2011A&A...534A..33R


Query : 2011A&A...534A..33R

2011A&A...534A..33R - Astronomy and Astrophysics, volume 534A, 33-33 (2011/10-1)

Multi-wavelength observations of the young binary system Haro 6-10: the case of misaligned discs.

ROCCATAGLIATA V., RATZKA T., HENNING T., WOLF S., LEINERT C. and BOUWMAN J.

Abstract (from CDS):

We present a multi-wavelength, high-resolution observational survey of the young binary system Haro 6-10 (GV Tau, IRAS 04263+2426), which harbours one of the few known infrared companions. The primary goal of this project is to determine the physical and geometrical properties of the circumstellar and circumbinary material in the Haro 6-10 system. High-resolution optical (HST/WFPC2) and near-infrared (VLT/NACO) images in different bands were analysed to investigate the large-scale structures of the material around the binary. Mid-infrared interferometry (VLTI/MIDI) and spectroscopy (TIMMI2 at the 3.6m ESO telescope) were carried out to determine the structure and optical depth of the circumstellar material around the individual components. The multi-wavelength observations suggest that both components of the binary system Haro 6-10 are embedded in a common envelope. The measured extinction indicates a dust composition of the envelope similar to that of the interstellar medium. Each component of the system has a circumstellar disc-like structure typical of young stars. The discs are highly misaligned: the northern component is seen almost edge-on and the southern component is an almost face-on disc. The two main formation scenarios of binary systems with misaligned discs are the gravitational capture of a passing object in a dense environment and the fragmentation of the collapsing molecular cloud. Given the low-density environment of the Taurus-Aurigae star-forming region, the first scenario is unlikely for Haro 6-10. The binary system most probably formed via fragmentation of two different parts of the collapsing molecular cloud combined with other dynamical processes related to the cloud and/or the protostars. This can also be the explanation for other binary systems with an infrared companion.

Abstract Copyright:

Journal keyword(s): binaries: general - stars: formation - protoplanetary disks - stars: individual: Haro 6-10

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 * 37 Tau PM* 04 04 41.7128811713 +22 04 54.946823724 6.41 5.44 4.37 3.58 3.05 K0III-IIIb 183 0
2 V* T Tau TT* 04 21 59.4319873992 +19 32 06.432393336   11.22 10.12 9.80   K0IV/Ve 1402 1
3 LDN 1524 DNe 04 27 57.7 +24 39 18           ~ 83 0
4 V* GV Tau TT* 04 29 23.7314759229 +24 33 00.216016292 19.20         K7 283 0
5 V* GV Tau A * 04 29 23.7322948921 +24 33 00.241218221           ~ 35 0
6 V* GV Tau B * 04 29 23.7603742259 +24 32 59.248875580           ~ 31 0
7 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1353 0
8 * alf Tau LP? 04 35 55.23907 +16 30 33.4885 4.32 2.40 0.86 -0.37 -1.31 K5+III 1251 2
9 * eta02 Pic PM* 05 04 58.0142014896 -49 34 40.202725008 8.35 6.47 5.01 3.81 2.90 K5III 50 0
10 * eps Lep PM* 05 05 27.6644072506 -22 22 15.724153311 6.41 4.64 3.18 2.08 1.27 K4III 156 0
11 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2311 0
12 * phi02 Ori PM* 05 36 54.3885728561 +09 17 26.416510827 5.70 5.04 4.09 3.33 2.78 G9.5IIIbFe-2.5 359 0
13 * 17 Mon * 06 47 19.8301708488 +08 02 14.122870224 7.82 6.17 4.77 3.74 3.04 K4III 118 0
14 * tet CMa PM* 06 54 11.3988612864 -12 02 19.061163780 7.20 5.51 4.08 2.95 2.17 K3/4III 218 0
15 * u Car PM* 10 53 29.6561115087 -58 51 11.413331344 5.39 4.74 3.79 3.07 2.57 K0IV 95 0
16 * tet Cen PM* 14 06 40.94752 -36 22 11.8371 3.94 3.04 2.05 1.29 0.76 K0-IIIb 252 1

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