2012A&A...540A..46D


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.15CET12:25:43

2012A&A...540A..46D - Astronomy and Astrophysics, volume 540A, 46-46 (2012/4-1)

Protoplanetary disks of T Tauri binary systems in the Orion Nebula Cluster.

DAEMGEN S., CORREIA S. and PETR-GOTZENS M.G.

Abstract (from CDS):

We present a study of protoplanetary disks in spatially resolved low-mass binary stars in the well-known Orion nebula cluster (ONC) to assess the impact of binarity on the properties of circumstellar disks. This is currently the largest such study in a clustered high-stellar-density star-forming environment, as opposed to previous studies, which have mostly been focussed on the young, low-stellar-density Taurus association. We particularly aim to determine the presence of magnetospheric accretion and dust disks for each binary component, and measure the overall disk frequency. We carried out spatially resolved adaptive-optics-assisted observations to acquire near-infrared photometry and spectroscopy of 26 binaries in the ONC, and determine stellar parameters such as effective temperatures, spectral types, luminosities, and masses, as well as accretion properties and near-infrared excesses for the individual binary components. On the basis of our medium resolution K-band spectroscopy, we infer the presence of magnetospheric accretion around each binary component by measuring the strength of the Brackett-γ emission. The accretion disk frequency among the ONC binaries is then estimated from Bayesian statistics. The observed disk signatures, measured accretion luminosities, and mass accretion rates are investigated with respect to the binary separation, mass ratios, and distance to the center of the ONC. A fraction of 40+10–9% of the binary components in the sample can be inferred to be TTauri stars possessing an accretion disk. This is only marginally smaller than the disk fraction of single stars of ∼50% in the ONC. We find that disks in wide binaries of >200AU separation are consistent with random pairing, while the evolution of circumprimary and circumsecondary disks is observed to be synchronized in close binaries (separations <200AU). Circumbinary disks appear to be unsuitable to explain this difference. Furthermore, we identify several mixed pairs of accreting and non-accreting components, suggesting that these systems are common and that there is no preference for either the more or less massive component to evolve faster. The derived accretion luminosities and mass accretion rates of the ONC binary components are of similar magnitude as those for both ONC single stars and binaries in the Taurus star-forming region. The paper concludes with a discussion of the (presumably weak) connection between the presence of inner accretion disks in young binary systems and the existence of planets in stellar multiples.

Abstract Copyright:

Journal keyword(s): binaries: visual - stars: late-type - stars: pre-main sequence

Simbad objects: 50

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Number of rows : 50

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 V* V892 Tau Ae* 04 18 40.6120892867 +28 19 15.641672501   16.6 14.69 14.35   A0Ve 256 1
2 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1182 1
3 V* GG Tau TT* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 630 1
4 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3322 0
5 V* V1441 Ori Or* 05 34 42.9558173865 -05 20 07.004154858 17.571 16.010 14.928   12.524 K7+M3 42 0
6 V* V1458 Ori Or* 05 34 52.1751161466 -05 22 31.910573803 18.427 16.614 15.387   12.371 M0+M0 39 0
7 V* KQ Ori B * 05 34 57.7441363194 -05 23 51.542647669   16.358 15.197   12.589 ~ 36 0
8 V* KQ Ori Or* 05 34 57.772536 -05 23 52.44432   15.13 13.49 13.05   K7+M0 41 0
9 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1907 1
10 V* V405 Ori Or* 05 35 03.5690151032 -05 29 26.042362731 18.273 17.369 16.268 15.03 13.422 M3 31 0
11 V* V2149 Ori Or* 05 35 05.2109864551 -05 14 50.369040502 13.260 12.141 11.246   9.280 G0+F7 48 0
12 [BOM2000] d124-132 Y*O 05 35 12.40103 -05 21 31.6488     22.00     ~ 15 0
13 [AD95] 2380 pr* 05 35 12.5633768444 -05 16 33.280018351         18.154 ~ 14 0
14 V* V2228 Ori Or* 05 35 12.8165402678 -05 20 43.581977465 16.895 16.413 15.458   12.848 M1e 45 1
15 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 1945 1
16 MAX 66 * 05 35 14.8800 -05 23 05.100           K4 13 0
17 V* V2279 Ori Or* 05 35 15.9338 -05 23 50.056 14.794 13.648 12.730   10.537 M0.5+M2 84 0
18 TCC 55 Y*O 05 35 16.0785 -05 22 54.123           M3 18 0
19 * tet01 Ori C ** 05 35 16.46375 -05 23 22.8486 4.20 5.15 5.13 4.91 4.73 O7Vp 1256 1
20 [FRM2016] 306 Y*O 05 35 16.4933279950 -05 22 35.154361064     17.77   14.600 M4 31 0
21 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1433 1
22 V* V1510 Ori Or* 05 35 17.5577527626 -05 22 56.723187707   15.991 15.003   12.239 K7+M1 39 0
23 [AD95] 1468 pr* 05 35 17.5818380905 -05 16 12.866376741         18.456 M4 8 0
24 JW 558 Y*O 05 35 17.65 -05 23 40.5 16.251 15.348 15.343   14.390 M5.9e 66 0
25 JW 566 pr* 05 35 17.990 -05 16 13.63   14.9 18.7   15.757 K7+M1.5 29 0
26 NAME Ori Complex Cld 05 35.3 -05 23           ~ 317 0
27 V* V2336 Ori Or* 05 35 18.7046195630 -05 22 56.847269340     15.466   12.640 K5+M2 38 0
28 V* V1520 Ori Or* 05 35 20.454 -05 23 29.77   17.572 15.912   12.924 M0+M3.5 44 0
29 V* V1524 Ori Or* 05 35 21.35 -05 23 45.4   17.621 16.471   13.850 M1+M3.5 17 1
30 V* V2380 Ori Or* 05 35 21.6830858370 -05 21 47.000248996   13.7 18.089   14.591 M2.5+M2 31 0
31 Parenago 1994 Y*O 05 35 22.1987557574 -05 26 37.479691890   16.512 15.388 14.09 12.807 M0.5 32 0
32 * tet02 Ori A SB* 05 35 22.9022511214 -05 24 57.817182421 5.37 6.30 6.39 6.30 6.35 O9.5IVp 487 0
33 [HC2000] 754 * 05 35 23.062 -05 24 59.57           M2+M7 12 0
34 V* V1344 Ori BY* 05 35 25.2376374502 -05 09 27.716127013   13.5 15.86   13.080 M3-3.5 31 0
35 V* V2499 Ori Or* 05 35 31.2647679226 -05 18 56.002923274 15.924 15.314 14.344   12.076 K8Ve 53 0
36 V* V360 Ori TT* 05 35 31.953 -05 09 27.96   13.79 12.3   10.66 M0.5+M1.5 63 0
37 V* AN Ori Or* 05 35 41.968248 -05 28 12.79200 13.240 12.297 11.580 11.13 10.199 K3+K3 69 0
38 2MASS J05354416-0536397 pr* 05 35 44.1606683853 -05 36 39.716872798   19.597 18.328   14.111 M6 24 0
39 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 812 1
40 NAME Cha I MoC 11 06 48 -77 18.0           ~ 940 1
41 V* DP Leo AM* 11 17 15.9238061197 +17 57 41.680410866           ~ 206 1
42 BD-07 3477 HS* 12 44 20.2386520980 -08 40 16.848587212   10.46 10.594 10.895   sdB2VIIHe3 242 1
43 V* QS Vir WD* 13 49 52.0031855330 -13 13 37.001934702 14.27 14.98 14.40 14.37   DA3+dM 118 1
44 V* NN Ser No* 15 52 56.1202658103 +12 54 44.432043501   16.0 16.51     DAO1+M4 218 2
45 PSR B1620-26 Psr 16 23 38.2218 -26 31 53.769     21.30     ~ 263 2
46 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2938 0
47 NAME CrA Complex reg 19 15 00.0 -37 30 00           ~ 101 1
48 Kepler-16 Al* 19 16 18.1759181246 +51 45 26.777781114   12.1   11.90   K7V 186 1
49 V* HU Aqr AM* 21 07 58.1945403160 -05 17 40.557984218   15.1   15.4   D+M4V 250 1
50 HD 202206 PM* 21 14 57.7684954746 -20 47 21.162361638   8.79 8.07     G6V 192 1

    Equat.    Gal    SGal    Ecl

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2019.11.15-12:25:43

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