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Orbital angular momentum loss in PSR 1957 + 20It is suggested that the companion winds, excited by the radiation from the neutron star in PSR 1957 + 20 form only through the combined action of the radiation heat on the companion's atmosphere and the radiation force on the slowly lifting wind. Ballistic simulations suggest that these winds leave only from selected areas of the illuminated surface of the companion; surface currents channel into these regions relatively hot (but altogether cooler than the companion escape velocity) 'coronal' matter from the whole illuminated area. Under suitable conditions, wind particles spend some time trailing the companion at close distances before taking off to escape from the system. This can torque the binary into angular momentum loss that will be as efficient as the one recently observed in PSR 1957 + 20 if the companion is bloated to dimensions close to that of the Roche lobe.
Document ID
19920046178
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Banit, Menashe
(NASA Headquarters Washington, DC United States)
Shaham, Jacob
(Columbia University New York, United States)
Date Acquired
August 15, 2013
Publication Date
March 20, 1992
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters
Volume: 388
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
92A28802
Funding Number(s)
CONTRACT_GRANT: NAGW-1618
CONTRACT_GRANT: NCC5-37
CONTRACT_GRANT: NSF PHY-89-04035
Distribution Limits
Public
Copyright
Other

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