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5 Publications visible to you, out of a total of 5
Hot Jupiter engulfment by an early red giant in 3D hydrodynamics

Abstract (Expand)

Hot Jupiters are gas giant planets with orbital periods of a few days and are found in 0.1–1% of Sun-like stars. They are expected to be engulfed during their host star’s radial expansion on the red … giant branch, which may account for observed rapidly rotating and chemically enriched giant stars. We performed 3D hydrodynamical simulations of hot Jupiter engulfment by a 1 M⊙, 4 R⊙ early red giant. Our ‘global’ simulations simultaneously resolve the stellar envelope and planetary structure, modelling the hot Jupiter as a polytropic gas sphere. The hot Jupiter spirals in due to ram-pressure drag. A substantial fraction of its mass is continuously ablated in this process, although the mass-loss rate is resolution dependent. We estimate that this could enhance the surface lithium abundance by up to ≈0.1 dex. The hot Jupiter is disrupted by a combination of ram pressure and tidal forces near the base of the convective envelope, with the deepest material penetrating to the radiative zone. The star experiences modest spin-up (∼1 km s−1), and engulfing a more massive companion may be required to produce a rapidly rotating giant. Drag heating near the surface and hydrogen recombination in the small amount of unbound ejecta recorded in the simulation could power an optical transient, although this needs to be confirmed by a calculation that has adequate resolution at the stellar surface.

Authors: Mike Y. M. Lau, Matteo Cantiello, Adam S. Jermyn, Morgan MacLeod, Ilya Mandel, Daniel J. Price

Date Published: 1st Feb 2025

Publication Type: Journal

Dusty Common Envelope Evolution

Abstract (Expand)

We present the first hydrodynamical simulations of common envelope evolution that include the formation of dust and the effect of radiation pressure on dust grains. We performed smoothed particle … hydrodynamics simulations of the CE evolution for two systems made of a 1.7 M⊙ and 3.7 M⊙ AGB star primary with a 0.6 M⊙ binary companion. The results of our calculations indicate that dust formation has a negligible impact on the gas dynamics essentially because dust forms in the already unbound material. The expansion and cooling of the envelope yield very early and highly efficient production of dust. In our formalism, which does not consider dust destruction, almost 100% of the available carbon that is not locked in CO condensates in dust grains. This massive dust production, thus, strongly depends on the envelope mass and composition, in particular, its C/O ratio, and has a considerable impact on the observational aspect of the object, resulting in a photospheric radius that is approximatively one order of magnitude larger than that of a non-dusty system.

Authors: Lionel Siess, Luis C. Bermúdez-Bustamante, Orsola De Marco, Daniel J. Price, Miguel González-Bolívar, Chunliang Mu, Mike Y. M. Lau, Ryosuke Hirai, Taïssa Danilovich

Date Published: 1st Dec 2024

Publication Type: Journal

From spherical stars to disk-like structures: 3D common-envelope evolution of massive binaries beyond inspiral

Abstract

Not specified

Authors: Marco Vetter, Friedrich K. Röpke, Fabian R. N. Schneider, Rüdiger Pakmor, Sebastian T. Ohlmann, Mike Y. M. Lau, Robert Andrassy

Date Published: 1st Nov 2024

Publication Type: Journal

Dust formation in common envelope binary interactions – II: 3D simulations with self-consistent dust formation

Abstract (Expand)

We performed numerical simulations of the common envelope (CE) interaction between thermally-pulsing asymptotic giant branch (AGB) stars of 1.7 M⊙ and 3.7 M⊙, respectively, and a 0.6 M⊙ compact companion. … We use tabulated equations of state to take into account recombination energy. For the first time, formation and growth of dust is calculated explicitly, using a carbon dust nucleation network with a C/O abundance ratio of 2.5 (by number). The first dust grains appear within ∼1–3 yrs after the onset of the CE, forming an optically thick shell at ∼10–20 au, growing in thickness and radius to values of ∼400–500 au over ∼40 yrs, with temperatures around 400 K. Most dust is formed in unbound material, having little effect on mass ejection or orbital evolution. By the end of the simulations, the total dust yield is ∼8.4 × 10−3 M⊙ and ∼2.2 × 10−2 M⊙ for the CE with a 1.7 M⊙ and a 3.7 M⊙ AGB star, respectively, corresponding to a nucleation efficiency close to 100%, if no dust destruction mechanism is considered. Despite comparable dust yields to single AGB stars, in CE ejections the dust forms a thousand times faster, over tens of years as opposed to tens of thousands of years. This rapid dust formation may account for the shift in the infrared of the spectral energy distribution of some optical transients known as luminous red novae. Simulated dusty CEs support the idea that extreme carbon stars and ‘water fountains’ may be objects observed after a CE event.

Authors: Luis C Bermúdez-Bustamante, Orsola De Marco, Lionel Siess, Daniel J Price, Miguel González-Bolívar, Mike Y M Lau, Chunliang Mu, Ryosuke Hirai, Taïssa Danilovich, Mansi M Kasliwal

Date Published: 30th Jul 2024

Publication Type: Journal

Expansion of Accreting Main-sequence Stars during Rapid Mass Transfer

Abstract (Expand)

Accreting main-sequence stars expand significantly when the mass accretion timescale is much shorter than their thermal timescales. This occurs during mass transfer from an evolved giant star onto a … main-sequence companion in a binary system and is an important phase in the formation of compact binaries including X-ray binaries, cataclysmic variables, and gravitational-wave sources. In this study, we compute 1D stellar models of main-sequence accretors with different initial masses and accretion rates. The calculations are used to derive semianalytical approximations to the maximum expansion radius. We assume that mass transfer remains fully conservative as long as the inflated accretor fits within its Roche lobe, leading stars to behave like hamsters, stuffing excess material behind their expanding cheeks. We suggest a physically motivated prescription for the mass growth of such "hamstars," which can be used to determine mass-transfer efficiency in rapid binary population synthesis models. With this prescription, we estimate that progenitors of high-mass X-ray binaries and gravitational-wave sources may have experienced highly nonconservative mass transfer. In contrast, for low-mass accretors, the accretion timescale can exceed the thermal timescale by a larger factor without causing significant radial expansion.

Authors: Mike Lau, Ryosuke Hirai, Ilya Mandel, Christopher A. Tout

Date Published: 24th Apr 2024

Publication Type: Journal

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