Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 452, Issue 3, Pages 2654-2674Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv1493
Keywords
asteroseismology; methods: data analysis; stars: interiors; stars: oscillations; stars: rotation; stars: solar-type
Categories
Funding
- Japan Society for Promotion of Science (JSPS) [25-13316]
- JSPS KAKENHI [26400219]
- CNES
- Grants-in-Aid for Scientific Research [13F03316, 26400219] Funding Source: KAKEN
Ask authors/readers for more resources
The rotation rates in the deep interior and at the surface of 22 main-sequence stars with masses between 1.0 and 1.6 M-circle dot are constrained by combining asteroseismological analysis with spectroscopic measurements. The asteroseismic data of each star are taken by the Kepler or CoRoT space mission. It is found that the difference between the surface rotation rate and the average rotation rate (excluding the convective core) of most of stars is small enough to suggest that an efficient process of angular momentum transport operates during and/or before the main-sequence stage of stars. If each of the surface convective zone and the underlying radiative zone, for individual stars, is assumed to rotate uniformly, the difference in the rotation rate between the two zones turns out to be no more than a factor of 2 in most of the stars independently of their ages.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available