Common envelope evolution and triple dynamics as potential pathways to form the inner white dwarf + brown dwarf binary of the triple star system Gaia 0007−1605

Lagos, Felipe; Zorotovic, M.; Schreiber, M. R.; Gänsicke, B. T.

doi:10.1093/mnras/stac3675

Cited by 2 publications

(1 citation statement)

References 48 publications

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“…Only a few planets and planet candidates have been detected around white dwarfs (Gänsicke et al 2019;Vanderburg et al 2020;Blackman et al 2021), and just one of them is located at a distance where it could have survived the evolution of its host star (Blackman et al 2021). The others must either have scattered inwards (Maldonado et al 2021), which would imply the existence of additional planets, reached large eccentricities through angular momentum exchange with a distant tertiary (O'Connor et al 2021;Muñoz & Petrovich 2020;Stephan et al 2021), survived common envelope evolution (Lagos et al 2021(Lagos et al , 2023, or be second-generation planets formed in a latter circumstellar disc (Perets 2010;Kluska et al 2022;Ledda et al 2023).…”

Section: Discs and Giant Planets Around Intermediate-mass Starsmentioning

confidence: 99%

Planet formation around intermediate-mass stars

Ronco,

Schreiber,

Villaver

et al. 2024

A&A

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The study of protoplanetary disc evolution and theories of planet formation has predominantly concentrated on solar- (and low-) mass stars since they host the majority of confirmed exoplanets. Nevertheless, the confirmation of numerous planets orbiting stars more massive than the Sun (up to sim 3\ has sparked considerable interest in understanding the mechanisms involved in their formation, and thus in the evolution of their hosting protoplanetary discs. We aim to improve our knowledge of the evolution of the gaseous component of protoplanetary discs around intermediate-mass stars and to set the stage for future studies of planet formation around them. We study the long-term evolution of protoplanetary discs affected by viscous accretion and photoevaporation by X-ray and far-ultraviolet (FUV) photons from the central star around stars in the range of 1 - 3 considering the effects of stellar evolution and solving the vertical structure equations of the disc. We explore the effect of different values of the viscosity parameter and the initial mass of the disc. We find that the evolutionary pathway of protoplanetary disc dispersal due to photoevaporation depends on the stellar mass. Our simulations reveal four distinct evolutionary pathways for the gas component not reported before that are a consequence of stellar evolution and that likely have a substantial impact on the dust evolution, and thus on planet formation. As the stellar mass increases from one solar mass to sim 1.5 - 2 the evolution of the disc changes from the conventional inside-out clearing, in which X-ray photoevaporation generates inner holes, to a homogeneous disc evolution scenario where both inner and outer discs formed after a gap is opened by photoevaporation vanish over a similar timescale. As the stellar mass continues to increase, reaching sim 2 - 3 we identify a distinct pathway that we refer to as revenant disc evolution. In this scenario, the inner and outer discs reconnect after the gap opened. For the largest masses, we observe outside-in disc dispersal, in which the outer disc dissipates first due to a stronger FUV photoevaporation rate. Revenant disc evolution stands out as it is capable of extending the disc lifespan. Otherwise, the disc dispersal timescale decreases with increasing stellar mass except for low-viscosity discs.

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Section: Discs and Giant Planets Around Intermediate-mass Starsmentioning

confidence: 99%

Planet formation around intermediate-mass stars

Ronco,

Schreiber,

Villaver

et al. 2024

A&A

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The C/N ratio from FUV spectroscopy as a constraint on evolution of the dwarf nova HS 0218 + 3229

Toloza

Gänsicke

Guzman-Rincon

et al. 2023

Monthly Notices of the Royal Astronomical Society

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White dwarfs that accrete from non-degenerate companions show anomalous carbon and nitrogen abundances in the photospheres of their stellar components have been postulated to be descendants of supersoft X-ray binaries. Measuring the carbon-to-nitrogen abundance ratio may provide constraints on their past evolution. We fit far-ultraviolet spectroscopy of the cataclysmic variable HS 0218+3229 taken with the Cosmic Origins Spectrograph using Markov Chain Monte Carlo methods, and found the carbon-to-nitrogen ratio is about one tenth of the Solar value ($\mbox{$\log \mathrm{[C/N]}$}=-0.56\pm 0.15$). We also provide estimates of the silicon and aluminium abundances, and upper limits for iron and oxygen. Using the parameters we derived for HS 0218+3229 we reconstruct its past. We calculated a grid of MESA models and implemented Gaussian process fits in order to determine its most likely initial binary configuration. We found that an initial mass of the donor of $M_{\rm donor;i}=0.90-0.98,\mbox{$\mathrm{M}_{\odot }$}$ and an initial orbital period of Porb; i = 2.88 d (Porb; i = 3.12 − 3.16 d) for an assumed initial white dwarf mass of $\mbox{$M_{\mathrm{WD}}$}_\mathrm{;i}=0.83\, \mbox{$\mathrm{M}_{\odot }$}$ ($\mbox{$M_{\mathrm{WD}}$}_{\rm ;i}=0.60\, \mbox{$\mathrm{M}_{\odot }$}$) can replicate the measured parameters. The low mass ratio, $M_{\rm donor;i} / \mbox{$M_{\mathrm{WD}}$}_{\rm ;i} =1.08-1.18\, (1.5-1.63)$, suggests that the system did not go through a phase of hydrogen-burning on the white dwarf’s surface. However, we can not exclude a phase of thermal timescale mass transfer in the past. We predict that HS 0218+3229 will evolve below the ≃ 76.2 ± 1 min period minimum for normal cataclysmic variables.

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Common envelope evolution and triple dynamics as potential pathways to form the inner white dwarf + brown dwarf binary of the triple star system Gaia 0007−1605

Cited by 2 publications

References 48 publications

Planet formation around intermediate-mass stars

Planet formation around intermediate-mass stars

The C/N ratio from FUV spectroscopy as a constraint on evolution of the dwarf nova HS 0218 + 3229

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