Rotation of Low-mass Stars in Taurus with K2
| العنوان: | Rotation of Low-mass Stars in Taurus with K2 |
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| المؤلفون: | Ann Marie Cody, John R. Stauffer, Trevor J. David, N. Roggero, Lynne A. Hillenbrand, Jerome Bouvier, Luisa Rebull |
| المصدر: | The Astronomical Journal. 159:273 |
| بيانات النشر: | American Astronomical Society, 2020. |
| سنة النشر: | 2020 |
| مصطلحات موضوعية: | 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stellar classification, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, Star formation, Stellar rotation, Molecular cloud, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Pleiades, Low Mass |
| الوصف: | We present an analysis of K2 light curves (LCs) from Campaigns 4 and 13 for members of the young ($\sim$3 Myr) Taurus association, in addition to an older ($\sim$30 Myr) population of stars that is largely in the foreground of the Taurus molecular clouds. Out of 156 of the highest-confidence Taurus members, we find that 81\% are periodic. Our sample of young foreground stars is biased and incomplete, but nearly all (37/38) are periodic. The overall distribution of rotation rates as a function of color (a proxy for mass) is similar to that found in other clusters: the slowest rotators are among the early M spectral types, with faster rotation towards both earlier FGK and later M types. The relationship between period and color/mass exhibited by older clusters such as the Pleiades is already in place by Taurus age. The foreground population has very few stars, but is consistent with the USco and Pleiades period distributions. As found in other young clusters, stars with disks rotate on average slower, and few with disks are found rotating faster than $\sim$2 d. The overall amplitude of the light curves decreases with age and higher mass stars have generally lower amplitudes than lower mass stars. Stars with disks have on average larger amplitudes than stars without disks, though the physical mechanisms driving the variability and the resulting light curve morphologies are also different between these two classes. Comment: 39 pages, 12 figures. Accepted by AJ |
| وصف الملف: | application/pdf |
| تدمد: | 1538-3881 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::71467f3ecda8b72e6baf26236c77ee8d https://doi.org/10.3847/1538-3881/ab893c |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi.dedup.....71467f3ecda8b72e6baf26236c77ee8d |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 15383881 |
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