New photometric and spectroscopic observations of the central star of Abell 35

Details New photometric and spectroscopic observations of the central star of Abell 35 New photometric and spectroscopic observations of the central star of Abell 35

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...261..314j&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 261, no. 1, p. 314-320.

Astronomy and Astrophysics

Astrophysics

4

Binary Stars, G Stars, Planetary Nebulae, Stellar Activity, Stellar Spectrophotometry, Subgiant Stars, Chromosphere, Emission Spectra, Stellar Atmospheres, Stellar Evolution

Scientific paper

We report on new photometric and spectroscopic observations carried out in 1989 and 1990 of the visible central star LW Hya = BD-22 3467 deg of the planetary nebula Abell 35. The period of P = 0.766 days we have already found in 1986 and 1987 (Jasniewicz and Acker, 1988) is confirmed by the 1990 photometric data, but no photometric variations were found in the 1989 observing run. A second periodicity not yet very well established seems probable (4.2 or 1.9 yr). In addition we have detected emission cores in the H and K Ca II lines: they also vary in intensity both on short and long-term intervals of time. Nevertheless, the short-term variations of Ca II are poorly related to the short photometric period (0.766 d) but seem to be somewhat in antiphase. New spectroscopic observations will be necessary to estimate correctly the long period of the Ca II emission variations. We can thus conclude that a chromospheric activity develops probably at the surface of the subgiant G8 component of the binary system, on the basis of the presence of Ca II emission line cores and on the presence of dark spots deduced by us previously (Acker and Jasniewicz, 1990) to explain brightness variations.

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