A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Young solar type active stars: the TYC 2627-638-1 system
Tekijät: 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
Kustantaja: EDP SCIENCES S A
Julkaisuvuosi: 2010
Lehti:: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: ASTRONOMY & ASTROPHYSICS
Lehden akronyymi: ASTRON ASTROPHYS
Artikkelin numero: ARTN A81
Vuosikerta: 515
Sivujen määrä: 11
ISSN: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/200912892
Tiivistelmä
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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