Computer Science
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008cxo..prop.2971k&link_type=abstract
Chandra proposal ID #10208330
Computer Science
Scientific paper
The nature of the infamous 2002 outburst of V838 Mon (Bond 2007; Tylenda et al. 2009 [T09]) remains uncertain. No nova-like "hot phase" was observed and the presence of a B3V companion and a small cluster implies the system is too young to harbor an accreting white dwarf. Among the leading models for the outburst is that of a stellar merger (Soker & Tylenda 2007 [ST07]). The merger product should become magnetically active well after outburst (ST07), suggesting that V838 Mon should make a delayed appearance as an X-ray source. Indeed, V838 Mon went undetected by CXO in 2003 (Orio et al 2003), but when we reobserved the object in 2008 with XMM we detected a luminous X-ray source very near its position (Antonini et al 2009). This source may be the spun-up merger remnant. However, V838Mon s ejecta had just engulfed its companion at the time of our XMM observation (T09). Hence the XMM source might be due instead to interactions between V838 Mon s ejecta and its companion.
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