Sign on
ADS Classic is now deprecated. It will be completely retired in October 2019. This page will automatically redirect to the new ADS interface at that point.

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (160) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
· Translate This Page
Evolution of close neutron star binaries
Clark, J. P. A.; Eardley, D. M.
AA(Yale University Observatory, New Haven, Conn.), AB(Yale University, New Haven, Conn.)
Astrophysical Journal, Part 1, vol. 215, July 1, 1977, p. 311-322. Research supported by the Dominion Astrophysical Laboratory (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Binary Stars, Gravitational Waves, Neutron Stars, Orbit Decay, Energy Dissipation, Neutrinos, Roche Limit, Stellar Evolution, Stellar Models
Bibliographic Code:


In binary systems consisting of two neutron stars, the orbit decays by gravitational radiation. A crude model shows that the less massive star may suffer either immediate tidal disruption or slow mass stripping when it reaches its Roche radius, depending on the initial masses and on the details of mass exchange or mass loss. Typical energy releases are 4 x 10 to the 52 ergs in gravitational waves before the onset of stripping, 2 x 10 to the 52 ergs in gravitational waves after the onset of stripping, 2 x 10 to the 53 ergs in neutrinos after the onset of stripping. The stripping process always ends in tidal disruption of the less massive star after a few seconds or a few hundred revolutions. As the endpoint of binary stellar evolution, such events are estimated to occur only about every 100 yr out to a radius of 15 Mpc, and are thus less important than supernovae as sources of gravitational waves; the observed wave amplitude would be about 10 to the -21. Such events may occur in Type II supernovae, if the collapsing stellar core rotates rapidly enough to fission into two neutron stars.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences

More Article Retrieval Options

HELP for Article Retrieval

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints