Delorme, P.; Cameron, A. C.; Hebb, L.; Rostron, J. ; Lister, T. A.; Norton, A. J.; Pollacco, D. and West, R. G.
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We present the results of photometric surveys for stellar rotation in the Hyades and in Praesepe, using data obtained as part of the SuperWASP exoplanetary transit-search programme. We determined accurate rotation periods for more than 120 sources whose cluster membership was confirmed by common proper motion and colour-magnitude fits to the clusters' isochrones. This allowed us to determine the effect of magnetic braking on a wide range of spectral types for expected ages of ~600 Myr for the Hyades and Praesepe. Both clusters show a tight and nearly linear relation between J–Ks colour and rotation period in the F, G and K spectral range. This confirms that loss of angular momentum was significant enough that stars with strongly different initial rotation rates have converged to the same rotation period for a given mass, by the age of Hyades and Praesepe. In the case of the Hyades our colour-period sequence extends well into the M dwarf regime and shows a steep increase in the scatter of the colour-period relation, with identification of numerous rapid rotators from ~0.5M☉ down to the lowest masses probed by our survey (~0.25M☉). This provides crucial constraints on the rotational braking timescales and further clears the way to use gyrochronology as an accurate age measurement tool for main-sequence stars.
|Item Type:||Conference Item|
|Copyright Holders:||2011 Astronomical Society of the Pacific|
|Extra Information:||16th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
Ed. Christopher M. Johns-Krull, Matthew K. Browning, and Andrew A. West,
28 August – 2 September, 2010 Seattle, Washington
Print ISBN: 978-1-58381-776-6
E-book ISBN: 978-1-58381-777-3
|Academic Unit/Department:||Science > Physical Sciences|
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Andrew Norton|
|Date Deposited:||10 May 2012 09:52|
|Last Modified:||17 Nov 2012 18:17|
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