Spectral and Photometric Evolution of the Symbiotic Nova HM Sagittae in 1986-2002

Details Spectral and Photometric Evolution of the Symbiotic Nova HM Sagittae in 1986-2002 Spectral and Photometric Evolution of the Symbiotic Nova HM Sagittae in 1986-2002

Apr 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004astl...30..258a&link_type=abstract

Astronomy Letters, vol. 30, p. 258-267 (2004)

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the results of our photometric and spectroscopic observations of the symbiotic nova HM Sge in 1994-2002. After its outburst in 1975, the star was shown to fade in the U, B, V bands at a rate of about 0.5 mag per year. The behavior of the B-V and U-B color indices reflects the variations of emission lines and, in part, the fading of the erupted component. We have studied the evolution of the emission spectrum in the range from H_delta to lambda 7751 A over the period 1986-2002. The absolute fluxes in the hydrogen lines decreased by half, the ionization of the gaseous envelope continued to increase, and the Raman O VI lines appeared and strengthened. The significant (threefold) decrease in the ratio of the auroral and nebular O III lines is interpreted as a drop in the electron temperature of the envelope as its density decreased by a factor of about 1.5. We have measured the absolute intensity of the near-infrared continuum up to 10000 A and show that the infrared continuum follows the pulsations of the Mira star in the system HM Sge. We conclude that the dust envelope around the cool component became noticeably transparent in the 1990s.

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