The great escape: how exoplanets and smaller bodies desert dying stars
Veras, Dimitri ; Wyatt, Mark C ; Mustill, Alexander LU
; Bonsor, Amy
and Eldridge, John J
(2011)
In Monthly Notices of the Royal Astronomical Society
417(3).
p.2104-2123
- Abstract
- Mounting discoveries of extrasolar planets orbiting post-main-sequence stars motivate studies to understand the fate of these planets. In the traditional 'adiabatic' approximation, a secondary's eccentricity remains constant during stellar mass-loss. Here, we remove this approximation, investigate the full two-body point-mass problem with isotropic mass-loss, and illustrate the resulting dynamical evolution. The magnitude and duration of a star's mass-loss combined with a secondary's initial orbital characteristics might provoke ejection, modest eccentricity pumping, or even circularization of the orbit. We conclude that Oort Clouds and wide-separation planets may be dynamically ejected from 1-7 M☉ parent stars during AGB evolution. The... (More)
- Mounting discoveries of extrasolar planets orbiting post-main-sequence stars motivate studies to understand the fate of these planets. In the traditional 'adiabatic' approximation, a secondary's eccentricity remains constant during stellar mass-loss. Here, we remove this approximation, investigate the full two-body point-mass problem with isotropic mass-loss, and illustrate the resulting dynamical evolution. The magnitude and duration of a star's mass-loss combined with a secondary's initial orbital characteristics might provoke ejection, modest eccentricity pumping, or even circularization of the orbit. We conclude that Oort Clouds and wide-separation planets may be dynamically ejected from 1-7 M☉ parent stars during AGB evolution. The vast majority of planetary material that survives a supernova from a 7-20 M☉ progenitor will be dynamically ejected from the system, placing limits on the existence of first-generation pulsar planets. Planets around >20 M☉ black hole progenitors may easily survive or readily be ejected depending on the core collapse and superwind models applied. Material ejected during stellar evolution might contribute significantly to the free-floating planetary population. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/4500277
- author
- Veras, Dimitri
; Wyatt, Mark C
; Mustill, Alexander
LU
; Bonsor, Amy
and Eldridge, John J
- publishing date
- 2011
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Oort Cloud, Physics - Classical Physics, planet-star interactions, planets and satellites: dynamical evolution and stability, stars: AGB and post-AGB, stars: evolution, supernovae: general
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 417
- issue
- 3
- pages
- 2104 - 2123
- publisher
- Oxford University Press
- external identifiers
-
- scopus:80055102444
- ISSN
- 1365-2966
- DOI
- 10.1111/j.1365-2966.2011.19393.x
- language
- English
- LU publication?
- no
- id
- 3ed11226-12e7-47ab-bc5d-11592ef097ba (old id 4500277)
- date added to LUP
- 2016-04-04 10:42:54
- date last changed
- 2025-10-14 09:49:36
@article{3ed11226-12e7-47ab-bc5d-11592ef097ba,
abstract = {{Mounting discoveries of extrasolar planets orbiting post-main-sequence stars motivate studies to understand the fate of these planets. In the traditional 'adiabatic' approximation, a secondary's eccentricity remains constant during stellar mass-loss. Here, we remove this approximation, investigate the full two-body point-mass problem with isotropic mass-loss, and illustrate the resulting dynamical evolution. The magnitude and duration of a star's mass-loss combined with a secondary's initial orbital characteristics might provoke ejection, modest eccentricity pumping, or even circularization of the orbit. We conclude that Oort Clouds and wide-separation planets may be dynamically ejected from 1-7 M☉ parent stars during AGB evolution. The vast majority of planetary material that survives a supernova from a 7-20 M☉ progenitor will be dynamically ejected from the system, placing limits on the existence of first-generation pulsar planets. Planets around >20 M☉ black hole progenitors may easily survive or readily be ejected depending on the core collapse and superwind models applied. Material ejected during stellar evolution might contribute significantly to the free-floating planetary population.}},
author = {{Veras, Dimitri and Wyatt, Mark C and Mustill, Alexander and Bonsor, Amy and Eldridge, John J}},
issn = {{1365-2966}},
keywords = {{Astrophysics - Earth and Planetary Astrophysics; Astrophysics - Solar and Stellar Astrophysics; Oort Cloud; Physics - Classical Physics; planet-star interactions; planets and satellites: dynamical evolution and stability; stars: AGB and post-AGB; stars: evolution; supernovae: general}},
language = {{eng}},
number = {{3}},
pages = {{2104--2123}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{The great escape: how exoplanets and smaller bodies desert dying stars}},
url = {{http://dx.doi.org/10.1111/j.1365-2966.2011.19393.x}},
doi = {{10.1111/j.1365-2966.2011.19393.x}},
volume = {{417}},
year = {{2011}},
}