Dust evolution in Nova Cassiopeia 1993

S. P.S. Eyres*, T. R. Geballe, J. M. C. Rawlings, A. Evans, J. K. Davies

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review


We present UKIRT spectroscopy of Nova Cassiopeia 1993 (= V705 Cas) in KLNQ bands, taken in 1994 and 1995. Fitting the continuum indicates a dust temperature T ∼ 740-750 K in the latter part of 1994; this is similar to earlier measurements, and consistent with the "isothermal" behaviour observed in novae with optically thick dust shells. The β-index drops from 0.8 to 0.4 over the same period. This suggests grain growth; grain diameter increases from < 0.54 μm around day 256, to > 0.57 μm by day 342. The UIR features differ from those in other Galactic sources, and are similar to those in V842 Gen. This suggests fundamental differences between the UIR carriers, or environments, in novae and other Galactic sources. The silicate feature is consistent with an amorphous structure, in contrast to previous novae. We believe that grains in V705 Gas form two populations: silicates, and hydrocarbons.

Original languageEnglish
Pages (from-to)303-309
Number of pages7
JournalAstrophysics and Space Science
Issue number1-2
Publication statusPublished - 1997


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