Photometric and Halpha observations of LSI+61·303: detection of a 26 day V and JHK band modulation

We present new optical and infrared photometric observations and high resolution H α spectra of the periodic radio star LSI+61◦303. The optical photometric data set covers the time interval 1985-1993 and amounts to about a hundred nights. A period of ∼26 days is found in the V band. The infrared dat...

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Detalles Bibliográficos
Autores: Paredes i Poy, Josep Maria, Marziani, P., Martí Ribas, Josep, Fabregat, Jaime, Coe, M. J., Everall, C., Figueras Siñol, Francesca, Jordi i Nebot, Carme, Norton, A. J., Prince, T., Reglero, V., Roche, P., Torra Roca, Jorge, Unger, S. J., Zamanov, R. K.
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:1994
País:España
Institución:Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya)
Repositorio:Recercat. Dipósit de la Recerca de Catalunya
OAI Identifier:oai:recercat.cat:2445/45406
Acceso en línea:https://hdl.handle.net/2445/45406
Access Level:acceso abierto
Palabra clave:Estels
Estels binaris de raigs X
Astronomia de raigs X
Astrofísica
Stars
X-ray binaries
X-ray astronomy
Astrophysics
Descripción
Sumario:We present new optical and infrared photometric observations and high resolution H α spectra of the periodic radio star LSI+61◦303. The optical photometric data set covers the time interval 1985-1993 and amounts to about a hundred nights. A period of ∼26 days is found in the V band. The infrared data also present evidence for a similar periodicity, but with higher amplitude of variation ((0.m 2). The spectroscopic observations include 16 intermediate and high dispersion spectra of LSI+61◦303 collected between January 1989 and February 1993. The H α emission line profile and its variations are analyzed. Several emission line parameters -- among them the H α EW and the width of the H α red hump -- change strongly at or close to radio maximum, and may exhibit periodic variability. We also observe a significant change in the peak separation. The H α profile of LSI+61◦303 does not seem peculiar for a Be star. However, several of the observed variations of the H α profile can probably be associated with the presence of the compact, secondary star.

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