CSI 2264: Accretion process in classical T Tauri stars in the young cluster NGC 2264

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Volume 586 (February 2016)

A&A, 586 (2016) A47

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Table 7

Parameters used to calculate corotation radius (R_C) and magnetic field strength (B_∗) of the three AA Tau-like stars that present observational evidence that the inner disk warp is located at the corotation radius.

Mon ID^a	M _∗ ^b	R _∗ ^c	Ṁ _Hα ^d	P_CoRoT_2011 ^e	P _Hα ^f	R _C ^g	B _∗ ^h
	(M_⊙)	(R_⊙)	(M_⊙/ yr)	(days)	(days)	(R_∗)	(kG)


CSIMon-000250	1.63	1.35	1.44e-09	8.93	7.5/8.9	12.3	0.81
CSIMon-000660	1.86	1.4	1.45e-10	5.10	5.2	7.5	0.07
CSIMon-000811	0.91	1.97	6.75e-09	7.88	7.9/12.5*	8.2	0.44

Notes.

^(a)

CSIMon is an internal identification of the CSI 2264 campaign.

^(b)

Stellar mass obtained by Venuti et al. (2014).

^(c)

Stellar radius obtained by Venuti et al. (2014).

^(d)

Mass-accretion rates calculated with Hα equivalent width.

^(e)

Photometric period obtained from the 2011 CoRoT light curve.

^(f)

Period obtained with the Hα line from FLAMES spectra.

^(g)

Calculated corotation radius.

^(h)

Calculated stellar magnetic field.

^(*)

This star shows only a faint hint of periodicity in Hα at the photometric period (~7.9 days) that we used as the stellar rotational period.

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