K- and L- band spectroscopy of Be stars

dc.creator	Granada, Anahí
dc.creator	Arias, María Laura
dc.creator	Cidale, Lydia Sonia
dc.creator	Mennickent, Ronald E.
dc.date	2011-07-12
dc.date	2019-10-25T13:47:35Z
dc.identifier	http://sedici.unlp.edu.ar/handle/10915/84051
dc.identifier	issn:1743-9213
dc.description	We 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.
dc.description	Facultad de Ciencias Astronómicas y Geofísicas
dc.description	Instituto de Astrofísica de La Plata
dc.format	application/pdf
dc.format	392-393
dc.language	en
dc.rights	http://creativecommons.org/licenses/by-nc-sa/4.0/
dc.rights	Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.subject	Ciencias Astronómicas
dc.subject	Ciencias Exactas
dc.subject	Be stars
dc.subject	Circumstellar matter
dc.subject	Stars: emission-line
dc.title	K- and L- band spectroscopy of Be stars
dc.type	Articulo
dc.type	Comunicacion