A Spectroscopic and Evolutionary Study of the Pre-Cataclysmic Variable Nn-Serpentis

Details A Spectroscopic and Evolutionary Study of the Pre-Cataclysmic Variable Nn-Serpentis A Spectroscopic and Evolutionary Study of the Pre-Cataclysmic Variable Nn-Serpentis

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.269..879c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 269, NO. 4/AUG15, P. 879, 1994

Astronomy and Astrophysics

Astronomy

34

Scientific paper

Phase-resolved spectra of NN Ser taken in the blue and far red are presented. The spectra show Balmer lines in absorption, characteristic of hot white dwarf stars, and phase-dependent narrow single-peaked Balmer, He 1 and Ca ii lines in emission, which we interpret as reprocessed light coming from the illuminated hemisphere of the red dwarf. We classify the primary as a DAO 1 white dwarf, with an age in the range 1 06 1 0 yr. A cross-correlation technique was applied to find the radial velocities of the emission features. We find the semi-amplitude of the radial velocity curve for the Ha line to be K2=310I10 km 1 Based on this and previous observational data, we derive a complete set of system parameters for NN Ser (Table 4). A study of the reflection effect on the secondary star shows symmetric heating only on the surface directly facing the primary star. An initial estimate of the temperature of the illuminated part yields 5650 < T*j1 < 8150 K. The evolutionary implications of our results based on current theoretical stellar models make it probable that this system will show cataclysmic activity in about 2.2 x 1 0 yr. Key words: binaries: close - binaries: eclipsing - stars: evolution - stars: fundamental parameters - stars: individual: NN Ser - white dwarfs.

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