2000ApJ...532..474S


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.22CET09:50:54

2000ApJ...532..474S - Astrophys. J., 532, 474-486 (2000/March-3)

Accretion-induced lithium line enhancements in classical T Tauri stars: RW Aurigae.

STOUT-BATALHA N.M., BATALHA C.C. and BASRI G.S.

Abstract (from CDS):

It is widely accepted that much of the stochastic variability of T Tauri stars is due to accretion by a circumstellar disk. The emission-line spectrum as well as the excess continuum emission are common probes of this process. In this communication, we present additional probes of the circumstellar environment in the form of resonance lines of low ionization potential elements. Using a set of 14 high-resolution echelle observations of the classical T Tauri star (CTTS) RW Aur, taken between 1986 and 1996, we carefully measure the continuum veiling at each epoch by comparing more than 500 absorption lines with those of an appropriate template. This allows us to accurately subtract out the continuum emission and to recover the underlying photospheric spectrum. In doing so, we find that selected photospheric lines are enhanced by the accretion process, namely, the resonance lines of Li I and K I. A resonance line of Ti I and a low excitation potential line of Ca I also show weak enhancements. Simple slab models and computed line bisectors lead us to propose that these line enhancements are markers of cool gas at the beginning of the accretion flow which provides an additional source of line opacity. These results suggest that published values of surface lithium abundances of classical T Tauri stars are likely to be overestimated. This would account for the various reports of surface lithium abundances in excess of meteoritic values among the extreme CTTSs. Computing LTE lithium abundances of RW Aur in a low and then high accretion state yields abundances which vary by 1 order of magnitude. The low accretion state lithium abundance is consistent with theoretical predictions for a star of this age and mass, while the high accretion state spectrum yields a supermeteoritic lithium abundance.

Abstract Copyright:

Journal keyword(s): Accretion, Accretion Disks - Stars: Circumstellar Matter - Stars: Abundances - Stars: Individual: Constellation Name: RW Aurigae - Stars: Late-Type - Stars: Pre-Main-Sequence

CDS comments: p.482 : Oph120S = NTTS 162814-2427 , Oph052 = NTTS 160905-1859

Simbad objects: 44

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Number of rows : 44

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 * 54 Psc PM* 00 39 21.8055114029 +21 15 01.716052732 7.29 6.71 5.88 5.21 4.82 K0.5V 515 1
2 HD 3765 PM* 00 40 49.2699101367 +40 11 13.819725965   8.30   6.8   K2V 230 0
3 * 107 Psc PM* 01 42 29.7634932653 +20 16 06.660242064 6.57 6.08 5.24 4.55 4.12 K1V 493 0
4 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1068 1
5 HD 16160 PM* 02 36 04.9023844802 +06 53 12.431588708   6.81   5.2   K3V 477 1
6 NGC 1039 OpC 02 42 05 +42 45.7           ~ 363 0
7 HD 19305 PM* 03 06 26.7371937234 +01 57 54.628015605 11.697 10.44 9.055 8.201 7.427 M0V 113 0
8 * kap01 Cet BY* 03 19 21.6963205 +03 22 12.715139 5.71 5.52 4.85 4.27 3.91 G5V 811 0
9 Cl Melotte 20 OpC 03 26 42 +48 48.0           ~ 741 0
10 V* OU Tau Fl* 03 45 32.9382648825 +24 18 11.647131333   14.63 13.36   12.02 K4V 80 0
11 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2912 0
12 V* V816 Tau BY* 03 51 53.3859483764 +24 23 13.077396311   13.67 12.69   11.54 K0V 64 0
13 * eps Per bC* 03 57 51.2320472 +40 00 36.775143 1.71 2.71 2.89 2.96 3.14 B1.5III 494 0
14 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2586 0
15 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1182 1
16 HD 32147 PM* 05 00 48.9991346145 -05 45 13.220341956 8.27 7.27 6.21 5.36 4.87 K3+V 407 1
17 V* RW Aur TT* 05 07 49.538 +30 24 05.07   10.86 9.60 9.95   K1/5e+K5e 696 0
18 HD 36395 PM* 05 31 27.3958475290 -03 40 38.021551815 10.626 9.443 7.968 6.996 5.913 M1.5Ve 418 0
19 V* V1321 Ori Or* 05 35 04.3009468008 -05 08 12.736574621   11.94 10.538   9.117 K0III 89 0
20 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1547 1
21 NGC 2516 OpC 07 58 04 -60 45.2           ~ 576 0
22 HD 88230 Fl* 10 11 22.1400209197 +49 27 15.249158750 9.23 7.94 6.61 5.36 4.56 K6VeFe-1 417 0
23 IC 2602 OpC 10 42 58 -64 24.0           ~ 539 0
24 HD 95735 Fl* 11 03 20.19400 +35 58 11.5682 10.030 8.960 7.520 5.99 4.79 M2+V 611 1
25 V* VW Cha TT* 11 08 01.3974165580 -77 42 28.579297348 13.91 14.04 12.80   10.69 K7+M0 165 0
26 * 61 UMa PM* 11 41 03.0159358291 +34 12 05.882438337 6.31 6.08 5.34 4.73 4.38 G8V 561 0
27 NAME Chamaeleon Region SFR 12 00 -79.0           ~ 168 1
28 * 70 Vir PM* 13 28 25.8081883620 +13 46 43.642951116 5.930 5.680 4.970 4.37 3.98 G4Va 662 1
29 HD 131977 BY* 14 57 28.0008928545 -21 24 55.726897561 7.89 6.83 5.72 4.74 4.19 K4V 443 0
30 NAME Lup Cloud SFR 16 03 -38.1           ~ 482 0
31 Wa Oph 2 TT* 16 11 59.2701883216 -19 06 53.315967884       11.57   K2Ve 56 0
32 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2939 0
33 V* V2131 Oph Or* 16 31 15.7390747430 -24 34 02.512884637   12.0 12.05 11.06 10.13 ~ 91 0
34 IC 4665 OpC 17 46 18 +05 43.0           ~ 307 0
35 NGC 6475 OpC 17 53 51 -34 47.6           ~ 329 0
36 * ome Sgr SB* 19 55 50.3625499909 -26 17 57.693299065   5.45 4.70     G5IV 127 0
37 * b01 Cyg RS* 20 06 21.7674289928 +35 58 20.887464451   6.21   4.8   G8.5IVa 156 0
38 * 31 Vul SB* 20 52 07.6835241741 +27 05 48.995100470   5.399 4.568     G7IIIFe-1 129 0
39 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 930 0
40 * 61 Cyg B Fl* 21 06 55.2640651855 +38 44 31.362140913 8.63 7.40 6.03 4.86 3.55 K7V 659 1
41 * 42 Cap RS* 21 41 32.8593786524 -14 02 51.419701067 6.03 5.83 5.18     G2IV 168 0
42 HD 208527 * 21 56 23.9845774113 +21 14 23.486334463 10.090 8.060 6.370     K5V 54 1
43 BD+29 5007 PM* 23 50 27.8618928401 +30 21 11.729095492 11.79 10.60 9.34 9.155 7.945 K5V 48 0
44 HD 223778 SB* 23 52 25.4066877164 +75 32 40.368591630   7.37   5.8   K3V 126 0

    Equat.    Gal    SGal    Ecl

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2019.11.22-09:50:54

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