Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 446, Issue 4, Pages 4008-4018Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu2371
Keywords
techniques: photometric; stars: individual: RT Aur; stars: individual: SZ Tau; stars: variables: Cepheids
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Funding
- 'Lendulet-Young Researchers' Program of the Hungarian Academy of Sciences
- Hungarian OTKA [K83790]
- European Community [269194, 312844]
- ESA PECS [4000110889/14/NL/NDe]
- Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences
- ES-TEC [4000106398/12/NL/KML]
- Chandra X-ray Center NASA [NAS8-03060]
- NSERC (Canada)
- AFJM
- Austrian Science Fonds [FWF P22691-N16]
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The quantity and quality of satellite photometric data strings is revealing details in Cepheid variation at very low levels. Specifically, we observed a Cepheid pulsating in the fundamental mode and one pulsating in the first overtone with the Canadian MOST (Microvariability and Oscillations of Stars) satellite. The 3.7-d period fundamental mode pulsator (RT Aur) has a light curve that repeats precisely, and can be modelled by a Fourier series very accurately. The overtone pulsator (SZ Tau, 3.1 d period) on the other hand shows light-curve variation from cycle to cycle which we characterize by the variations in the Fourier parameters. We present arguments that we are seeing instability in the pulsation cycle of the overtone pulsator, and that this is also a characteristic of the O - C curves of overtone pulsators. On the other hand, deviations from cycle to cycle as a function of pulsation phase follow a similar pattern in both stars, increasing after minimum radius. In summary, pulsation in the overtone pulsator is less stable than that of the fundamental mode pulsator at both long and short time-scales.
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