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Title: Investigating coronal saturation and supersaturation in fast-rotating M-dwarf stars
Authors: Jeffries, R. D.
Jackson, R. J.
Briggs, K. R.
Evans, P. A.
Pye, J. P.
First Published: 1-Mar-2011
Publisher: Oxford University Press
Citation: Monthly Notices of the Royal Astronomical Society, 2011, 411 (3), pp. 2099-2112
Abstract: At fast rotation rates, the coronal activity of G- and K-type stars has been observed to ‘saturate’ and then decline again at even faster rotation rates – a phenomenon dubbed ‘supersaturation’. In this paper, we investigate coronal activity in fast-rotating M-dwarfs using deep XMM–Newton observations of 97 low-mass stars of known rotation period in the young open cluster NGC 2547 and combine these with published X-ray surveys of low-mass field and cluster stars of known rotation period. Like G- and K-dwarfs, we find that M-dwarfs exhibit increasing coronal activity with decreasing Rossby number N[subscript: R], the ratio of period to convective turnover time, and that activity saturates at L[subscript: X]/L[subscript: bol]≃ 10[superscript: −3] for log N[subscript: R] < −0.8. However, supersaturation is not convincingly displayed by M-dwarfs, despite the presence of many objects in our sample with log N[subscript: R] < −1.8, where supersaturation is observed to occur in higher mass stars. Instead, it appears that a short rotation period is the primary predictor of supersaturation; P ≤ 0.3 d for K-dwarfs and perhaps P ≤ 0.2 d for M-dwarfs. These observations favour the ‘centrifugal stripping’ model for supersaturation, where coronal structures are forced open or become radiatively unstable as the Keplerian corotation radius moves inside the X-ray-emitting coronal volume.
DOI Link: 10.1111/j.1365-2966.2010.17848.x
ISSN: 0035-8711
eISSN: 1365-2966
Version: Publisher Version
Type: Journal Article
Rights: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2010 The Authors Monthly Notices of the Royal Astronomical Society © 2010 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s open access archiving policy.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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