Published February 11, 2003
| Published + Submitted
Journal Article
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A variational formalism for tidal excitation: non-rotating, homentropic stars
Abstract
We present a variational formalism for describing the dynamical evolution of an oscillating star with a point-mass companion in the linear, non-relativistic regime. This includes both the excitation of normal modes and the back-reaction of the modes on the orbit. The general formalism for arbitrary fluid configurations is presented, and then specialized to a homentropic potential flow. Our formalism explicitly identifies and conserves both energy and angular momentum. We also consider corrections to the orbit up to 7/2 post-Newtonian order.
Additional Information
© 2003 RAS. Accepted 2002 October 4. Received 2002 October 2; in original form 2002 August 12. We would like to thank Alessandra Buonanno, Donald Lynden-Bell and Kaloyan Penev for several useful discussions. RB thanks J. Ostriker for stimulating his interest in the fate of white dwarfs captured on to compact objects. Special thanks go to the referee for improving the readability of this paper. We acknowledge support under NASA grant NAGWS-2837.Attached Files
Published - Rathore_et_al-2003-Monthly_Notices_of_the_Royal_Astronomical_Society.pdf
Submitted - 0209003.pdf
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Rathore_et_al-2003-Monthly_Notices_of_the_Royal_Astronomical_Society.pdf
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Additional details
- Eprint ID
- 85961
- Resolver ID
- CaltechAUTHORS:20180418-162756319
- NAGWS-2837
- NASA
- Created
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2018-04-19Created from EPrint's datestamp field
- Updated
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2021-11-15Created from EPrint's last_modified field
- Caltech groups
- TAPIR