Evolution of the symbiotic binary system AG Dranconis

Details Evolution of the symbiotic binary system AG Dranconis Evolution of the symbiotic binary system AG Dranconis

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109.1289m&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 109, no. 3, p. 1289-1307

Astronomy and Astrophysics

Astronomy

58

Stellar Activity, Stellar Envelopes, Stellar Evolution, Stellar Luminosity, Stellar Winds, Symbiotic Stars, Ultraviolet Spectra, Visible Spectrum, Line Spectra, Mass Ratios, Radial Velocity, Radiant Flux Density, Spectrum Analysis, Stellar Orbits, Stellar Spectrophotometry

Scientific paper

We present an analysis of new and archival photometric and spectroscopic observations of the symbiotic star AG Draconis. This binary has undergone several 1 - 3 mag optical and ultraviolet eruptions during the past 15 years. Our combination of optical and ultraviolet spectroscopic data allow a more complete analysis of this system than in previous papers. AG Dra is composed of a K-type bright giant Mg approximately 1.5 solar mass) and a hot, compact star Mh approximatelly 0.4 - 0.6 solar mass embedded in a dense, low metallicity nebula. The hot component undergoes occasional thermonuclear runaways that produce 2 - 3 mag optical/ultraviolet eruptions. During these eruptions, the hot component develops a low velocity wind that quenches x-ray emission from the underlying hot white dwarf. The photoionized nebula changes its volume by a factor of 5 throughout an eruptin cycle. The K bright giant occults low ionization emission lines during superior conjunctions at all outburst phases but does not occult high ionization lines in outburst (and perhaps quiescence). This geometry and the component masses suggest a system inclination of i approximately 30 deg - 45 deg.

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