M. F. Bode et al. 2006 ApJ 652 629 doi:10.1086/507980
M. F. Bode1, T. J. O'Brien2, J. P. Osborne3, K. L. Page3, F. Senziani4,5,6, G. K. Skinner5,7, S. Starrfield8, J.-U. Ness8, J. J. Drake9, G. Schwarz10, A. P. Beardmore3, M. J. Darnley1, S. P. S. Eyres11, A. Evans12, N. Gehrels13, M. R. Goad3, P. Jean5,7, J. Krautter14 and G. Novara4,6
Show affiliationsRS Ophiuchi began its latest outburst on 2006 February 12. Previous outbursts have indicated that high-velocity ejecta interact with a preexisting red giant wind, setting up shock systems analogous to those seen in supernova remnants. However, in the previous outburst in 1985, X-ray observations did not commence until 55 days after the initial explosion. Here we report on Swift observations covering the first month of the 2006 outburst with the Burst Alert Telescope (BAT) and X-Ray Telescope (XRT) instruments. RS Oph was clearly detected in the BAT 14-25 keV band from t = 0 to t ~ 6 days. XRT observations from 0.3 to 10 keV started 3.17 days after outburst. The rapidly evolving XRT spectra clearly show the presence of both line and continuum emission, which can be fitted by thermal emission from hot gas whose characteristic temperature, overlying absorbing column (NH)W, and resulting unabsorbed total flux decline monotonically after the first few days. Derived shock velocities are in good agreement with those found from observations at other wavelengths. Similarly, (NH)W is in accord with that expected from the red giant wind ahead of the forward shock. We confirm the basic models of the 1985 outburst and conclude that standard phase I remnant evolution terminated by t ~ 6 days and the remnant then rapidly evolved to display behavior characteristic of phase III. Around t = 26 days, however, a new, luminous, and highly variable soft X-ray source began to appear, whose origin will be explored in a subsequent paper.
binaries: close; binaries: symbiotic; novae, cataclysmic variables; stars: individual (RS Ophiuchi); supernovae: general; white dwarfs
Issue 1 (2006 November 20)
Received 2006 April 20, accepted for publication 2006 July 13
M. F. Bode et al. 2006 ApJ 652 629
J D Mullett et al 2007 J. Phys. D: Appl. Phys. 40 4730
V Talasila et al 2004 J. Phys. A: Math. Gen. 37 9705
Martin P McHugh et al 2005 Class. Quantum Grav. 22 S965
Vijay Balasubramanian et al 2002 Class. Quantum Grav. 19 5655
Christophe Texier and Gilles Montambaux 2005 J. Phys. A: Math. Gen. 38 3455
Salomon S Mizrahi and Diógenes Galetti 2002 J. Phys. A: Math. Gen. 35 3535
K. Z. Stanek et al 2003 ApJ 591 L17
Zhong Su et al 2005 Phys. Med. Biol. 50 2907
L Marder 1978 J. Phys. D: Appl. Phys. 11 2489