Double Core Evolution. X. Through the Envelope Ejection Phase

Sandquist, Eric L.; Taam, Ronald E.; Chen, Xingming; Bodenheimer, Peter; Burkert, Andreas

doi:10.1086/305778

Cited by 182 publications

(299 citation statements)

References 51 publications

Supporting

Mentioning

282

Contrasting

Order By: Relevance

“…In both simulations this initial configuration results in the giant stars massively overflowing their Roche lobe radii. This is the case with many CE simulations (e.g., Sandquist et al 1998;Passy et al 2012a) and may have some effect on the CE outcome (Iaconi et al, 2016, in preparation). However, in the case of planetary companions, it is likely that the effect of starting close to the surface is minimal: companions as far as 2-3 stellar radii are likely to be captured (Villaver & Livio 2009;Mustill & Villaver 2012), but the angular momentum of the orbit transferred to the primary would confer to it only a relatively minor surface velocity of 1.1 − 1.3 km s −1 for the AGB star and 3.2 − 3.9 km s −1 for the RGB star (this range was found assuming that all the orbital angular momentum of the planet at a distance of 2-3 stellar radii is transferred to the envelope of the giant, and that this envelope rotates rigidly), not too different from our non-rotating initial models.…”

Section: Methodsmentioning

confidence: 95%

“…CE simulations using a variety of techniques (e.g. Sandquist et al 1998;Ricker & Taam 2012;Passy et al 2012a;Nandez et al 2014;Staff et al 2016) have a range of uncertainties and shortcomings (e.g., , but can be used as starting points to determine the nature of star-planet interactions. By running hydrodynamic simulations of the CE interaction between a 10 MJ planet and an RGB or an AGB star, we start addressing numerically aspects of the interaction such as the timescale of the interaction, the final separation or the extent to which the stellar envelope is spun-up.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

127

100

View full text Add to dashboard Cite

We present the results of hydrodynamic simulations of the interaction between a 10 Jupiter mass planet and a red or asymptotic giant branch stars, both with a zeroage main sequence mass of 3.5 M ⊙ . Dynamic in-spiral timescales are of the order of few years and a few decades for the red and asymptotic giant branch stars, respectively. The planets will eventually be destroyed at a separation from the core of the giants smaller than the resolution of our simulations, either through evaporation or tidal disruption. As the planets in-spiral, the giant stars' envelopes are somewhat puffed up. Based on relatively long timescales and even considering the fact that further inspiral should take place before the planets are destroyed, we predict that the merger would be difficult to observe, with only a relatively small, slow brightening. Very little mass is unbound in the process. These conclusions may change if the planet's orbit enhances the star's main pulsation modes. Based on the angular momentum transfer, we also suspect that this star-planet interaction may be unable to lead to large scale outflows via the rotation-mediated dynamo effect of Nordhaus and Blackman. Detectable pollution from the destroyed planets would only result for the lightest, lowest metallicity stars. We furthermore find that in both simulations the planets move through the outer stellar envelopes at Mach-3 to Mach-5, reaching Mach-1 towards the end of the simulations. The gravitational drag force decreases and the in-spiral slows down at the sonic transition, as predicted analytically.

show abstract

Section: Methodsmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

127

100

View full text Add to dashboard Cite

show abstract

“…Three-dimensional (3D) hydrodynamical studies of the CE phase have also been carried out (e.g., Terman, Taam, & Hernquist 1994;Rasio & Livio 1996;Livio & Soker 1988). Sandquist et al (1998) studied the stages when the envelope is ejected. Also, Bobrick et al (2017), found that jet appearance and quenching during CE can produce transient objects.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of jets during the common-envelope phase

Méndez

López-Cámara

Colle

2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Common envelope (CE) is an important phase in the evolution of many binary systems. Giant star / compact object interaction in binaries plays an important role in highenergy phenomena as well as in the evolution of their environment. Material accreted onto the compact object may form a disk and power a jet. We study analytically and through numerical simulations the interaction between the jet and the CE. We determine the conditions under which accreting material quenches the jet or allows it to propagate successfully, in which case even the envelope may be ejected. Close to the stellar core of the companion the compact object accretes at a larger rate. A jet launched from this region needs a larger accretion-to-ejection efficiency to successfully propagate through the CE compared to a jet launched far from the stellar core, and is strongly deflected by the orbital motion. The energy deposited by the jet may be larger than the binding energy of the envelope. The jet can, thus, play a fundamental role in the CE evolution. We find that the energy dissipation of the jet into the CE may stop accretion onto the disk. We expect the jet to be intermittent, unless the energy deposited is large enough to lead to the unbinding of the outer layers of the CE. Given that the energy and duration of the jet are similar to those of ultra-long GRBs, we suggest this as a new channel to produce these events.

show abstract

“…For instance, Livio & Soker (1988) and Rasio & Livio (1996) suggest that the energy is deposited in a very short time, because most of the gravitational energy is released at small orbital separations where the radius decreases quickly. On the other hand, Sandquist et al (1998) estimate that the overall timescale of the process lasts ∼200 days, while De Marco et al (2003) derived timescales of 9−18 yrs until a negligible amount of material remained in the envelope. The numerical simulations by Passy et al (2012), on the other hand, indicate a typical timescale of 100−200 days.…”

Section: Introductionmentioning

confidence: 99%

“…The implications of rotation during the common envelope phase have been explored by Sandquist et al (1998), who showed that a differentially rotating structure, similar to a thick disk, surrounds the binary during an intermediate phase of the CE evolution. A similar thick disk structure was analytically obtained by Soker (1992Soker ( , 2004 and De Marco et al (2011).…”

Section: Introductionmentioning

confidence: 99%

Planet formation from the ejecta of common envelopes

Schleicher

Dreizler

2014

A&A

View full text Add to dashboard Cite

Context. The close binary system NN Serpentis must have gone through a common envelope phase before the formation of its white dwarf. During this phase, a substantial amount of mass was lost from the envelope. The recently detected orbits of circumbinary planets are probably inconsistent with planet formation before the mass loss. Aims. We explore whether new planets may have formed from the ejecta of the common envelope and derive the expected planetary mass as a function of radius. Methods. We employed the Kashi & Soker model to estimate the amount of mass that is retained during the ejection event and inferred the properties of the resulting disk from the conservation of mass and angular momentum. The resulting planetary masses were estimated from models with and without radiative feedback. Results. We show that the observed planetary masses can be reproduced for appropriate model parameters. Photoheating can stabilize the disks in the interior, potentially explaining the observed planetary orbits on scales of a few AU. We compare the expected mass scale of planets for 11 additional systems with observational results and find hints of two populations, one consistent with planet formation from the ejecta of common envelopes and the other a separate population that may have formed earlier.Conclusions. The formation of the observed planets from the ejecta of common envelopes seems feasible. The model proposed here can be tested through refined observations of additional post-common envelope systems. While it appears observationally challenging to distinguish between the accretion on pre-existing planets and their growth from new fragments, it may be possible to further constrain the properties of the protoplanetary disk through additional observations of current planetary candidates and post-common envelope binary systems.

show abstract

Double Core Evolution. X. Through the Envelope Ejection Phase

Cited by 182 publications

References 51 publications

Hydrodynamic simulations of the interaction between giant stars and planets

Hydrodynamic simulations of the interaction between giant stars and planets

Dynamics of jets during the common-envelope phase

Planet formation from the ejecta of common envelopes

Contact Info

Product

Resources

About