared disk emission scales is generally Figure 1: also forms around the planetdisk. and the planet continues its growth through2. accretion of Transitional Disks the circumplanetary by their unusual SEDs atexhibit near-infrared strong (NIR) dust and emission mid-infrared at (MIR) wavelengths [4]. The transitional disks relative to typical T Tauri disks atdisks, shorter the wavelengths so-called (e.g., pre-transitional [5; disks, 6; there 7]). isdust evidence In near for a the emission subgroup from star of warm, [7; transitional optically-thick 8], while in other transitional disks the emission at Young Planets PoS(BASH2015)004 Zhaohuan Zhu 4 The SEDs for a full classical (upper panels) and a transitional disk (lower panels). Spatially resolved protoplanetay disk SAO 206462 from VLT (left panel from [19]) using polar- Theoretically, it is known that young planets can gravitationally interact with disks, launching Gap opening process has been throughly studied in viscous disks (e.g. [28; 29]) and MHD spiral density waves [26] and inducing gaps in disks [27]. 3.1 Gaps Figure 3: At ultraviolet wavelengths (the leftmagnetosphericial panels), accretion. the The excess right emission panels above areleft the from panel stellar [23]. is photosphere The from upper is [25]. left due panel to is the from [24] and the lower asymmetric structures at submm/mm, and 4) spiral patterns at Optical/NIR. 3. Indirect Signatures of Young Planets Figure 2: ized scattered light at NIR,structures and have been ALMA revealed at at submm variousslightly (right wavelengths. different. panel Please from note that [17]). the Complicated orientation and of the different two disk images are Young Planets PoS(BASH2015)004 m µ Zhaohuan Zhu . Using a viscous disk model 1 01) derived from observations. − . 0 yr

∼ M 8 m for the inner disk is 100–1000 [22], − µ 10 ∼ at 0.1 AU. Considering that the nominal opacity 5 2 4 is surrounded by a transitional disk [6] with a 14 AU / , the optical depth at 10 g / 2 cm 0.01 and an accretion rate of ∼ disk. Thus, cavities revealed by submm observations may not be present in 1 − m is 10 is derived to be 10–100 g/cm yr µ g

Σ M 8 − 01, . 0 10 = = ˙ α This observational signature is supported by recent observations that caivities revealed by On the other hand, how to deplete micron sized dust within the hole to explain the NIR deficit One possible solution is that multiple planets are present in transitional disks. If multiple Another possibility is that the small dust grains in the inner disk are highly depleted by physical However, companions have not been found inside the cavity of most transitional disks. Thus, Observations have also suggested that gaps in some transitional disks are indeed induced by M submm/mm observations are missing atNIR NIR observations [41; of 19; the 42] samedepletion or objects. in Herbig are The Ae/Be larger stars dust thanof surrounded filtration cavities stars by picture surrounded revealed transitional by by is disks full also compared disks with supported [43]. metal by abundance the metal of transitional dsks is stilldust fragmentation unclear. at the [44] gap has edge done and 1-D suggested that calculations micron-sized considering particles dust may growth also and be filtered. NIR observations. planets from 0.1 AUaccelerated to and passed tens from of onesubstantial AU planet disk to can accretion another rate open so onto that a thetrapped a star mutual at low [22; disk gap, 35]. 2:1 surface However, mean-motion the considering density resonance, giantto can gas planets a sustain pass flow tend large a gas to can number be from of be severalthrough giant tens continuously each planets of planet, are a AU needed fraction all offinal in the accretion the this way rate gas model down onto can the to be star 0.1 intercepted could and AU. be accreted Furthermore, smaller by than when the observed gas planetremoval rates. passes or so grain that growth, the to theopacity. point where Dust the filtration dust [36] opacity in isgas the one drag, NIR possible is dust mechanism far to smaller particles thanof differentiate always the dust a ISM drift from planet-induced to gas. gap, the Duepossibly pressure where to overcoming their maximum the the coupling in pressure to disks reaches thethe inward [37]. gap’s a accreting outer maximum, gas. edge At Dust dust while the particlesfirst the particles will outer simulated gas drift then edge by flows remain outwards, [38; through at the 39].simulations gap. evolving Particle over This diffusion viscous dust due timescales, trapping to wherebeen at a disk achieved. quasi-steady the turbulence [40] state gap is found for edge later that both was micron includedin gas sized a [40] and particles dust in are has 2-D difficult to filter by a mass planet which is 4–5 orders of magnitude larger than the optical depth ( with an optical depth of with of ISM dust at 10 we need to askunseen whether planets. the One serious observed challenge for gap/cavityis almost properties the all fact theoretical are that models some to consistent transitional explain transitional disks withgas disks exhibit accretion the large dust rates existence clearings onto while of the still maintaining star. significant For example, GM Aur has an optically thin inner disk at 10 cavity [32], and insideAU the [33]. cavity The it observed gap hascircumbinary width a disks and [34]. nearly binary separation equal are mass consistent companion with theoretical with studies a on separation of 8 companions. For example, CoKu Tau Young Planets turbulent disks (e.g. [30; 31]). PoS(BASH2015)004 Zhaohuan Zhu =0.01, upper panels) α , and dust concentration in 3 − 10 . α 6 ) [58; 59]. The vortex is also unstable in a disk with magnetic fields [60]. By considering The disk surface density for the gas (leftmost panels) and dust in viscous ( 5 − 10 To explain the large scale lopsided dust structure observed in transitional disks, particle trap- On the other hand, the vortex can dissipate quickly in a disk even with a small viscosity ∼ ν such vortices can explain ALMA observations. non-ideal MHD effects which significantly suppressbe the present turbulence, for [61] found thousands that of the vortex in can a disk with equivalent ping in the azimuthal directionlong by lived vortices and is proposed. can efficientlyby It trap various is hydrodynamical known dust that instabilities particles anticyclonic in [46;the vortices disks gap 47]. are [48], edge in is the subjectformation Although scenario [49; to 50]. of vortices the gap can Spiral Rossby shocks opening be waveleading excited by generated instability by to planets, a (RWI) gap planet which opening. push can thebump This naturally which disk process has lead material a also away to vortensity from piles minimum vortex the and upping planet, is in material subject 3-D at to vortices the the has RWI gap also [51;dust been 52; edge, dynamics studied 53; leading 54; using [56; to 55]. 3-D 57], hydrodynamical Particle a which trap- globalthan density suggests simulations 100 that including increase particles in the at dust certain surface sizes density could within have the a vortex. ( factor of more and inviscid (lower panels)particles simulations. from the In outer the disk toparticles viscously the are accreting inner trapped disk disk, in while the the leaves gap big accretion edge particles vortex flow at and the carries planet gap co-orbital small edge. region. In ([3]) the3.2 inviscid disk, Large Scale Asymmetric Structures Figure 4: Young Planets Also by constructing a 1-Dplanet can model, blow small [45] dust has away during suggestedasymmetric the that filtration within process. radiation the Considering pressure the gap, flow from 2-D patternpressure the is may simulations highly accreting be including needed dust to growth, better understand fragmentation, the and dust radiation filtration process. PoS(BASH2015)004 Zhaohuan Zhu rotational symmetry are 100 AU which is too high o ∼ R 200 K at ∼ 7 ) become spiral shocks which propagate at speeds faster than the local J M Recent 3-D simulations have suggested that the pitch angle formula derived from the linear Overall, companion-induced spiral arms not only pinpoint the companion’s position but also Since these disks also have holes at the center, one scenario to explain both spiral patterns and However, there are two difficulties in explaining the observed spiral patterns using spiral wakes Recent high-resolution direct imaging observations have revealed spiral structure in proto- Recent theoretical works start to include dust feedback to vortices (e.g. [62; 63; 64; 65]) theory does not applyhigh to mass the planets (e.g. high 1 planet mass cases [73; 74]. Spiral wakes that are excited by provide three independent ways (pitchto angle, constrain separation the between companion’s two mass. arms, and contrast of arms) for any realistic disk structure.contrasts than Second, suggested the by the observed synthetic spiralsimulations observations with arms based the on exhibit assumption two much that dimensional higher (2-D) the planet-disk disk brightness is in vertical hydrostatic equilibrium [72]. sound speed [75; 76].non-linear Thus, extension the of pitch the angle difficulty spiralcomplicated above shock non-hydrostatic can 3-D theory. structure be which The alleviated can spiral by leadsurface. arms to considering strong (especially the Since density the perturbation NIR at inner observations theeffect arms) disk is alleviates have the sensitive second to difficulty the mentionedtant density above. role perturbation Thermodynamics on can at the also the spiralthe play disk planet structure an surface, (see impor- [77; also this 78]. [79]).modeling Furthermore, [74] Thus has only a shown one secondary that planet planet-induced inner innering is arm spiral observations necessary arms is of to can SAO also explain explain 206462 recent excited two and NIRarms spiral by MWC direct in arms. 758. imag- this However, model, Detailed since it the ismechanisms, planets difficult e.g. are to another outside explain planet the the or spiral gaps photoevaporation, discovered are at needed small to radii explain these in gaps. these disks. Other gaps/holes is that these disksgaps harbor and excite low-mass spiral companions waves (e.g. at the young same time. planets) which can open induced by a planetsuggests inside that the the disk gaps. has a relative First, high temperature, the e.g. large pitch angle of all the observed spiral arms present in both SAO 206462 andWhirlpool MWC 758, M51). similar to The the spiral grand arms design also in exhibit a a spiral high galaxy contrast (e.g. against the the background disk. planetary disks around Herbig Ae/Bethe stars NIR (e.g. polarized SAO intensity 206462, images, [18; 19], two MWC spiral 758, arms [70; with 71]). roughly In 180 3.3 Spiral Structures and consider the effect ofband gas ALMA gravity and on EVLA observations particlestructure start concentration [68; to [66; 69]. reveal 67]. particle Eventually, size with Observationally,to distributions ALMA’s multi- high probe within spatial the the anticyclonic and lopsided gas spectral motion resolution,or directly we disprove through may the velocity be scenario channel able maps, thatasymmetric which particle structures. could concentration confirm by vortices is responsible to these large scale Young Planets PoS(BASH2015)004 = ˙ (4.1) [73]. M 2000 ). The ∼ 5 α ; enough to 1 Zhaohuan Zhu − yr

M 8 − planet accreting at 10 J planet can be brighter than ∼ J bands) because the emission ˙ M N , ,

M L , 3 0 − L 10 around a 1 M × 1 5 − . planet has a maximum temperature of 1 yr J

8 = M ˙ M J 10 J − M 2R G bands), this disk is as bright as a late M-type = K , disk L H , J ) and distinguish them from brown dwarfs or hot high mass planets, J source within LkCa 15 [81] could be a CPD undergoing magnetospheric α planet within 1 Myr) around a 1 M has an accretion luminosity of J planet with a “hot start”. To use direct imaging to find the accretion disks around 1 − J yr

M Detailed SEDs for CPDs accreting at different accretion rates are shown in Figure Besides thermal emission, CPD can also be probed by dust continuum [86], velocity channel Features in protoplanetary disks (e.g. gaps, large scale asymmetry, spiral arms) may have Accreting circumplanetary disks can release a large amount of thermal energy due to the 8 − accretion. Table 1 summarizes recent detections ofpredictions point sources based in protoplanetary on disks, [73]. and model 1 For Jupiter the radii. theoretical predictions, To derive thegiven references the disk for absolute inner each magnitudes, source. radius the We is fitmagnitudes distance assumed the at and model to other to disk be wavelength the inclination bands. observed arewell. L’ Generally, band from the magnitudes, the and model predict agrees with observations reasonably maps [87], or disk chemical abundances [88].we With could ALMA’s high probe sensitivity all and these spatial three resolution, signatures of CPDs. 5. Conclusion already implied young planets ingaps and disks. finer features, With which ALMA can limit andtime, the Extreme-AO, potential we parameter we also space start have of young great to planets.disks. hope see At In to narrower the the same detect future, young both indirect planetsoccurrence and directly of direct young through methods planets, will accreting which allow will circumplanetary us shedand to light determine on reveal the the distribution how decades-old and problem young ofbillions planetary planet of formation, systems years after can they evolve were born. into older ones such as our , 10 which is as bright as a late M-type/early L-type brown dwarf. Circumplanetary disks only accreting atthe 10 planet itself.form A a moderately 10 M accreting circumplanetary disk ( recently discovered H or a 10 M low mass planets (e.g., 1 M small size and deep potential of the planet [73]. A disk around a 1 M it is crucial to obtain photometry at mid-infrared bands ( Young Planets 4. Direct Signatures of Young Planets K, and at NIR wavelengths ( from circumplanetary disks falls off moredwarfs slowly or planets. towards longer When wavelengths the than giant planetthe those has of CPD, strong brown magnetic leading fields (>100 to Gauss), magnetosphericadditional they can blue accretion truncate component [80; from 73]. the5). hot Besides spot Magnetospheric the on accretion emission the around from star T-Tauri the is stars disk, also leads present an to (the strong right line panel emission of (e.g. Figure H PoS(BASH2015)004 , 0 L , K , H , J Zhaohuan Zhu 0.16 ± 5 . 0.1 13.33 0.5 0 ± ± ± Full Disk 0.11 13.92 0.5 13.2 ± ± 9 0.32 >15.43 LkCa 15 from [81] HD169142 from [82] ± HD100546 from [83; 84] J H K L’ M N 14.8 14.66 13.82 12.2 11.62 10.12 20.66 18.4116.09 16.50 15.92 13.9 14.96 13.05 13.2 11.37 12.54 11.04 ) yr 6 6 / Magnitudes of Accreting Circumplanetary Disks compared with Observations − − 5 2 J − 10 10 M ( × × ˙ M The SEDs of accreting circumplanetary disks (black curves) and young planets (red and blue bands. Left: the circumplanetary disk extends all the way to the planet surface. Right: the disk is M Table 1: N , and The. 10 The. 2 The. 7 Obs. 14.2 Obs.Obs. >13.8 19.4 12.2 M truncated by the magnetic field fromFor the comparison, young the planet SED and of thedetections GM disk for Aur is HD undergoing is 169142b magnetospheric shown and accretion. as HD100546b. the green curve. The blue and green dots/upper limit are Figure 5: curves from [85]). The redfrom curves the are “cold the start” models. SEDsscaled based For to on another 100 the comparison, pc. the “hot At green the start” top curve models, of is while each the panel, the SED the blue of black curves curves the are indicate protostar the GM transmission Aur functions of Young Planets PoS(BASH2015)004 , , Proto- , Circum- , Zhaohuan Zhu Resolving the , , ApJ, 791 (2014), ETY ULLEMOND , A&A, 460 (2006), KRUTSKIE J.P Mid-Infrared Variability Comparison of the Dust , ., C. P. D M. F. 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