Application of the O-C technique in the pulsating pre-white dwarf star PG0122+200

Details Application of the O-C technique in the pulsating pre-white dwarf star PG0122+200 Application of the O-C technique in the pulsating pre-white dwarf star PG0122+200

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..256...51f&link_type=abstract

Observational Aspects of Pulsating B- and A Stars, ASP Conference Proceedings, Vol. 256. Edited by Christiaan Sterken and Donal

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The photometric results obtained on PG0122+200 during five observing seasons are presented. The light curves are used to get maximum times of the dominant frequency f=2.497 mHz for each observing night. However, the O-C technique has not yet been applied to the times due to the uncertainty in counting the cycle numbers, which results from the big gaps between the observing runs and the insufficient precision in the frequency determination. A possible solution to this problem is to observe this star with two runs within a 3-month interval. This will be implemented in October and December 2001 by multi-site observing campaigns to obtain the secular change of the dominant frequency and give an observational limit to the evolutionary time-scale of PG0122+200.

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