6533b834fe1ef96bd129cdac
RESEARCH PRODUCT
Spectroscopic Observations of the Delta Scorpii Binary during Its Recent Periastron Passage
A. S. MiroshnichenkoJ. FabregatK. S. BjorkmanD. C. KnauthN. D. MorrisonA. E. TarasovPablo ReigI. NegueruelaP. Blaysubject
Bright starAstrophysics::High Energy Astrophysical PhenomenaBinary numberFOS: Physical sciencesOrbital eccentricityAstrophysicsAstrophysicsUNESCO::ASTRONOMÍA Y ASTROFÍSICA01 natural sciencesSpectral lineSpectroscopic Technich0103 physical sciencesAstrophysics::Solar and Stellar AstrophysicsBinary systemSpectroscopy010303 astronomy & astrophysicsAstrophysics::Galaxy AstrophysicsLine (formation)Physics010308 nuclear & particles physicsBinariesAstrophysics (astro-ph)Astronomy and Astrophysics:ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogonia [UNESCO]Emission-line ; Binaries ; Sco ; Spectroscopic TechnichOrbitScoSpace and Planetary ScienceAstrophysics::Earth and Planetary AstrophysicsUNESCO::ASTRONOMÍA Y ASTROFÍSICA::Cosmología y cosmogoniaEmission-line:ASTRONOMÍA Y ASTROFÍSICA [UNESCO]description
The bright star delta Sco has been considered a typical B0-type object for many years. Spectra of the star published prior to 1990 showed no evidence of emission, but only of short-term line profile variations attributed to nonradial pulsations. Speckle interferometric observations show that delta Sco is a binary system with a highly-eccentric orbit and a period of 10.6 years. Weak emission in the H-alpha line was detected in its spectrum for the first time during a periastron passage in 1990. Shortly before the next periastron passage in the summer of 2000, the binary entered a strong H-alpha emission and enhanced mass loss phase. We monitored the spectroscopic development of the Be outburst from July 2000 through March 2001. In this paper we present results from our spectroscopy, refine elements of the binary orbit, and discuss possible mechanisms for the mass loss.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2001-06-27 |