تقرير
A New Asteroseismic $\textit{Kepler}$ Benchmark Constrains the Onset of Weakened Magnetic Braking in Mature Sun-Like Stars
العنوان: | A New Asteroseismic $\textit{Kepler}$ Benchmark Constrains the Onset of Weakened Magnetic Braking in Mature Sun-Like Stars |
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المؤلفون: | Bhalotia, Vanshree, Huber, Daniel, van Saders, Jennifer L., Metcalfe, Travis S., Stassun, Keivan G., White, Timothy R., Børsen-Koch, Víctor Aguirre, Ball, Warrick H., Basu, Sarbani, Serenelli, Aldo M., Sawczynec, Erica, Guzik, Joyce A., Howard, Andrew W., Isaacson, Howard |
سنة النشر: | 2024 |
المجموعة: | Astrophysics |
مصطلحات موضوعية: | Astrophysics - Solar and Stellar Astrophysics |
الوصف: | Stellar spin down is a critical yet poorly understood component of stellar evolution. In particular, results from the Kepler Mission imply that mature age, solar-type stars have inefficient magnetic braking, resulting in a stalled spin down rate. However, a large number of precise asteroseismic ages are needed for mature ($\geq$ 3Gyr) stars in order to probe the regime where traditional and stalled spin-down models differ. In this paper, we present a new asteroseismic benchmark star for gyrochronology discovered using reprocessed Kepler short cadence data. KIC 11029516 (Papayu) is a bright ($K_{p}$ = 9.6 mag) solar-type star with well-measured rotation period (21.1$\pm$0.8 days) from spot modulation using 4 years of Kepler long cadence data. We combine asteroseismology and spectroscopy to obtain $T_{eff}=5888\pm100$ K, $\rm{[Fe/H]} = 0.30 \pm 0.06\,$ dex, $M = 1.24 \pm 0.05 M_{\odot}$, $R = 1.34 \pm 0.02 R_{\odot}$ and age of 4.0 $\pm$ 0.4 Gyr, making Papayu one of the most similar stars to the Sun in terms of temperature and radius with an asteroseismic age and a rotation period measured from spot modulation. We find that Papayu sits at the transition of where traditional and weakened spin-down models diverge. A comparison with stars of similar zero-age main-sequence temperatures supports previous findings that weakened spin-down models are required to explain the ages and rotation periods of old solar-type stars. |
نوع الوثيقة: | Working Paper |
URL الوصول: | http://arxiv.org/abs/2405.12362 |
رقم الأكسشن: | edsarx.2405.12362 |
قاعدة البيانات: | arXiv |
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