Rotational velocities of nearby young stars | Astronomy & Astrophysics (A&A)

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Volume 517 (July 2010)

A&A, 517 (2010) A88

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Table 2:

Sub-samples used to investigate the dependence of $v\sin i$ on the evolutionary state of the stars.
Sub-sample	Description	$n_{\rm stars}$	$n_{\rm M-stars}$	$\langle{\rm Age}\rangle$	$\langle v\sin i\rangle$	$\sigma_{v\sin i}$	Results
				Myr	km s^-1	km s^-1
(i)	accreting stars	11	3	5	$10\pm 1$	$3\pm 1$	small $\langle v\sin i\rangle$ , no fast rotators
(ii)	non-accreting stars, thick disks	12	4	7	$15\pm 2$	$8\pm 2$	larger $\langle v\sin i\rangle$ , fast rotators
(iii)	stars with debris disks	23	2	33	$10\pm 1$	$5\pm 1$	small $\langle v\sin i\rangle$ , fast rotators
(iv)	stars without disks	81	1	90	$11\pm 1$	$4\pm 1$	small $\langle v\sin i\rangle$ , tail of fast rotators
(v)	no disk info, same age as (iv)	81	3	90	$7\pm 1$	$2\pm 1$	similar to (iv)
(iv)+(v)	combined (iv)+(v)	162	4	90	$8\pm1$	$2\pm 1$	small $\langle v\sin i\rangle$ , tail of fast rotators

Notes. We list the selection criteria for the sub-sample, the number of stars and M-type lower-mass stars, mean age, $v\sin i$ , and the width of the Gaussian fit to the distribution $\sigma_{v\sin i}$ .

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