PoS()014 http://pos.sissa.it/ ce. s the Chandrasekhar and its ), the accreted material (chemical tant step to clarify this point is to binary systems. The characteristics ting white dwarfs, but the exact sce- Institut d’Estudis Espacials de analysis of the outcome of accretion nary system (mass accretion rate), are ques de la Mediterrània) arcelona) and Institut d’Estudis ive Commons Attribution-NonCommercial-ShareAlike Licen ∗ [email protected] [email protected] composition) and those related with the properties of the bi and the implications for thethermonuclear growth explosion of is the presented. toward Thermonuclear (type Ia) supernovae are explosionsnario in leading accre to these explosionsunderstand the is behaviour still of unclear. accreting whiteof dwarfs An the in impor white close dwarf (mass, chemical composition, luminosity crucial for the further evolution towards the explosion. An Speaker. ∗ Copyright owned by the author(s) under the terms of the Creat c Supernovae: lights in the darkness (XXIIIOctober Trobades 3-5 Científi 2007 Mao, Menorca, Spain Margarita Hernanz Accreting White Dwarfs Institut de Ciències de l’Espai (CSIC-IEEC),Espacials Bellaterra de (B Catalunya, Barcelona, Spain E-mail: Jordi José Departament de Física i Enginyeria Nuclear,Catalunya, EUETIB, Barcelona, UPC Spain and E-mail:

PoS(SUPERNOVA)014 . ⊙ Margarita Hernanz rf will be discussed in next logical tools, as crucial con- upernova explosions: the single h smaller than 8-11 M rging of two white dwarfs is the ed matter is pure . In the ccretion rate) are strongly depen- result of the explosion of a - l explosion, in case this is the final f accretion and initial white dwarf ter from a or giant s, because is not seen in vitational force, show a wide range r H, He -with some metals- or CO) ure He or a mixture of carbon and ated with accretion of H-rich matter, l purposes. In contrast, core colllapse henever they are isolated. However, axy, and as the triggering mechanism on; these are out of the scope of this ng phenomena can happen, like resting phenomena, but there is a long d by accretion, and its link to the final degenerate and the double degenerate exploding white dwarf. The mass and s initial luminosity, are also crucial for s paper we concentrate on the scenario oepke’s contribution [37]). y for carbon ignition; this occurs either n addition, there are not yet successful e progenitor is extremely large. generate conditions. Therefore, it is ex- orm, in agreement with the observations, , explosions. Accretion carbon ignition conditions. Once ignition ed matter is always hydrogen-rich, except 2 There are two basic scenarios for the progenitors of type Ia s The influence of accretion on the final outcome of the white dwa In spite of the importance of type Ia supernovae both as cosmo It is widely accepted that thermonuclear supernovae are the White dwarfs are the final stages of the evolution of stars wit when the companion is a helium [20] and therefore accret paper, but are treated in other papers of this volume (e.g., R 2. Scenarios of SNIa degenerate scenario, where thecompanion, white and dwarf the is double accretingresponsible degenerate for mat the scenario, final explosion. where In the the first me case, accret double degenerate scenario, accretedoxygen, matter depending on can the be type of either white dwarf p companion. section. Here we justsince mention it the is observational problem a rel crucialscenarios. point to Accretion disentangle of between the H-rich single material poses some problem pected that the properties of such explosions are quite unif occurs, other problems occur, related to the flame propagati oxygen (CO) white dwarf, once itat reaches the the center critical densit of the star or off-center, always in stronglyallowing de the use of them assupernovae, standard candles where for a cosmologica massive starof explodes observational because properties, of since the the range gra of masses of th tributors to the chemical and dynamicalfor evolution star of formation, the their Gal exactsimulations scenario of the is explosion still (see unknown. theissue, review with I by a [15]). special In emphasis thi onfate the of fundamental role the playe white dwarf.and the The rate type at of whichdent material matter on accreted falls the (eithe onto type of thechemical interacting white composition binary dwarf of hosting (mass the the white a potential dwarfits itself, outcome. as well There as it isconditions, a such that complicated it interplay is not between straightforward type to reach o the The final fate ofwhen such they stars belong is to just interactingexplosions binary cooling and supernovae systems, to of more the invisibility, thermonuclear exciti w class, i.e. and complicated path from theoutcome onset of of the accretion evolution. up to the fina Accreting White Dwarfs 1. Introduction of matter from the companion star is at the origin of such inte PoS(SUPERNOVA)014 k 10 − 8 ∼ Margarita Hernanz ing white dwarfs, depending er which the white dwarf pro- of the white dwarf star: Chan- bon and leaves ONe cores, is a of the basic properties defining f can form is between tes, burning can occur in steady at relatively low-mass CO white elf, e.g., mass and chemical com- e as type Ia supernovae, since they tonation models of Chandrasekhar n the inclusion or not of overshoot- t Branch), without carbon ignition to models, some hydrogen should terial at a lower density (than in the ts have been obtained which do not . This hydrogen is predicted to be uring the thermal pulses themselves the single degenerate scenario- and, ted to collapse, because of the effect and thus the mass accretion) rate and he absence of intermediate-mass ele- n top of the white dwarf would drive s arise in this sub-Chandrasekhar sce- cenario is based on the explosion of a /yr for H-accretion [31, 38], the exact re possible for white dwarfs: helium, ]. It is worth mentioning that for larger d a lot of multidimensional works have ies of the intermediate-mass elements; or He accretion, steady burning occurs ed. Large accretion rates are needed to ave been serious attempts to search for , indicative of a giant companion (i.e., ⊙ for the explosion (see for instance [41]). for instance [19] and references therein). M ) 5357 . 3 0 − ⊙ (M/M × 10000 km/s), and its detection is hard at the stages where bul 7 − ∼ 10 × Mg (see for instance [30, 32, 1, 9] and references therein). 066 24 . Two possibilities have been suggested, concerning the mass There is a variety of nuclear burning regimes on top of accret Another issue is to know the properties of the white dwarf its , depending on the treatement of convection (and specially o ⊙ M ing) and mass loss during[36, the 3]. previous Only binary CO evolution white and dwarfs d are are carbon-rich. expected On to be the able contrary, ONe toof white explod electron dwarfs captures are on expec drasekhar and sub-Chandrasekhar scenarios. TheChandrasekhar standard mass s CO white dwarf,dwarfs but could it also has explode. been In claimedthe this final th case, central helium or detonation off-center o carbonThe ignition propagation of responsible the outward carbonChandrasekhar detonation mass through white ma dwarf) alleviates thements problem (such of as t Si and S,mass for white dwarfs instance) (see of for the instance oldnario, [29]). pure since But carbon it other de problem does nothowever, well this reproduce scenario has the not observed been velocit completelybeen ruled devoted out, to an it (e.g., [7, 4] and references therein) 3. Accretion mainly on the accreted mass composition,the the mass mass of transfer ( the whitestate, dwarf. so that For matter is a burnedfulfill narrow at this range the condition: of same rate 3 accretion as ra it is accret value depending on the metallicity offor the mass accretion accreted rates matter; roughly f 10 times larger [5, 6, 16, 18 material expands at larger speeds.hydrogen In in the the last spectra years, of therecompletely type h contradict Ia the supernovae, single and degenerate scenario upper (see limi In fact, there has been detection of circumstellar material single degenerate scenario) in a few cases [10, 33]. position, which are strongly related.carbon-oxygen (CO) Three and compositions oxygen-neon a (ONe).genitor star The undergoes mass either range theand ov AGB leaving (from CO Asymptotic cores, Gian orbit the controversial. super-AGB The phase, mass which range burns for car which an ONe white dwar Accreting White Dwarfs the spectra of type Ia supernovae (absence of hydrogen is one the type I -andbe in stripped particular from Ia- the secondary class).therefore, star some during However, hydrogen the according explosion shouldat -in exist small in velocities the (lower ejecta than [26, 27] PoS(SUPERNOVA)014 ) 3 ) . Adapted 3 . Adapted ⊙ ⊙ , and larger g/cm 4 g/cm max 2 T (10 Margarita Hernanz (10 He H ρ ρ K) K) 8 7 (10 (10 sponding to the steady burning ell temperatures, ytical model in the plane parallel H He ds to the so-called supersoft X-ray ng mass loss and they are strictly l white dwarf mass 1.2 M al white dwarf mass 1.2 M T T ain ignition conditions, both for H- own in Tables 1 and 2; these results the Chandrasekhar mass, without any e intensity of the flashes increases as eing hot because of steady burning of -ray energy range (i.e., below about 1 ) increases as the mass accretion rate reted mass implies higher degeneracy giant envelope, whereas for even larger r accretion (because radiation pressure ow), accumulated matter reaches partial rec K) K) erate scenarios for type Ia supernovae. 7 7 P (10 (10 H , He , 4 min min T T K) K) 8 8 10 ( (10 H , He , max T max T (yr) 9 1.3 3.4 6.03 0.78 22 1.4 2.9 4.36 1.20 50 1.4 2.6 3.63 1.58 (yr) 357 1.5 2.0 2.69 2.57 832 1.6 1.8 2.45 3.09 5828 1.7 1.5 2.04 4.47 rec 1369168640 1.7 1.9 1.3 1.2 1.86 1.66 5.37 8.32 199 4.1 11.5 1.55 0.85 471 4.3 9.8 1.29 1.17 P 9081 5.0 6.7 0.98 2.34 1124 4.5 8.7 1.15 1.44 rec 22129 5.2 6.1 0.93 2.82 P 8 7 9 10 10 − − − 6 8 7 /yr) − − 8 7 9 − − − ⊙ /yr) − − − 6 7 10 10 10 10 10 ⊙ − − 10 10 10 M 10 10 10 × × × ( Properties of models with weak H-shell flashes, for an initia Properties of models with weak He-shell flashes, for an initi × × M 10 10 ˙ × × × 5 2 5 ( 5 2 M ˙ 2 5 5 M Whenever the accretion rate is smaller than the values corre An interesting case of steady burning of hydrogen correspon diminishes, because a larger massand needs He-rich accretion. to be As accreted athe to consequence accretion of att rate this decreases; increase, theand th thus reason a is stronger that flash a [18] (as larger seen acc by the larger maximum sh from José, Hernanz & Isern [18] degeneracy and weak flashes occur. These flashes are not drivi sources (SSSs); these objects emitkeV), just and in are the interpreted “super as soft” hothydrogen) X white [39]. dwarf Provided that photospheres, they b have enoughcatastrophic time mass-loss to event, reach they are viable single degen regime, but larger than some critical values (explained bel periodic. The general properties ofwere these obtained weak by flashes José, are Hernanzapproximation. sh & It Isern is [18], shown with that a the semi-anal recurrence period ( rates the Eddington limit isforce reached, counteracts gravitational which force). inhibits furthe accretion rates, the envelope expands and behaves like a red Table 2: Table 1: Accreting White Dwarfs from José, Hernanz & Isern [18] PoS(SUPERNOVA)014 , 8 ⊙ − /yr, ⊙ 10 1M ) along . M × 1 He 10 ρ ∼ − 10 and − H , obtained). The Margarita Hernanz 9 ρ − min T 10 changes when double − H ∼ , is worth noticing that H rec max P gth of the H or He flashes T / He , cur are ekhar mass are not possible for on top of an accreting CO white res, es is about 400 times larger than e flashes are expected for a range cretion rates larger than 5 rec lope (for a given accreted mass) mework of both one dimensional ) and densities ( an prevent the growth of the white flashes are probable [2, 34]. More P natively, weak He flashes allowing cretion rates, flashes are not weak on problematic for H (see [18] and onditions and drive a hydrodynamic ength of the flash is the ratio of the He g and ensuing strong flashes are dif- ion: the larger the initial white dwarf ulation of He. Therefore, one indirect ornambe and Piersanti et al. [2, 34]). T influences the evolution of the bottom s for which there is a strong He flash flashes have small ratios, whereas the y of the white dwarf and on the metal- hase” longer; see [16, 18] for details). aneously along a spherical shell. This bout the final flashing of He are given ash is expected whenever the accretion atio r white dwarf masses below ore, to a milder flash [18]. On the other t in 1D simulations with spherical sym- ing propagation; see below). Therefore, nova explosions occur, leading to a large ties, from hundreds to thousands of km/s and H T ( He 5 T /yr [29, 40], for any initial white dwarf mass. For ⊙ and M H 9 T − and 10 8 − 10 × 5 ∼ Up to now we have described direct accretion of H and He, but it The critical accretion rates for surface degenerate burnin Coming back to direct accretion, we have shown that the stren The further hydrodynamical evolution after a strong He flash /yr, would happen [28]. ⊙ effect of the initial white dwarfmass, mass the goes in higher the the sameand pressure direct then at the stronger the the“on base flash. phase” of duration Another the to indication the accretedmilder of recurrence enve flashes the period: have str the larger strongest ratiosThe (i.e., average they values stay of shell in temperatures the “on p Accreting White Dwarfs difference between the maximum and minimum shell temperatu burning (steadily or through weak flashes) leadsway to to the accrete accum He is throughof weak direct H flashes; H in accretion fact, doublethe rates, H-H complete e.g., hydrostatic those simulations mentioned fromAs Cassisi, above shown Iben as in & n Tables T 1 andthat 2, of H the flashes, typical for period a of given single (large) accretion He rate; flash but the r the period are shown in Tables 1 and 2. the exact values depending on thelicity initial of mass the and accreted luminosit matter [25].rate Concerning ranges He, a between strong fl smaller accretion rates, a strong flash is again predicted fo increase of visual luminosity and mass-loss[13, at large 17]. veloci For He accretion, there is a rangeweak of flashes accretion rate leading to a growing CO core towards the Chandras flashes are considered. The existence ofHe a top layer, hydrogen leading shell to a shorter recurrence period and, theref increases with decreasing accretionanymore, rate. because accumulated For matter can lowevent, reach enough with degenerate potential ac c mass loss. For H-rich mass accretion, (probably leading to a He detonation, i.e., supersonic burn this range of mass accretion rates. ferent for H and He. The lower limits for which weak H flashes oc hand, the accumulation of He as a consequence of H accretion c dwarf mass up to the Chandrasekhardetails, limit, in since the dynamical framework He ofbelow, hydrodynamical but simulations, just for a direct He accretion. M dwarf has been subject toand multidimensional debate simulations. during It many is years,metry, worth ignition in noticing can tha the only fra occur either at the center or simult but no He flash occurs iffor the the white increase dwarf of is the more white massive; dwarf alter mass, as in the case of He ac PoS(SUPERNOVA)014 O 18 ) γ , ones at α α C( 14 ) ν ). , ⊙ Margarita Hernanz − N(e 14 N, whereas for solar or larger effect of accretion onto white the main characteristics of the e of accretion rates is not clear 14 fs with initial sub-Chandrasekhar er, Piersanti, Cassisi & Tornambe of the nucleosynthesis constraints ible for the final C ignition, at the ble detonation, whereas in 2D they avoided (leading to a recurrent He he NCO reactions are not included; nation induces a carbon detonation wever, it is worth reminding that the ep the He shell hot enough to avoid quence is that the He layer is heated rmed as a consequence of the strong fs, of 0.6 and 0.8 M detonation, indicated that C was not he white dwarf spin-up caused by ac- eration of the ferential rotation made it ignite under al 1D works (e.g., [29, 40]) tried first rarefaction effects not included in their enario is. For instance, the presence of ealistic initial models of white dwarfs. simulations [24], they concluded that a nduced chemical mixing; they deduced ding to the so-called double detonation r [23], who analyzed the consequences ), which compete with the 3 t an inward C detonation wave; instead l, requiring multidimensional analyses; elated to the details of the burning prop- which deserves particular attention (see enough 3 , but was prevented in less massive white − e ignition, also plays a very important role ⊙ ld for triggering the NCO reactions (notice ns seem quite robust, and the predictions of g cm 6 6 As a summary, the outcome of He accretion in the critical rang The final fate of all the scenarios described above, as well as Last but not least: an important factor which determines the N in the accreted material is critical, since it allows the op in fact, the initial stages of He ignition play ato crucial elucidate role if a HeHe detonation wave flash. propagating outwards A fo relatedat issue the is core to envelope determine interface, if propagatingsupernova inwards the [29]. and initial lea More He recent deto mass studies devoted accreting to at CO the white criticalignited dwar regime at the leading core-envelope to interface, external soa He that compressional there shock was wave no propagatingcenter inwards or was near it respons [21, 41, 12]. Accreting White Dwarfs instantaneous ignition throughout a shell seems unphysica for instance [7] and [4] and references therein). The origin at all. Just as anof illustration, an let’s off-center mention He Livne detonation: & incould Glasne neither 1D confirm they nor did exclude it, not but obtain theyanalysis mentioned a most that dou probably would prevent it.double In detonation later occurred numerical for masses larger than 1.2 M 1D and 2D models agreeon quite the well type (see of [22]; burning a propagation recent can be analysis found in [8]). ensuing type Ia explosion -whenever it occurs-agation, are which tightly are r reviewed by Roepke inpresupernova this evolution, volume leading [37]. to Ho the initial stageson of the th further development of14 the explosion, whatever the sc dwarfs. Fortunately, the gross nucleosynthesis predictio low temperatures and high densities [11,and 41]. ignition density The becomes main lower conse thanthis in could the prevent models the where development t of[35] a obtain strong that He the flash. NCOstrong energy Howev electron contribution degeneracy, is and not thus able aThe to He ke reason flash is results, for that r for low initial metallicities there is not (NCO) reactions (above the density threshold 10 that their models are for sub-Chandrasekhar mass white dwar metallicities the densities attained are below the thresho dwarfs is rotation. Yoon & Langercretion [42] of studied angular the momentum, effect and of the t that further the rotationally heating i of theless He degenerate envelope by conditions, friction and relatednova thus to explosion He dif instead of detonation a might type be Ia supernova). PoS(SUPERNOVA)014 eded to the years (for an 5 f the hydrogen, 10 years of classical sion is expected; Margarita Hernanz 5 × 10 − 4 mbiotic recurrent 07-61593 and AYA2007- 10 (the maximum mass of a CO ∼ ⊙ n the Galaxy) are potential type s why it belongs to the recurrent cta. But this is a long standing n leading to nova outbursts, but erves attention, specially because d. This scenario is different from ion, for large accretion rates, e.g. 1M al mass to develop a nova outburst . h (very close to the Chandrasekhar previous epoch of steady burning or tes. Recent models by Hernanz & a consequence, the accretion rate in s. Its orbital period is 456 days and rf grows towards the Chandrasekhar 1 ted to increase (and not decrease) as nion is a main sequence star and the ite dwarf massive enough, the Chan- ade of ONe, and not of CO, according seems not to be in contradiction with nario. But a problem remains with this ∼ apers. d to explain the short recurrence period e in 2006. It was observed at practically t explode as a type Ia supernova. There ies of RS Oph, with white dwarf initial ion related with it: the symbiotic recur- ce periods anges between 3 and 7 7 /yr. An important result is that the accreted masses are ⊙ M 8 − , typically, after each eruption. The corresponding time ne 10 /yr). ⊙ − ⊙ M 7 M and accretion rates (of matter with solar composition, from − 6 7 − ⊙ 10 − × 10 ). An additional problem with this scenario is how to get rid o × ⊙ /yr, there is not degenerate H-burning and thus no nova explo ⊙ M 38 M . 7 1 − − 10 − 35 RS Oph has undergone various recorded nova outbursts (that’ There is a particular scenario for type Ia supernova that des This research has been funded by the spanish MEC grants ESP20 Therefore, RS Oph and its relatives (just a few -less than 5- i . 6 1 nova − ∼ nova class), with a recurrence period ofall 21 years, wavelengths, the spanning last the on rangethe from companion radio of to the hard white X-ray the dwarf scenario is of a “standard” red classical giantperiods star, novae, - with where and a the thus win compa orbitalRS separations Oph - is are much much larger smaller. andmuch the shorter As (some time decades, needed instead to of the accrete typical the recurren critic there is a lot of recent and accurate observational informat with the peculiarity that thea mass consequence of the of white the dwarf explosion.drasekhar is mass Therefore, expec can for be an reached initial in wh a reasonable amount of time. rent nova RS Oph. This phenomenon is related with H-accretio reach the mass limit, i.e., to reach explosion conditions, r novae). According to what10 was mentioned in the previous sect Accreting White Dwarfs 4. A particular scenario for type Ia supernovae: the RS Oph sy companion) about 2 larger than the ejected ones, so that the mass of the white dwa mass; it increases by 10 however, if the initial massmass), of the the explosion white occurs dwarfJosé is even [14], large for have enoug such successfully reproduced large the accretion global ra propert masses 1.35 and 1.38 M which has been observedproblem in of large the amounts single-degenerate in scenario,the the which, observations however expanding (see section eje 1), according to some recent p Acknowledgments Ia candidates, in the framework ofscenario: the a single white degenerate dwarf sce of such largeto initial standard mass stellar should be evolution; m then itis would not collapse a and clear no way tovery solve weak this flashes, conflict, allowing for unless the there growth was of some the mass from accretion rate of 2 core ”at birth”) to the values of( the white dwarf mass require PoS(SUPERNOVA)014 , , , 2008, dwarfs , 1999, GB stars and ion densities , 1998, ApJ, , 2007, Journal ernovae ons Margarita Hernanz . 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