2007A&A...468..413B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST16:11:37

2007A&A...468..413B - Astronomy and Astrophysics, volume 468, 413-424 (2007/6-3)

The X-ray activity-rotation relation of T Tauri stars in Taurus-Auriga.

BRIGGS K.R., GUEDEL M., TELLESCHI A., PREIBISCH T., STELZER B., BOUVIER J., REBULL L., AUDARD M., SCELSI L., MICELA G., GROSSO N. and PALLA F.

Abstract (from CDS):

The Taurus-Auriga star-forming complex hosts the only population of T Tauri stars in which an anticorrelation of X-ray activity and rotation period has been observed. We aim to explain the origin of the X-ray activity-rotation relation in Taurus-Auriga. We also aim to put the X-ray activity of these stars into the context of the activity of late-type main-sequence stars and T Tauri stars in the Orion Nebula Cluster. We have used XMM-Newton's European Photon Imaging Cameras to perform the most sensitive survey to date of X-ray emission (0.3-10keV) from young stars in Taurus-Auriga. We investigated the dependences of X-ray activity measures - X-ray luminosity, LX, its ratio with the stellar luminosity, LX/L*, and the surface-averaged X-ray flux, FXS - on rotation period and compared them with predictions based solely on the observed dependence of LX on a star's L* and whether it is accreting or not. We tested for differences in the distributions of LX/L* of fast and slow rotators, accretors and non-accretors, and compared the dependence of LX/L* on the ratio of the rotation period and the convective turnover timescale, the Rossby number, with that of late-type main-sequence stars. We found significant anticorrelations of LX and FXS with rotation period, but these could be explained by the typically higher stellar luminosity and effective temperature of fast-rotators in Taurus-Auriga and a near-linear dependence of LX on L*. We found no evidence for a dependence of LX/L* on rotation period, but for accretors to have lower LX/L* than non-accretors at all rotation periods. The Rossby numbers of accretors and non-accretors were found to be the same as those of late-type main-sequence stars showing saturated X-ray emission. Non-accreting T Tauri stars show X-ray activity entirely consistent with the saturated activity of fast-rotating late-type main-sequence stars. Accreting T Tauri stars show lower X-ray activity, but this cannot be attributed to their slower rotation.

Abstract Copyright:

Journal keyword(s): stars: pre-main sequence - stars: activity - stars: rotation - X-rays: stars - open clusters and associations: individual: Taurus-Auriga

Simbad objects: 28

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Number of rows : 28

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 2MASS J04034930+2610520 TT* 04 03 49.308 +26 10 52.03   15.99 14.52     M3.9 61 0
2 2MASS J04035084+2610531 TT* 04 03 50.8393021714 +26 10 53.015575434   15.57 14.17     M2.8 52 0
3 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 315 0
4 NAME CoKu Tau 1 Y*O 04 18 51.4865838204 +28 20 26.105713878     19.3     K7+M 76 0
5 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 648 1
6 HD 283572 Or* 04 21 58.8482823933 +28 18 06.511915195   9.80 9.03 9.14   G5IVe 267 0
7 V* FS Tau Or* 04 22 02.1925017485 +26 57 30.331063489 17.57   14.10 15.63   M3.5e+M0e 257 0
8 EM* LkCa 21 Or* 04 22 03.1462377202 +28 25 39.099044680   10.94       M3/4Ve 76 0
9 IRAS F04192+2647 TT* 04 22 16.7670021430 +26 54 57.171796087 18.78 18.9 17.8     M1IVe 37 0
10 V* FV Tau Or* 04 26 53.5415038432 +26 06 53.942994170 19.58     15.26   K5 125 2
11 CoKu FV Tau c TT* 04 26 54.4012605412 +26 06 50.942995443 20.35   16.70     M3.5e+M2.5e 60 0
12 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
13 V* GV Tau TT* 04 29 23.7314759229 +24 33 00.216016292 19.20         K7 271 2
14 V* DH Tau Or* 04 29 41.5520056304 +26 32 58.123761109 15.14 14.62 13.10 13.01   M1Ve 263 0
15 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1216 0
16 V* V1213 Tau Or* 04 31 37.47192 +18 12 24.4800           K7 516 0
17 V* XZ Tau Or* 04 31 40.0868968022 +18 13 56.642439056     10.40 13.12   M2e+M2e 408 1
18 V* GH Tau Or* 04 33 06.2181025969 +24 09 33.628411049     13.20 12.59   M3Ve 167 0
19 V* V830 Tau TT* 04 33 10.0299730541 +24 33 43.255853678   13.91 12.08 11.30   M0-1 171 1
20 IRAS S04301+2608 Y*O 04 33 14.3602980976 +26 14 23.494786529           M0 33 0
21 V* HO Tau Or* 04 35 20.2103777721 +22 32 14.557063236     15.20     M0.5 106 0
22 [BLH2002] KPNO-Tau 8 Y*O 04 35 41.8388746981 +22 34 11.595178814 20.64   19.261     M6Ve 35 0
23 CoKu HP Tau G2 Or* 04 35 54.1553246504 +22 54 13.404170652 13.63 12.31 11.158 10.14 9.172 G2e 113 0
24 JH 223 TT* 04 40 49.5107760683 +25 51 18.966786927 18.25     15.09   M2.8 47 0
25 ITG 33A TT* 04 41 08.2613426749 +25 56 07.368386155           M3 39 0
26 V* DP Tau Or* 04 42 37.6996387891 +25 15 36.992730557 15.84 15.2 13.70 14.42   M0.8 154 1
27 V* SU Aur Or* 04 55 59.3861369488 +30 34 01.499800471   10.33 9.30 9.17   G2IIIne 533 0
28 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1977 1

    Equat.    Gal    SGal    Ecl

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2020.07.08-16:11:37

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