B. F. Lane et al. 2007 ApJ 658 520 doi:10.1086/511414
B. F. Lane1, J. L. Sokoloski2, R. K. Barry3,4, W. A. Traub5, A. Retter6, M. W. Muterspaugh7, R. R. Thompson8, J. A. Eisner9, E. Serabyn5 and B. Mennesson5
Show affiliationsWe report observations of the recurrent nova RS Oph using long-baseline near-IR interferometry. We are able to resolve emission from the nova for several weeks after the 2006 February outburst. The near-IR source initially expands to a size of ~5 mas. However, beginning around day 10, the IR source appears to begin to shrink, reaching ~2 mas by day 100. We combine our measured angular diameters with previously available interferometric and photometric data to derive an emission measure for the source, and hence are able to determine the mass-loss rate of the nova in the days following the outburst.
Issue 1 (2007 March 20)
Received 2006 September 1, accepted for publication 2006 November 28
B. F. Lane et al. 2007 ApJ 658 520
J. A. Eisner et al. 2003 ApJ 588 360
Domenico D'Alessandro 2003 J. Phys. A: Math. Gen. 36 9721
Sébastien Galtier and Eric Buchlin 2007 ApJ 656 560
J. A. Eisner and S. R. Kulkarni 2002 ApJ 574 426
Valerii V Ryazanov et al 2004 Phys.-Usp. 47 732
Zhao Ke et al 2006 Chinese Phys. 15 2338
Kenneth Hong and Edward Teo 2003 Class. Quantum Grav. 20 3269
Stephen J McMahon et al 2008 Phys. Med. Biol. 53 5635
P Blaudeck et al 1992 J. Phys.: Condens. Matter 4 6389