Variability of the post-AGB star HR 4049 - Dust obscuration in a binary system

Details Variability of the post-AGB star HR 4049 - Dust obscuration in a binary system Variability of the post-AGB star HR 4049 - Dust obscuration in a binary system

Feb 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...242..433w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 242, no. 2, Feb. 1991, p. 433-442.

Astronomy and Astrophysics

Astrophysics

52

Asymptotic Giant Branch Stars, Binary Stars, Peculiar Stars, Radial Velocity, Stellar Envelopes, Variable Stars, Color-Magnitude Diagram, Interstellar Extinction, Iue, Main Sequence Stars, Stellar Evolution, Stellar Spectrophotometry

Scientific paper

Results obtained from a large number of coordinated photometric and spectroscopic observations lead to the conclusion that HR 4049 is a binary with an orbital period near 434 days and a companion of similar mass which either is a white dwarf or a main-sequence star, more likely the second. The H-alpha line is in emission with either a P Cygni profile or a shell profile. The data suggest a smooth transition from P Cygni to shell and back, correlated with the photometric and radial-velocity variations. The mass flow from HR 4049 is thus altered by the presence of a companion. The photometric variability is best explained by variable extinction of the star by circumstellar matter surrounding the system. The infrared variability can only be explained if the extinction variations reflect a change in the characteristics of dust rather than purely geometric changes.

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