Spectroscopic survey of emission line stars in open clusters

Subramaniam, A; Mathew, B

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dc.contributor.author	Subramaniam, A
dc.contributor.author	Mathew, B
dc.date.accessioned	2010-09-09T16:26:40Z
dc.date.available	2010-09-09T16:26:40Z
dc.date.issued	2010
dc.identifier.citation	Chaudhuri, R. K., Mekkaden, M. V., Raveendran, A. V & Narayanan, A. S., eds., Recent Advances In Spectroscopy: Theoretical, Astrophysical And Experimental Perspectives, Proceedings of the International Conference on Recent Advances in Spectroscopy - Theoretical, Astrophysical and Experimental Perspectives, Jan 28-31, 2009, Indian Institute of Astrophysics, Kodaikanal Observatory, Bangalore, India, pp. 217-222	en
dc.identifier.uri	http://hdl.handle.net/2248/5245
dc.description	Restricted Access	en
dc.description	The original publication is available at springerlink.com
dc.description.abstract	We summarize a study of emission-line stars in young open clusters. The study was done in two phases. The first phase was the survey, where the emission stars in young open clusters were identified using the slitless spectral images. The identified emission stars were then studied in detail using their slit spectra in the 3700–9000 °A range. The results of the study suggest that there could be two mechanisms responsible for the Be phenomenon. The early type B stars are likely to become Be stars in the second half of their MS lifetime, whereas the late type B stars are likely to be born as Be stars.	en
dc.language.iso	en	en
dc.publisher	Springer	en
dc.relation.ispartofseries	Astrophysics and Space Science Proceedings
dc.relation.uri	http://www.springerlink.com/content/v347tq538455l59p/	en
dc.rights	© Springer	en
dc.title	Spectroscopic survey of emission line stars in open clusters	en
dc.type	Article	en