Physical Properties of Be Stars in Open Clusters

1997 ◽  
Vol 109 ◽  
pp. 1396
Author(s):  
J. M. Torrejon
Keyword(s):  
Physical Properties ◽  
Open Clusters ◽  
Be Stars

scholarly journals Search for Pulsational Instability among h Persei Stars

1995 ◽  
Vol 155 ◽  
pp. 299-300
Author(s):  
J. Krzesinski
Keyword(s):  
Northern Hemisphere ◽  
Open Clusters ◽  
Age Group ◽  
Be Stars ◽  
Double Cluster

AbstractThe northern-hemisphere double cluster h and χ Persei is one of the richest young open clusters. At least half of the brightest stars in the cluster appear to be variables and most of them axe Be stars. Till now there was no evidence for the presence of β Cephei stars in the cluster. It is remarkable that the similar age southern cluster NGC 3293 and other clusters belonging to the same age group are documented as clusters in which β Cephei stars have been observed. In this work we report finding one suspected β Cephei-like object, basing on our own observations.

scholarly journals Abundances of Be Stars in Very Young Open Clusters

2000 ◽  
Vol 175 ◽  
pp. 59-62 ◽  
Author(s):  
A. Marco ◽  
G. Bernabeu ◽  
J.M. Torrejón ◽  
J.J. Rodes ◽  
J. Fabregat
Keyword(s):  
Open Clusters ◽  
Be Stars ◽  
Ccd Photometry ◽  
The Galaxy

AbstractWe present here standard uvbyβ CCD photometry for five open clusters of the Galaxy in order to determine abundances of Be stars, as a function of age.

scholarly journals Composite Colour-Magnitude and Colour-Colour Diagrams for Be Stars in Open Clusters

1982 ◽  
Vol 98 ◽  
pp. 23-26
Author(s):  
J.-C. Mermilliod
Keyword(s):  
Age Groups ◽  
Open Clusters ◽  
Be Stars ◽  
Photoelectric Photometry ◽  
Absolute Magnitudes ◽  
Colour Indices

By the end of 1980, the total number of Be stars discovered in the field of open clusters amounted to 180 stars distributed in 60 clusters. Among these, 110 Be stars belong to 32 clusters included in the sample I studied, which contains 75 open clusters younger than the Hyades. But only 88 stars with complete UBV photoelectric photometry have been taken into consideration here. The concept of age groups, defined elsewhere (Mermilliod 1981a), is used throughout the present analysis, as well as the new estimate of the colour excesses and distance moduli I obtained for these 32 clusters. Under the assumption of uniform reddening across the clusters, absolute magnitudes and dereddened colour indices have been calculated for the 88 Be stars.

scholarly journals K- and L-band spectroscopy of Be stars

2010 ◽  
Vol 6 (S272) ◽  
pp. 392-393
Author(s):  
Anahí Granada ◽  
María L. Arias ◽  
Lydia S. Cidale ◽  
Ronald E. Mennickent
Keyword(s):  
Physical Properties ◽  
Emission Lines ◽  
Circumstellar Disk ◽  
Be Stars ◽  
Circumstellar Envelopes ◽  
Hydrogen Emission ◽  
Group I ◽  
Hydrogen Emission Lines ◽  
L Band ◽  
Thick Medium

AbstractWe describe the behaviour of IR hydrogen emission lines of a sample of Be stars and discuss the physical properties of the circumstellar envelopes of Be stars classified in Groups I and II (Mennickent et al. 2009). We find that while Humphreys and Pfund lines of Group I stars form in an optically thick envelope/disk, Group II stars show Pfund lines that form in an optically thick medium and Humphreys lines originating in optically thinner regions. The transition between Groups I and II could be understood in terms of the evolution of the circumstellar disk of the star and might bring clues on the mechanism originating the Be phenomenon.

scholarly journals VARIABILITY OF Be STARS IN SOUTHERN OPEN CLUSTERS

2009 ◽  
Vol 700 (2) ◽  
pp. 1216-1232 ◽  
Author(s):  
M. Virginia McSwain ◽  
Wenjin Huang ◽  
Douglas R. Gies
Keyword(s):  
Open Clusters ◽  
Be Stars

scholarly journals Be stars in open clusters. I. uvby $ ^{\bf \beta}$ photometry

1996 ◽  
Vol 119 (2) ◽  
pp. 271-279 ◽  
Author(s):  
J. Fabregat ◽  
J. M. Torrejón ◽  
P. Reig ◽  
G. Bernabeu ◽  
J. Busquets ◽  
...  
Keyword(s):  
Open Clusters ◽  
Be Stars

scholarly journals Be stars in open clusters

1997 ◽  
Vol 124 (2) ◽  
pp. 329-347 ◽  
Author(s):  
J. M. Torrejón ◽  
J. Fabregat ◽  
G. Bernabeu ◽  
S. Alba
Keyword(s):  
Open Clusters ◽  
Be Stars

scholarly journals Be Star Surveys in Open Clusters with Balmer-line Photometry

2000 ◽  
Vol 175 ◽  
pp. 63-66
Author(s):  
Gemma Capilla ◽  
Juan Fabregat ◽  
Deborah Baines
Keyword(s):  
Emission Line ◽  
Main Sequence ◽  
Open Clusters ◽  
Balmer Line ◽  
Be Stars ◽  
Late Type ◽  
Efficient Tool ◽  
Be Star ◽  
Almost All ◽  
Evolutionary Interpretation

AbstractWe present CCD Hα and Hβ photometry of young open clusters. We show that the comparison of the α and β photometric indices provides an efficient tool for identifying emission line stars. We report on the discovery of several new Be stars.The preliminary results of our survey are the following: i. the younger clusters (age < 10 Myr) are almost lacking of Be stars, ii. clusters in the age interval 10–30 Myr are rich in Be stars. Almost all of them are of spectral types earlier than B5, while late-type Be stars are scarce. These results point towards an evolutionary interpretation of the Be phenomenon, in the sense that Be stars are close to the end of their main sequence lifetime.

Be stars in open clusters

1985 ◽  
Vol 59 ◽  
pp. 769 ◽  
Author(s):  
A. Slettebak
Keyword(s):  
Open Clusters ◽  
Be Stars
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