Rise and fall of silicate dust in RS Ophiuchi following the 2006 eruption

We present an analysis of archival Spitzer InfraRed Spectrograph (IRS) observations of the recurrent nova RS Ophiuchi obtained on several occasions, beginning about 7 months after the outburst in 2006. These data show atomic emission lines, absorption bands due to photospheric SiO, and the well-known silicate dust features at 9.7 and 18 mu m. The dust emission, arising in the wind of the secondary star, is fitted by DUSTY models for mass-loss rates in the range 1.0-1.7 x 10(-7) M-circle dot yr(-1). The silicate features are similar in profile to those seen in circumstellar environments of isolated late-type stars and some dusty symbiotic binaries, although the longer wavelength feature peaks at 17 mu m, instead of the usual 18 mu m, indicating peculiar grain properties. The dust features are variable, appearing stronger in 2006-2007 during outburst than in 2008-2009 when the system was in the quiescent state. This variability is attributed to changes in the ultraviolet output and the reformation of the accretion disc, although a decline in the mass-loss rate of the red giant secondary star could also play a role. Further observations, in the aftermath of the 2021 eruption, could provide a definitive conclusion.

Automated summary

An analysis of archival Spitzer IRS observations of RS Ophiuchi reveals atomic emission lines, absorption bands due to photospheric SiO, and silicate dust features. The variability of these dust features is influenced by changes in ultraviolet output, accretion disk reformulation, and a potential decline in the mass-loss rate of the red giant secondary star.