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Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: The early phase

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posted on 24.10.2012, 09:06 by A. Evans, T. Kerr, A. Adamson, B. Yang, Y. Matsuoka, Y. Tsuzuki, M. F. Bode, S. P. S. Eyres, T. R. Geballe, C. E. Woodward, R. D. Gehrz, D. K. Lynch, R. J. Rudy, R. W. Russell, T. J. O'Brien, R. J. Davis, S. G. Starrfield, J-U. Ness, J. Drake, J. P. Osborne, K. L. Page, G. Schwarz, J. Krautter
We present infrared spectroscopy of the recurrent nova RS Ophiuchi, obtained 11.81, 20.75 and 55.71 d following its 2006 eruption. The spectra are dominated by hydrogen recombination lines, together with He i, O i and O ii lines; the electron temperature of ∼104 K implied by the recombination spectrum suggests that we are seeing primarily the wind of the red giant, ionized by the ultraviolet flash when RS Oph erupted. However, strong coronal emission lines (i.e. emission from fine structure transitions in ions having high ionization potential) are present in the last spectrum. These imply a temperature of 930 000 K for the coronal gas; this is in line with X-ray observations of the 2006 eruption. The emission linewidths decrease with time in a way that is consistent with the shock model for the X-ray emission.

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Citation

Monthly Notices of the Royal Astronomical Society: LETTERS, 2007, 374 (1)

Version

VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society: LETTERS

Publisher

Royal Astronomical Society (RAS)

issn

1745-3933

Copyright date

2006

Available date

24/10/2012

Publisher version

http://mnrasl.oxfordjournals.org/content/374/1/L1

Language

en

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