Quantifying Irregularity in Pulsating Red Giants

Details Quantifying Irregularity in Pulsating Red Giants Quantifying Irregularity in Pulsating Red Giants

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009javso..37...71p&link_type=abstract

The Journal of the American Association of Variable Star Observers, vol. 37, no. 2, p. 71

Physics

6

Scientific paper

Hundreds of red giant variable stars are classified as “type L,” which the General Catalogue of Variable Stars (GCVS) defines as “slow irregular variables of late spectral type...which show no evidence of periodicity, or any periodicity present is very poorly defined....” Self-correlation (Percy and Muhammed 2004) is a simple form of time-series analysis which determines the cycle-to-cycle behavior of a star, averaged over all the available data. It is well suited for analyzing stars which are not strictly periodic. Even for non-periodic stars, it provides a “profile” of the variability, including the average “characteristic time” of variability. We have applied this method to twenty-three L-type variables which have been measured extensively by AAVSO visual observers. We find a continuous spectrum of behavior, from irregular to semiregular.

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