Simulating the Common Envelope Phase of a Red Giant Using Smoothed-Particle Hydrodynamics and Uniform-Grid Codes

Passy, Jean-Claude; Marco, Orsola De; Fryer, Chris L.; Herwig, Falk; Diehl, Steven; Oishi, Jeffrey S.; Low, Mordecai–Mark Mac; Bryan, Greg L.; Rockefeller, Gabriel

doi:10.1088/0004-637x/744/1/52

Cited by 246 publications

(385 citation statements)

References 50 publications

(67 reference statements)

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“…We used a modified version of the grid-based hydrodynamics code enzo (O'Shea et al 2004;Passy et al 2012a;Bryan et al 2014) to run the hydrodynamics simulations. The calculations were performed on a 256 3 grid in the adiabatic approximation with outflow boundary conditions.…”

Section: Methodsmentioning

confidence: 99%

“…The gravitational drag is instead due to gravitational forces between the gas flowing past the planet and the planet itself. Although there is no accurate expression for the gravitational drag in the presence of a density gradient (MacLeod & Ramirez-Ruiz 2015), an approximate expression can be found in Iben & Livio (1993) and Passy et al (2012a):…”

Section: Gravitational Vs Hydrodynamic Dragmentioning

confidence: 99%

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Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

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127

100

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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.

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Section: Methodsmentioning

confidence: 99%

Section: Gravitational Vs Hydrodynamic Dragmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

127

100

View full text Add to dashboard Cite

show abstract

“…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. Since the gravitational potential energy of the companion star scales as a −1 , where a denotes its distance from the core of the red giant, the energy deposition rate in a given range da scales as a −2 .…”

Section: Introductionmentioning

confidence: 98%

Planet formation from the ejecta of common envelopes

Schleicher

Dreizler

2014

A&A

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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.

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“…Also, Bobrick et al (2017), found that jet appearance and quenching during CE can produce transient objects. Other 3D studies focused on the formation of degenerate stars (Sandquist, Taam, & Burkert 2000), the formation of Wolf-Rayet stars (De Marco et al 2003), and the interaction of stellar objects within the CE phase, either by employing Eulerian (Ricker & Taam 2008, 2012 or Lagrangian (Passy et al 2012) meshes.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of jets during the common-envelope phase

Méndez

López-Cámara

Colle

2017

Monthly Notices of the Royal Astronomical Society

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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.

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Simulating the Common Envelope Phase of a Red Giant Using Smoothed-Particle Hydrodynamics and Uniform-Grid Codes

Cited by 246 publications

References 50 publications

Hydrodynamic simulations of the interaction between giant stars and planets

Hydrodynamic simulations of the interaction between giant stars and planets

Planet formation from the ejecta of common envelopes

Dynamics of jets during the common-envelope phase

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