XMM-Newton observations of β Centauri (B1 III): The temperature structure in the hot plasma and the photosphere-wind connection

Details XMM-Newton observations of β Centauri (B1 III): The temperature structure in the hot plasma and the photosphere-wind connection XMM-Newton observations of β Centauri (B1 III): The temperature structure in the hot plasma and the photosphere-wind connection

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...437..599r&link_type=abstract

Astronomy and Astrophysics, Volume 437, Issue 2, July II 2005, pp.599-609

Astronomy and Astrophysics

Astrophysics

6

Stars: Early-Type, Stars: Winds, Outflows, Stars: Variables: Β Cephei

Scientific paper

We present XMM-Newton observations of the B giant β Centauri (B1 III). The spectra are rich of spectral lines from a wide range of ionization stages which indicate temperatures in the range ~0.1-0.6 keV. Simultaneous fits to the rgs, epic-mos, and epic-pn spectra yield three plasma temperatures (0.1, 0.2, and 0.6 keV), emission measures, and elemental abundances which are quite close to solar values. These temperatures are confirmed by DEM modeling. According to the derived models the intrinsic source X-ray luminosity in the energy range 0.3-10 keV is Lx = 10 × 1030 erg s-1 at a distance of 161 pc. An analysis of the X-ray light curve suggests that the photospheric variability does not have much of an effect on the properties of the X-ray luminosity. The sensitivity of the He-like forbidden and intercombination lines to a strong ultraviolet stellar radiation field is used to constrain the radial distances at which the lines of Ne ix, O vii, and N vi originate.

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