Second-generation planet formation after tidal disruption from common envelope evolution
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| Main Authors: | , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866913718124675072 |
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| author | Chamandy, Luke Nordhaus, Jason Blackman, Eric G. Wilson, Emily |
| author_facet | Chamandy, Luke Nordhaus, Jason Blackman, Eric G. Wilson, Emily |
| contents | We propose that certain white dwarf (WD) planets, such as WD 1856+534 b, may form out of material from a stellar companion that tidally disrupts from common envelope evolution with the WD progenitor star. The disrupted companion shreds into an accretion disc, out of which a gas giant protoplanet forms due to gravitational instability. To explore this scenario, we make use of detailed stellar evolution models consistent with WD 1856+534. The minimum mass companion that produces a gravitationally-unstable disc after tidal disruption is $\sim0.15\,\mathrm{M}_\odot$. In this scenario, WD 1856+534 b might have formed at or close to its present separation, in contrast to other proposed scenarios where it would have migrated in from a much larger separation. Planet formation from tidal disruption is a new channel for producing second-generation planets around WDs. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2407_14190 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Second-generation planet formation after tidal disruption from common envelope evolution Chamandy, Luke Nordhaus, Jason Blackman, Eric G. Wilson, Emily Earth and Planetary Astrophysics Solar and Stellar Astrophysics We propose that certain white dwarf (WD) planets, such as WD 1856+534 b, may form out of material from a stellar companion that tidally disrupts from common envelope evolution with the WD progenitor star. The disrupted companion shreds into an accretion disc, out of which a gas giant protoplanet forms due to gravitational instability. To explore this scenario, we make use of detailed stellar evolution models consistent with WD 1856+534. The minimum mass companion that produces a gravitationally-unstable disc after tidal disruption is $\sim0.15\,\mathrm{M}_\odot$. In this scenario, WD 1856+534 b might have formed at or close to its present separation, in contrast to other proposed scenarios where it would have migrated in from a much larger separation. Planet formation from tidal disruption is a new channel for producing second-generation planets around WDs. |
| title | Second-generation planet formation after tidal disruption from common envelope evolution |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2407.14190 |