Volume 545, September 2012
|Number of page(s)||4|
|Section||Stellar structure and evolution|
|Published online||18 September 2012|
Astronomical Institute, Academy of Sciences of the Czech
2 Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, 611 37 Brno, Czech Republic
Received: 25 May 2012
Accepted: 10 August 2012
The spectrum of the Be star o Pup is shown to vary periodically with a period of 28.9 days. A radial-velocity variable He i 6678 Å emission component suggests that the star is the same type as φ Per, 59 Cyg, and FY CMa, i.e. binaries consisting of a Be star and a hot companion that illuminates the Be star disk (also called φ Per-type binaries or Be+sdO binaries). The range of radial-velocity variations of the stronger emission component in the helium line observed in o Pup is about 270 km s-1, a value in good agreement with the range derived for φ Per-type binaries. The radial velocity curves defined by the prominent emission peak in He i 6678 Å line and Hα + Paschen emission move in anti-phase. We suggest that o Pup is generically similar to φ Per-type systems and may represent the fourth case of a Be star with a hot subdwarf companion.
Key words: binaries: spectroscopic / stars: emission-line, Be / stars: individual:o Puppis / binaries: close
The Ondrejov spectra are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/545/A121
© ESO, 2012
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.