期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 441, 期 3, 页码 2361-2374出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu728
关键词
techniques: polarimetric; stars: activity; stars: evolution; stars: magnetic field; planetary systems; stars: rotation
资金
- Royal Astronomical Society Fellowship
- Swiss National Science Foundation via an Ambizione Fellowship
- Science and Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship [ST/J003255/1]
- RF via a consolidated grant [ST/J001651/1]
- ANR [Blanc SIMI5-6 020 01]
- STFC [PP/D000890/1, ST/J003255/1, ST/L00139X/1, ST/G001006/1, ST/J001651/1, PP/F000065/1, ST/I000666/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/D000890/1, ST/G001006/1, ST/I000666/1, ST/L00139X/1, ST/J003255/1, PP/F000065/1, ST/J001651/1] Funding Source: researchfish
We investigate how the observed large-scale surface magnetic fields of low-mass stars (similar to 0.1-2 M-aS (TM)), reconstructed through Zeeman-Doppler imaging, vary with age t, rotation and X-ray emission. Our sample consists of 104 magnetic maps of 73 stars, from accreting pre-main sequence to main-sequence objects (1 Myr a parts per thousand(2) t a parts per thousand(2) 10 Gyr). For non-accreting dwarfs we empirically find that the unsigned average large-scale surface field is related to age as t(-0.655 +/- 0.045). This relation has a similar dependence to that identified by Skumanich, used as the basis for gyrochronology. Likewise, our relation could be used as an age-dating method ('magnetochronology'). The trends with rotation we find for the large-scale stellar magnetism are consistent with the trends found from Zeeman broadening measurements (sensitive to large- and small-scale fields). These similarities indicate that the fields recovered from both techniques are coupled to each other, suggesting that small- and large-scale fields could share the same dynamo field generation processes. For the accreting objects, fewer statistically significant relations are found, with one being a correlation between the unsigned magnetic flux and rotation period. We attribute this to a signature of star-disc interaction, rather than being driven by the dynamo.
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