Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21349121l&link_type=abstract
American Astronomical Society, AAS Meeting #213, #491.21; Bulletin of the American Astronomical Society, Vol. 41, p.470
Astronomy and Astrophysics
Astronomy
Scientific paper
The recurrent nova RS Ophiuchi was well studied at all wavelengths after the 2006 outburst; we present an investigation of the evolution of the nebula in RS Oph from the quiescent period before the 2006 outburst through the current quiescent period. We use optical spectroscopy of the nebula and measure equivalent widths and fluxes of the emission lines of the H Balmer series, HeIλ5875, 6875, 4471, 7281, 7065, HeIIλ4686, O and Fe lines. The detailed time coverage of this data allows us to study the evolution of the nebula on long time-scales, before and after outburst. We find that the temperature and emitting volume of the nebula increase after the outburst, as expected, and by JD2454200 (April 9, 2007) RS Oph resumes quiescence values for EW of all the emission lines measured. From comparing the light curve for Hα to models created by Hachisu et al. (2007) we suggest that the emission of this line comes from both the nebula and an accretion disk. We use the flux ratio of Hα to Hβ to constrain the density of the nebula to. We also compare theoretical predictions of the white dwarf and nebula temperature evolution with our measurements and find good agreements. This work is supported in part by the NSF REU and DOD ASSURE programs under NSF grant no. 0754568 and by the Smithsonian Institution.
Kenyon Scott
Luna Gerardo J. M.
Lynch Christene R.
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