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TT Crateris - A long-period, double-lined dwarf novaTime-resolved CCD photometry and spectroscopy of the dwarf nova TT Crt during quiescence are presented. The spectra reveal Balmer emission as well as absorption features of a K5-M0 secondary. The B, V, R light curves are dominated by a periodic variation of full amplitude 0.35 mag in V, which are interpreted as the ellipsoidal variation of the secondary star. The remarkably large amplitude indicates a high inclination (50-65 deg) and a massive white dwarf M greater than 0.8 solar mass. The ratio of the radial velocity semiamplitudes of the primary to the secondary is 0.5-1.4. The best period that can be determined from the observations is 438.17 minutes, with a possible alias at 445 minutes.
Document ID
19920044559
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Szkody, Paula
(Washington, University Seattle, United States)
Williams, Robert E.
(Cerro Tololo Inter-American Observatory La Serena, Chile)
Margon, Bruce
(Washington, University Seattle, United States)
Howell, Steve B.
(Planetary Science Institute Tucson, AZ, United States)
Mateo, Mario
(Carnegie Institution of Washington, Observatories, Pasadena CA, United States)
Date Acquired
August 15, 2013
Publication Date
March 1, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 387
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
92A27183
Funding Number(s)
CONTRACT_GRANT: NSF AST-89-15445
CONTRACT_GRANT: NAS5-29293
CONTRACT_GRANT: NSF AST-89-14866
CONTRACT_GRANT: NAS5-26555
Distribution Limits
Public
Copyright
Other

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