Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1908t&link_type=abstract
American Astronomical Society, HEAD meeting #11, #19.08; Bulletin of the American Astronomical Society, Vol. 41, p.690
Astronomy and Astrophysics
Astronomy
Scientific paper
Classical novae are a class of cataclysmic variables. Sudden outbursts occur by nuclear fusion of hydrogen on the white dwarf surface. X-rays can be emitted at various stages in the post-burst evolution via different mechanisms. Hard X-rays are often seen from an early phase, originating presumably from shocks in the expanding ejecta. In contrast, soft X-rays emerge in a later phase when the hot photospheric emission of the white dwarf is revealed by a thinning envelope. When the secondary star is a giant, the released energy and mass can propagate through significant circumstellar material that can form an X-ray emitting shock structure similar to those of supernova remnants but on much smaller scales both in time and space.
We have performed ToO observations of recent classical novae with the Suzaku satellite. For the classical nova V458 Vul, the observation yielded a well-exposed X-ray spectrum 88 days after the outburst, and we could identify emission lines from highly ionized neon, magnesium, and silicon on a hard X-ray continuum (Tsujimoto et al. 2008, PASJ).
For V2491 Cyg, we obtained the first detection of non-thermal X-rays from a classical nova explosion (Takei et al. 2009, ApJL). The power-law emission, extending up to 70 keV with a very flat slope (photon index of 0.1), poses a challenge for understanding the emission mechanism as well as the acceleration mechanism of electrons in the explosion. For V2672 Oph, a timely pointed observation captured the rise phase of a remarkable soft X-ray flare. The flare spectral evolution during the rise was characterised by an increase only in the soft 0.5-1.5 keV band (Takei et al. in prep.). We present the results of these X-ray spectroscopic observations, and discuss their implications for understanding the nature of nova explosions.
Drake Jeremy J.
Kitamoto Shunji
Ness Jan-Use
Takei Dai
Tsujimoto Masahiro
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