dc.contributor.author |
Mathew, B |
|
dc.contributor.author |
Subramaniam, A |
|
dc.date.accessioned |
2011-03-17T15:11:41Z |
|
dc.date.available |
2011-03-17T15:11:41Z |
|
dc.date.issued |
2010 |
|
dc.identifier.citation |
Ojha, D. K., ed., Interstellar matter and star formation: a multi-wavelength Perspective, An international workshop held as part of the Homi Bhabha Birth Centenary Celebrations, Hyderabad, India Oct 5-7, 2009, pp. 85-89 |
en |
dc.identifier.issn |
978-81-8465-441-7 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/5425 |
|
dc.description |
Restricted Access |
en |
dc.description.abstract |
A spectroscopic study of 152 Classical Be stars in 42
young open clusters was performed using medium resolution spectra
in 3700-9000 A range, to understand the Be phenomenon. The
Balmer decrement is found to have a bimodal distribution which is
correlated with the nature of H,a profile. Classical Be stars with
higher Balmer decrement (76%) were found to have more number of
emission lines, higher H", equivalent width and (H - K)o values, suggesting
an optically and geometrically thick disk. Massive Be stars
of spectral type BO-B4 are found to have enhanced H", emission at
the end of their main sequence lifetime, as inferred from the enhancements
observed at 12.5 and 25 Myr. These results support our earlier
prediction that early B-type stars (BO-B4) spin up to Be phase while
others (B4-AO) are born as Be stars. |
en |
dc.language.iso |
en |
en |
dc.publisher |
Astronomical Society of India |
en |
dc.relation.ispartofseries |
ASI Conference Series, Vol. 1 |
|
dc.rights |
© Astronomical Society of India |
en |
dc.subject |
Stars: formation |
en |
dc.subject |
stars: emission-line |
en |
dc.subject |
Be - stars |
en |
dc.subject |
Open clusters |
en |
dc.title |
Spectroscopy of Be stars in young open clusters |
en |
dc.type |
Article |
en |