A1 Refereed original research article in a scientific journal
Young solar type active stars: the TYC 2627-638-1 system
Authors: Olah K, Korhonen H, Vida K, Ilyin I, Dall TH, Jarvinen SP, Jurcsik J, Andersen MI, Djupvik AA, Pursimo T, Moor A, Datson J, Karjalainen R, Liimets T, Kubat J, Kawka A
Publisher: EDP SCIENCES S A
Publication year: 2010
Journal: Astronomy and Astrophysics
Journal name in source: ASTRONOMY & ASTROPHYSICS
Journal acronym: ASTRON ASTROPHYS
Article number: ARTN A81
Volume: 515
Number of pages: 11
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/200912892
Abstract
Both components of the wide binary have clear emission cores in the Ca II H&K lines and filled-in H alpha absorption, indicating that both stars are chromospherically active. Our photometric time series reveals clear but only a few hundredths of a magnitude amplitude rotational modulation, which is most likely due to cool starspots. Two distinct periods, near 3.5 and 3.7 days, are found in the brightness variations. Photometry obtained separately of the two components of the wide binary show that these periodicities belong to the brighter star. The fainter component shows a much slower light variation of about 0.3 mag. amplitude. In addition, long-term changes in the brightness of both stars are seen. The spectral energy distribution shows a strong near-infrared excess in the fainter component of the wide binary.
Both components of the wide binary have clear emission cores in the Ca II H&K lines and filled-in H alpha absorption, indicating that both stars are chromospherically active. Our photometric time series reveals clear but only a few hundredths of a magnitude amplitude rotational modulation, which is most likely due to cool starspots. Two distinct periods, near 3.5 and 3.7 days, are found in the brightness variations. Photometry obtained separately of the two components of the wide binary show that these periodicities belong to the brighter star. The fainter component shows a much slower light variation of about 0.3 mag. amplitude. In addition, long-term changes in the brightness of both stars are seen. The spectral energy distribution shows a strong near-infrared excess in the fainter component of the wide binary.
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