Testing magnetically confined wind shock models for β Cephei using XMM-Newton and Chandra phase-resolved X-ray observations

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Table 3:

The joint best-fit spectral parameter for the 2-T fit with individually varying metal abundances for the 4 pn spectra. The notation `` $M/M_\odot$ '' indicates the ratio between the $\beta$ Cep coronal abundance and the solar photospheric abundance. The notation `` $M/M_{\rm phot}$ '' indicates the ratio between the coronal abundance of $\beta$ Cep determined here and the photospheric abundance of $\beta$ Cep determined by Morel et al. (2006). In all cases, the solar photospheric abundances of Grevesse & Sauval (1998) were used. The indicated uncertainties are 90% errors derived from a $\Delta \chi ^2$ analysis. For all heavy elements not explicitly indicated, the abundances are equal to the value for Fe.
$N({\rm H})$	$2.50 \pm 0.01 \times 10^{20}$ cm^-2
T₁	$0.24\pm0.01$ keV
T₂	$0.63\pm0.03$ keV
$E\!M_1$	$1.1\pm0.2$ 10⁵⁴ cm^-3
$E\!M_2$	$1.3\pm0.3$ 10⁵³ cm^-3
O/O $_\odot$	$0.12\pm0.02$
Ne/Ne $_\odot$	$0.18\pm0.03$
Si/Si $_\odot$	$0.31\pm0.06$
Fe/Fe $_\odot$	$0.33\pm0.04$
O/O $_{\rm phot}$	0.28
Si/Si $_{\rm phot}$	0.86
Fe/Fe $_{\rm phot}$	0.60

Source LaTeX | All tables | In the text

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