Volume 611, March 2018
|Number of page(s)||19|
|Section||Stellar structure and evolution|
|Published online||04 April 2018|
Frequency dependence of p-mode frequency shifts induced by magnetic activity in Kepler solar-like stars
IRFU, CEA, Université Paris-Saclay,
2 Université Paris Diderot, AIM, Sorbonne Paris Cité, CEA, CNRS, 91191 Gif-sur-Yvette, France
3 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
4 Universidad de La Laguna, Dpto. de Astrofísica, 38205 La Laguna, Tenerife, Spain
Accepted: 15 December 2017
The variations of the frequencies of the low-degree acoustic oscillations in the Sun induced by magnetic activity show a dependence on radial order. The frequency shifts are observed to increase towards higher-order modes to reach a maximum of about 0.8 μHz over the 11-yr solar cycle. A comparable frequency dependence is also measured in two other main sequence solar-like stars, the F-star HD 49933, and the young 1 Gyr-old solar analog KIC 10644253, although with different amplitudes of the shifts of about 2 μHz and 0.5 μHz, respectively. Our objective here is to extend this analysis to stars with different masses, metallicities, and evolutionary stages. From an initial set of 87 Kepler solar-like oscillating stars with known individual p-mode frequencies, we identify five stars showing frequency shifts that can be considered reliable using selection criteria based on Monte Carlo simulations and on the photospheric magnetic activity proxy Sph. The frequency dependence of the frequency shifts of four of these stars could be measured for the l = 0 and l = 1 modes individually. Given the quality of the data, the results could indicate that a physical source of perturbation different from that in the Sun is dominating in this sample of solar-like stars.
Key words: stars: oscillations / stars: solar type / stars: activity / methods: data analysis
© ESO 2018
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