{gamma} Cas radial velocity curve Virtual Observatory Resource

Authors

1. Smith M.A.
2. Lopes de Oliveira R.
3. Motch C.
4. Henry G.W.
5. Richardson N.D.,Bjorkman K.S.
6. Stee P.
7. Mourard D.
8. Monnier J.D.
9. Che X.
10. Buecke R.,Pollmann E.
11. Gies D.R.
12. Schaefer G.H.
13. ten Brummelaar T.
14. McAlister H.A.,Turner N.H.
15. Sturmann J.
16. Sturmann L.
17. Ridgway S.T.

Published by

CDS

Abstract

{gamma} Cas is the prototypical classical Be star and is recently best known for its variable hard X-ray emission. To elucidate the reasons for this emission, we mounted a multiwavelength campaign in 2010 centered around four XMM-Newton observations. The observational techniques included long baseline optical interferometry (LBOI) from two instruments at CHARA, photometry carried out by an automated photometric telescope and H{alpha} observations. Because {gamma} Cas is also known to be in a binary, we measured radial velocities from the H{alpha} line and redetermined its period as 203.55+/-0.20 days and its eccentricity as near zero.

Keywords

1. be-stars
2. emission-line-stars
3. radial-velocity

Bibliographic source Bibcode

2012A&A...540A..53S

See also HTML

https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/540/A53

IVOA Identifier IVOID

ivo://CDS.VizieR/J/A+A/540/A53

Document Object Identifer DOI

doi:10.26093/cds/vizier.35400053

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