2007A&A...468..425T


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.06CEST20:59:47

2007A&A...468..425T - Astronomy and Astrophysics, volume 468, 425-442 (2007/6-3)

X-ray emission from T Tauri stars and the role of accretion: inferences from the XMM-Newton extended survey of the Taurus Molecular Cloud.

TELLESCHI A., GUEDEL M., BRIGGS K.R., AUDARD M. and PALLA F.

Abstract (from CDS):

T Tau stars display different X-ray properties depending on whether they are accreting (classical T Tau stars; CTTS) or not (weak-line T Tau stars; WTTS). X-ray properties may provide insight into the accretion process between disk and stellar surface. We use data from the XMM-Newton Extended Survey of the Taurus molecular cloud (XEST) to study differences in X-ray properties between CTTS and WTTS. XEST data are used to perform correlation and regression analysis between X-ray parameters and stellar properties. We confirm the existence of a X-ray luminosity (LX) vs. mass (M) relation, LX∝M1.69±0.11, but this relation is a consequence of X-ray saturation and a mass vs. bolometric luminosity (L*) relation for the TTS with an average age of 2.4 Myr. X-ray saturation indicates LX=const. L*, although the constant is different for the two subsamples: const.=10–3.73±0.05 for CTTS and const.=10–3.39±0.06 for WTTS. Given a similar L* distribution of both samples, the X-ray luminosity function also reflects a real X-ray deficiency in CTTS, by a factor of ≃2 compared to WTTS. The average electron temperatures Tav are correlated with LX in WTTS but not in CTTS; CTTS sources are on average hotter than WTTS sources. At best marginal dependencies are found between X-ray properties and mass accretion rates or age. The most fundamental properties are the two saturation laws, indicating suppressed LX for CTTS. We speculate that some of the accreting material in CTTS is cooling active regions to temperatures that may not significantly emit in the X-ray band, and if they do, high-resolution spectroscopy may be required to identify lines formed in such plasma, while CCD cameras do not detect these components. The similarity of the LX vs. Tav dependencies in WTTS and main-sequence stars as well as their similar X-ray saturation laws suggests similar physical processes for the hot plasma, i.e., heating and radiation of a magnetic corona.

Abstract Copyright:

Journal keyword(s): stars: coronae - stars: formation - stars: pre-main sequence - X-rays: stars

Simbad objects: 38

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Number of rows : 38

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 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1697 1
2 2MASS J03542950+3203013 TT* 03 54 29.5045697196 +32 03 01.407089906   12.71 11.85     G0 48 0
3 2MASS J03543017+3203043 TT* 03 54 30.17472 +32 03 04.3488   13.25 12.31     G5 50 0
4 HD 283447 Or* 04 14 12.9232870093 +28 12 12.378540314 13.17 12.07 10.68 9.45 8.67 K3Ve 380 0
5 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 315 0
6 V* V410 Tau Or* 04 18 31.1083261392 +28 27 16.155411536   12.13 10.75 8.45 9.408 K3Ve 424 0
7 HD 283572 Or* 04 21 58.8482823933 +28 18 06.511915195   9.80 9.03 9.14   G5IVe 267 0
8 V* T Tau Or* 04 21 59.4323326335 +19 32 06.439974179   11.01 9.30 9.80   K0IV/Ve 1249 2
9 V* FS Tau Or* 04 22 02.1925017485 +26 57 30.331063489 17.57   14.10 15.63   M3.5e+M0e 257 0
10 HH 276 HH 04 22 07.3 +26 57 26           ~ 5 0
11 2MASS J04270266+2605304 Y*O 04 27 02.66593 +26 05 30.3790           ~ 135 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* DH Tau Or* 04 29 41.5520056304 +26 32 58.123761109 15.14 14.62 13.10 13.01   M1Ve 263 0
14 RAFGL 5123 FU* 04 31 34.07736 +18 08 04.9020           K3V/M3III 811 0
15 V* V1213 Tau Or* 04 31 37.47192 +18 12 24.4800           K7 516 0
16 V* V830 Tau TT* 04 33 10.0299730541 +24 33 43.255853678   13.91 12.08 11.30   M0-1 171 1
17 IRAS S04301+2608 Y*O 04 33 14.3602980976 +26 14 23.494786529           M0 33 0
18 [BLH2002] KPNO-Tau 8 Y*O 04 35 41.8388746981 +22 34 11.595178814 20.64   19.261     M6Ve 35 0
19 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
20 V* DP Tau Or* 04 42 37.6996387891 +25 15 36.992730557 15.84 15.2 13.70 14.42   M0.8 154 1
21 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 930 2
22 V* V1118 Ori Or* 05 34 44.9889538895 -05 33 41.344187987 15.053 15.378 14.430 15.22 12.701 M1e 121 0
23 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1977 1
24 V* V1647 Ori Or* 05 46 13.1370923766 -00 06 04.876812846     18.1     ~ 231 1
25 BD+20 2465 Er* 10 19 36.2808024653 +19 52 12.014037746   10.82 9.52 9.19   M4Vae 1145 0
26 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1532 1
27 V* V645 Cen Er* 14 29 42.9451234609 -62 40 46.170818907 14.21 12.95 11.13 9.45 7.41 M5.5Ve 958 0
28 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
29 * 36 Oph A PM* 17 15 20.7837627960 -26 36 06.120125290   5.93 5.08     K2V 247 0
30 * 36 Oph ** 17 15 20.9839376 -26 36 10.157115           K2V+K1V 116 0
31 * 36 Oph B PM* 17 15 20.9846233161 -26 36 10.159381821   5.88 5.03     K1V 227 0
32 * 70 Oph Ro* 18 05 27.28518 +02 30 00.3558 5.40 4.89 4.03 3.38 2.92 K0-V 607 0
33 * 70 Oph A SB* 18 05 27.370543 +02 29 59.31669       3.6   K0V 206 0
34 * 70 Oph B PM* 18 05 27.4622283249 +02 29 56.223591080   7.26 6.07 5.6   K4V 103 0
35 HD 319139 BY* 18 14 10.4818974563 -32 47 34.516106830   11.47 10.68   9.11 K5+K7 290 0
36 V* AT Mic Er* 20 41 51.15925 -32 26 06.8283 12.753 11.909 10.343 9.098 7.383 M4.5Ve+M4.5Ve 325 0
37 V* EV Lac Er* 22 46 49.7311740821 +44 20 02.372223230   11.85 10.26 9.89   M4.0V 800 2
38 BD+19 5116 ** 23 31 52.17898 +19 56 14.1505 12.737 11.749 10.165 8.982 7.446 M4+M5 419 0

    Equat.    Gal    SGal    Ecl

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2020.07.06-20:59:47

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