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Home All issues Volume 495 / No 1 (February III 2009) A&A, 495 1 (2009) 217-229 Full HTML
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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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