H$\alpha$ long term monitoring of the Be star $\beta$ Cep Aa
| Autor: | Catanzaro, G. |
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| Rok vydání: | 2008 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1111/j.1365-2966.2008.13263.x |
| Popis: | Recent papers published in the last years contributed to resolve the enigma on the hypothetical Be nature of the hot pulsating star $\beta$ Cep. This star shows variable emission in the H$\alpha$ line, typical for Be stars, but its projected rotational velocity is very much lower than the critical limit, contrary to what is expected for a typical Be star. The emission has been attributed to the secondary component of the $\beta$ Cep spectroscopic binary system. In this paper, using both ours and archived spectra, we attempted to recover the H$\alpha$ profile of the secondary component and to analyze its behavior with time for a long period. To accomplish this task, we first derived the atmospheric parameters of the primary: T$_{\rm eff}$ = 24000 $\pm$ 250 K and $\log g$ = 3.91 $\pm$ 0.10, then we used these values to compute its synthetic H$\alpha$ profile and finally we reconstructed the secondary's profile disentangling the observed one. The secondary's H$\alpha$ profile shows the typical two peaks emission of a Be star with a strong variability. We analyzed also the behavior versus time of some line width parameters: equivalent width, V/R, FWHM, peaks separation and radial velocity of the central depression. Projected rotational velocity ($v \sin i$) of the secondary and the dimension of the equatorial surrounding disk have been estimated, too. Comment: 9 pages, 6 figures, 2 tables, accepted for publication in MNRAS |
| Databáze: | arXiv |
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