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Double radio peak and non-thermal collimated ejecta in RS Ophiuchi following the 2006 outburst

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dc.contributor.author Eyres, S. P. S
dc.contributor.author O'Brien, T. J
dc.contributor.author Beswick, R
dc.contributor.author Muxlow, T. W. B
dc.contributor.author Anupama, G. C
dc.contributor.author Kantharia, N. G
dc.contributor.author Bode, M. F
dc.contributor.author Gawroński, M. P
dc.contributor.author Feiler, R
dc.contributor.author Evans, A
dc.contributor.author Rushton, M. T
dc.contributor.author Davis, R. J
dc.contributor.author Prabhu, T
dc.contributor.author Porcas, R
dc.contributor.author Hassall, B. J. M
dc.date.accessioned 2009-05-18T16:06:50Z
dc.date.available 2009-05-18T16:06:50Z
dc.date.issued 2009-05
dc.identifier.citation Monthly Notices of the Royal Astronomical Society, Vol. 395, No. 3, pp. 1533 - 1540 en
dc.identifier.issn 0035-8711
dc.identifier.uri http://hdl.handle.net/2248/4464
dc.description.abstract We report Multi-Element Radio-Linked Interferometer Network, Very Large Array, One-Centimetre Radio Array, Very Long Baseline Array (VLBA), Effelsberg and Giant Metrewave Radio Telescope observations beginning 4.5 days after the discovery of RS Ophiuchi undergoing its 2006 recurrent nova outburst. Observations over the first 9 weeks are included, enabling us to follow spectral development throughout the three phases of the remnant development. We see dramatic brightening on days 4 to 7 at 6 GHz and an accompanying increase in other bands, particularly 1.46 GHz, consistent with transition from the initial `free expansion' phase to the adiabatic expansion phase. This is complete by day 13 when the flux density at 5 GHz is apparently declining from an unexpectedly early maximum (compared with expectations from observations of the 1985 outburst). The flux density recovered to a second peak by approximately day 40, consistent with behaviour observed in 1985. At all times the spectral index is consistent with mixed non-thermal and thermal emission. The spectral indices are consistent with a non-thermal component at lower frequencies on all dates, and the spectral index changes show that the two components are clearly variable. The estimated extent of the emission at 22 GHz on day 59 is consistent with the extended east and west features seen at 1.7 GHz with the VLBA on day 63 being entirely non-thermal. We suggest a two-component model, consisting of a decelerating shell seen in mixed thermal and non-thermal emission plus faster bipolar ejecta generating the non-thermal emission, as seen in contemporaneous VLBA observations. Our estimated ejecta mass of 4 +/- 2 × 10-7Msolar is consistent with a white dwarf (WD) mass of 1.4Msolar. It may be that this ejecta mass estimate is a lower limit, in which case a lower WD mass would be consistent with the data. en
dc.language.iso en en
dc.publisher Blackwell Publishing en
dc.relation.uri http://arxiv.org/abs/0902.2265 en
dc.relation.uri http://adsabs.harvard.edu/abs/2009MNRAS.395.1533E en
dc.rights © Royal Astronomical Society en
dc.subject Stars: Individual: RS Oph en
dc.subject Novae en
dc.subject Cataclysmic Variables en
dc.subject Stars: Winds en
dc.subject Outflows en
dc.subject Radio Continuum: Stars en
dc.title Double radio peak and non-thermal collimated ejecta in RS Ophiuchi following the 2006 outburst en
dc.type Article en

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