2014A&A...570A.118F


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST12:29:42

2014A&A...570A.118F - Astronomy and Astrophysics, volume 570A, 118-118 (2014/10-1)

GW Orionis: Inner disk readjustments in a triple system.

FANG M., SICILIA-AGUILAR A., ROCCATAGLIATA V., FEDELE D., HENNING T., EIROA C. and MUELLER A.

Abstract (from CDS):

Disks are expected to dissipate quickly in binary or multiple systems. Investigating such systems can improve our knowledge of the disk dispersal. The triple system GW Ori, still harboring a massive disk, is an excellent target. We study the young stellar system GW Ori, concentrating on its accretion, wind activity and disk properties. We use high-resolution optical spectra of GW Ori to do spectral classification and derive the radial velocities (RV). We analyze the wind and accretion activity using the emission lines in the spectra. We also use U-band photometry, which has been collected from the literature, to study the accretion variability of GW Ori. We characterize the disk properties of GW Ori by modeling its spectral energy distribution (SED). By comparing our data to the synthetical spectra, we classify GW Ori as a G8 star. Based on the RVs derived from the optical spectra, we confirm the previous result as a close companion in GW Ori with a period of ∼242 days and an orbital semi-major axis of ∼1AU. The RV residuals after the subtraction of the orbital solution with the equivalent widths (EW) of accretion-related emission lines vary with periods of 5-6.7days during short-time intervals, which are caused by the rotational modulation. The Hα and Hβ line profiles of GW Ori can be decomposed in two central-peaked emission components and one blue-shifted absorption component. The blue-shifted absorption components are due to a disk wind modulated by the orbital motion of the close companion. Therefore, the systems like GW Ori can be used to study the extent of disk winds. We find that the accretion rates of GW Ori are rather constant but can occasionally be enhanced by a factor of 2-3. We reproduce the SED of GW Ori by using disk models with gaps ∼25-55AU in size. A small population of tiny dust particles within the gap produces the excess emission at near-infrared bands and the strong and sharp silicate feature at 10µm. The SED of GW Ori exhibits dramatic changes on timescales of ∼20yr in the near-infrared bands, which can be explained as the change in the amount and distribution of small dust grains in the gap. We collect a sample of binary/multiple systems with disks in the literature and find a strong positive correlation between their gap sizes and separations from the primaries to companions, which is generally consistent with the prediction from the theory.

Abstract Copyright:

Journal keyword(s): stars: pre-main sequence - binaries: spectroscopic - stars: individual: GW Orionis - accretion, accretion disks - line: profiles

Simbad objects: 39

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Number of rows : 39

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 EM* LkHA 330 TT* 03 45 48.2804487421 +32 24 11.851014679   12.30 10.97     F7 121 0
2 NAME IRAS 04114+2757G TT* 04 14 30.5533533766 +28 05 14.599582233           M2.2 46 0
3 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 649 1
4 V* IP Tau Or* 04 24 57.0823478325 +27 11 56.543062579   14.50   12.46   M0:Ve 190 0
5 V* DF Tau Or* 04 27 02.7917481241 +25 42 22.456361256 11.97 12.25 11.42 10.31 9.14 M3Ve 459 1
6 V* UX Tau A TT* 04 30 03.9931880444 +18 13 49.476948664   12.92 11.15     K2Ve 327 0
7 V* UX Tau Or* 04 30 03.99626 +18 13 49.4355 11.23 11.84 10.80 9.83 9.05 K2Ve+M1Ve 311 0
8 V* HK Tau Or* 04 31 50.5722969258 +24 24 17.775488652 16.81   15.10     M0.5 295 1
9 V* GG Tau Or* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 647 1
10 V* UZ Tau B TT* 04 32 42.82968 +25 52 31.4148   14.07 12.72 13.35   M1/3Ve 136 0
11 V* GK Tau Or* 04 33 34.5626781676 +24 21 05.854541262 15.50   13.00 12.02 10.62 K7:Ve 271 0
12 V* DM Tau Or* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 510 0
13 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 552 1
14 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3479 0
15 CoKu Tau-Aur Star 4 TT* 04 41 16.8106225314 +28 40 00.077173462   16.40 14.68 14.59   M1.5e 165 0
16 V* DP Tau Or* 04 42 37.6996387891 +25 15 36.992730557 15.84 15.2 13.70 14.42   M0.8 154 1
17 V* DQ Tau Or* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 286 0
18 2MASS J04542368+1709534 TT* 04 54 23.68272 +17 09 53.4744     13.5     M3.4 51 1
19 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 552 0
20 V* GW Ori Or* 05 29 08.3925564419 +11 52 12.653756566   10.83 10.10 9.52   G5/8Ve 299 0
21 Cl Collinder 69 OpC 05 35 06 +09 56.0     2.8     ~ 227 0
22 V* SZ Cha Or* 10 58 16.7496916561 -77 17 17.183339177     12.68   10.62 K0e 103 0
23 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1532 1
24 V* CS Cha Or* 11 02 24.8849252208 -77 33 35.683462615   12.88 11.69   10.123 K2Ve 191 0
25 NAME Cha I MoC 11 06 48 -77 18.0           ~ 968 1
26 Ass Cha T 1-20 Or* 11 08 39.0278260669 -77 16 04.168315197   18.44 16.28 15.822 13.17 K5Ve 76 0
27 V* VY Cha Or* 11 08 54.6053179733 -77 02 13.010307395   14.8     13.60 K8Ve 63 0
28 Ass Cha T 2-54 TT* 11 12 42.6696152636 -77 22 22.928829312     11.103   9.653 G8+K7 79 2
29 HD 98800B SB* 11 22 05.288454 -24 46 39.04974   11.18 9.92     ~ 110 1
30 V* T Cha Or* 11 57 13.5268556629 -79 21 31.521755129   10.00 11.86     K0e 234 1
31 V* DX Cha Ae* 12 00 05.0870448691 -78 11 34.559255151   6.81 6.60     A0_sh 306 0
32 RX J1604.3-2130 * 16 04 21.66 -21 30 28.4       11.8   K2 24 0
33 IRAS 16245-2423 TT* 16 27 37.1911764648 -24 30 35.031583716       16.66 14.67 B5-F2 235 0
34 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
35 V* V2131 Oph Or* 16 31 15.7390747430 -24 34 02.512884637   12.0 12.05 11.06 10.13 ~ 91 0
36 ROXs 43A TT* 16 31 20.1187037852 -24 30 05.059723324   11.89 10.93     G5IVe 47 0
37 2MASS J16335560-2442049 Y*O 16 33 55.6149601033 -24 42 05.006785530           K7 40 0
38 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 235 1
39 HD 319139 BY* 18 14 10.4818974563 -32 47 34.516106830   11.47 10.68   9.11 K5+K7 290 0

    Equat.    Gal    SGal    Ecl

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2020.07.12-12:29:42

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