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| Paper: |
Planets Surviving Stellar Evolution |
| Volume: |
398, Extreme Solar Systems |
| Page: |
167 |
| Authors: |
Villaver, E.; Livio, M. |
| Abstract: |
Over the last few years several groups have surveyed white dwarfs in the search for planets. The underlying assumption has been that planets can survive the parent star’s evolution if they manage to stay in a large enough orbit to avoid engulfment by the star, when the latter increases it’s radius as it ascends the Red Giant Branch and Asymptotic Giant Branch (AGB). We have explored this hypothesis by determining: (1) the planet’s survival during the AGB phase and the orbital changes due to the AGB mass-loss using the range of initial masses for white dwarfs progenitors, and (2) the range of parameters under which an outflow from the gas planet caused by irradiation by the planetary nebulae central star leads to the total destruction of the planet. We show that planets with masses less than one Jupiter mass do not survive the planetary nebula phase if located initially at orbital distances smaller than 3-5AU. Planets more massive than two Jupiter masses around low-mass stars (1M⊙ on the Main Sequence) survive the planetary nebulae stage down to orbital distances of ∼3 AU. Planets around white dwarfs with masses of MWD > 0.7M⊙ are generally expected to be found at orbital radii r> 15AU. |
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