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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 atomicemission lines, absorption bands due to photospheric SiO, and the well knownsilicate dust features at $9.7\,\mu$m and $18\,\mu$m. The dust emission,arising in the wind of the secondary star, is fitted by Dusty models formass-loss rates in the range $1.0-1.7\times10^{-7}$M$_{\odot}$yr$^{-1}$. Thesilicate features are similar in profile to those seen in circumstellarenvironments of isolated late-type stars and some dusty symbiotic binaries,although the longer wavelength feature peaks at $17\,\mu$m,, instead of theusual $18\,\mu$m, indicating peculiar grain properties. The dust features arevariable, appearing stronger in 2006-2007 during outburst than in 2008-2009when the system was in the quiescent state. This variability is attributed tochanges in the ultraviolet output and the reformation of the accretion disk,although a decline in the mass-loss rate of the red giant secondary star couldalso play a role. Further observations, in the aftermath of the 2021 eruption,could provide a definitive conclusion.

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