Does G29-38 have a massive companion

Journal Article · Sun Jul 01 04:00:00 EDT 1990 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/185757· OSTI ID:6863931

Graham, J R; Reid, I N; Mccarthy, J K; Rich, R M ^[1]

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1. Palomar Observatory, Pasadena, CA (USA) Texas Univ., Austin (USA) Columbia Univ., NY (USA)

Radial velocity measurements of G29-38 during the period of 182 days are used to show that the phase modulation of the optical pulsations is not due to orbital motion about a massive companion. Limits on the presence of a close brown dwarf companion are not stringent, but there is evidence for a linear trend in the radial velocity which may be part of a periodic variation with an amplitude greater or equal to 5 km/s and period greater or equal to 360 days. 18 refs.

• OSTI ID: 6863931
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 357; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
CHARGE-COUPLED DEVICES
DWARF STARS
LIMITING VALUES
MASS
OSCILLATIONS
PULSATIONS
RADIAL VELOCITY
SEMICONDUCTOR DEVICES
SPECTROPHOTOMETRY
STARS
VARIATIONS
VELOCITY
WHITE DWARF STARS