M. Orio, E. Behar, J. Gallagher, A. Bianchini, E. Chiosi, G. J. M. Luna
We present a {\sl Chandra} observation of the recurrent nova U Scorpii, done with the HRC-S detector and the LETG grating on day 18 after the observed visual maximum of 2010, and compare it with {\sl XMM-Newton} observations obtained in days 23 and 35 after maximum. The total absorbed flux was in the range 2.2-2.6 $\times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$, corresponding to unabsorbed luminosity 7-8.5 $\times$ 10$^{36} \times$(d/12 kpc)$^2$ for N(H)=2-2.7 $\times$ 10$^{21}$ cm$^{-2}$. On day 18, 70% of the soft X-tray flux was in a continuum typical of a very hot white dwarf (WD) atmosphere, which accounted for about 80% of the flux on days 23 and 35. In addition all spectra display very broad emission lines, due to higher ionization stages at later times. With {\sl Chandra} we observed apparent P Cygni profiles. We find that these peculiar profiles are not due to blue shifted absorption and red shifted emission in photoionized ejecta, like the optical P Cyg of novae, but they are rather a superposition of WD atmospheric absorption features reflected by the already discovered Thomson scattering corona, and emission lines due to collisional ionization in condensations in the ejecta. On days 23 and 35 the absorption components were no longer measurable, having lost the initial large blue shift that displaced them from the core of the broad emission lines. We interpret this as indication that mass loss ceased between day 18 and day 23. On day 35, the emission lines spectrum became very complex, with several different components. Model atmospheres indicate that the WD atmospheric temperature was about 730,000 K on day 18 and reached 900,000 K--one million K on day 35. This peak temperature is consistent with a WD mass of at least 1.3 M$_\odot$.
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http://arxiv.org/abs/1212.5026
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