UV and optical line emission from the shell of the old nova GK Persei

Details UV and optical line emission from the shell of the old nova GK Persei UV and optical line emission from the shell of the old nova GK Persei

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281a.183b&link_type=abstract

In ESA, A Decade of UV Astronomy with the IUE Satellite, Volume 1 p 183-185 (SEE N89-10682 01-89)

Astronomy and Astrophysics

Astronomy

4

Iue, Novae, Spaceborne Astronomy, Stellar Envelopes, Ultraviolet Astronomy, Abundance, Ejecta, Emission Spectra, Spectral Line Width

Scientific paper

Ultraviolet line emission is found in IUE spectra taken of the brightest region (bar) of the shell of GK Per in 1987. This makes the remnant of the nova of 1901 the first classical nova nebula to be detected in wavelengths from the radio region to the ultraviolet. Results suggest that the spectral line ratios can be fitted by a shock model assuming an underabundance of hydrogen and an overabundance of nitrogen. The observed shock velocities in the range 100 to 200 km/sec are characteristic of reverse shocks entering the nova ejecta.

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