The slow nova V1819 Cygni (Nova Cygni 1986)

Details The slow nova V1819 Cygni (Nova Cygni 1986) The slow nova V1819 Cygni (Nova Cygni 1986)

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989aj.....98..297w&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 98, July 1989, p. 297-310.

Astronomy and Astrophysics

Astronomy

26

Cygnus Constellation, Interstellar Extinction, Light Curve, Novae, Stellar Spectra, Balmer Series, H Alpha Line, H Beta Line, Radiative Transfer

Scientific paper

Spectrophotometric and spectropolarimetric observations of the slow nova Cygni 1986 were obtained with the 36-in Pine Bluff Observatory telescope beginning about one week after maximum and continuing for one-two years after maximum. An E(B-V) value of about 0.35 is found. In the months following maximum light, the Balmer decrement was extremely steep and variable with time. Departures from case B radiative transfer noted throughout most of the observational period are consistent with self-absorption of the Balmer lines due to high densities in parts of the nova shell. The results suggest that at 11 months after maximum the shell density was about 10 to the 7th/cu cm, dropping to about 10 to the 6th/cu cm two years after maximum.

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