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


Query : 2014A&A...570A.118F

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 - 2024
#notes
1 EM* LkHA 330 TT* 03 45 48.2805122064 +32 24 11.850978276   12.30 10.97     F7 142 0
2 NAME IRAS 04114+2757G TT* 04 14 30.5508810936 +28 05 14.596567332           M2.2 57 0
3 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 704 1
4 V* IP Tau Or* 04 24 57.0824018640 +27 11 56.539953888   14.50   12.46   M0:Ve 232 0
5 V* DF Tau TT* 04 27 02.7932020080 +25 42 22.453341516 11.97 12.25 11.42 10.31 9.14 M3Ve 500 1
6 V* UX Tau A TT* 04 30 03.9932216088 +18 13 49.469925504   12.92 11.15     K2Ve 356 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 355 0
8 V* HK Tau TT* 04 31 50.5715875272 +24 24 17.775307548 16.81 16.689 15.292     M0.5 340 1
9 V* GG Tau Or* 04 32 30.3506925552 +17 31 40.494063144 14.84 14.78 13.40 11.54   M0e+M2.0e 737 1
10 V* UZ Tau B TT* 04 32 42.8118779016 +25 52 31.198173600   14.07 12.72 13.35   M1/3Ve 150 0
11 V* GK Tau Or* 04 33 34.5630097872 +24 21 05.855136732 15.50   13.00 12.02 10.62 K7:Ve 308 0
12 V* DM Tau Or* 04 33 48.7336763736 +18 10 09.973460280 14.30 14.82 14.00     M2Ve 635 0
13 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 691 1
14 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4429 0
15 CoKu Tau-Aur Star 4 TT* 04 41 16.8104181312 +28 40 00.073831728   16.40 14.68 14.59   M1.5e 181 0
16 V* DP Tau Or* 04 42 37.6989071232 +25 15 36.983641716 15.84 15.2 13.70 14.42   M0.8 172 1
17 V* DQ Tau Or* 04 46 53.0575226016 +17 00 00.136127304 14.56 13.67 12.00 13.21   M1Ve 339 0
18 2MASS J04542368+1709534 TT* 04 54 23.6741496384 +17 09 53.495824464     13.5     M3.4 59 1
19 V* GM Aur Or* 04 55 10.9815576936 +30 21 59.373771876 14.59 13.351 12.242 11.798   K3Ve 690 0
20 V* GW Ori Or* 05 29 08.3928710640 +11 52 12.666457092   10.83 10.10 9.52   G5/8Ve 351 0
21 Cl Collinder 69 OpC 05 35 10.1 +09 48 47     2.8     ~ 313 0
22 V* SZ Cha Or* 10 58 16.7500775160 -77 17 17.185749900     12.68   10.62 K0e 124 0
23 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1898 1
24 V* CS Cha Or* 11 02 24.8763629208 -77 33 35.667131796   12.88 11.69   10.123 K2Ve 230 0
25 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1154 1
26 Ass Cha T 1-20 Or* 11 08 39.0261275112 -77 16 04.163889324   18.44 16.28 15.822 13.17 K5Ve 88 0
27 V* VY Cha Or* 11 08 54.6059374368 -77 02 13.006464720   14.8     13.60 K8Ve 75 0
28 Ass Cha T 2-54 TT* 11 12 42.6709132056 -77 22 22.943489160     11.103   9.653 G8+K7 92 2
29 HD 98800B SB* 11 22 05.2890267409 -24 46 38.767455498   11.18 9.92     ~ 131 1
30 V* T Cha Or* 11 57 13.5245085552 -79 21 31.530508884   10.00 11.86     K0e 272 1
31 V* DX Cha Ae* 12 00 05.0868602544 -78 11 34.565724312   6.81 6.60     A4V 344 0
32 RX J1604.3-2130 X 16 04.3 -21 30           ~ 34 0
33 IRAS 16245-2423 TT* 16 27 37.1906433768 -24 30 35.025246828       16.66 14.67 B5-F2 308 0
34 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3636 1
35 V* V2131 Oph Or* 16 31 15.7445171496 -24 34 02.161097472   12.0 12.05 11.06 10.13 ~ 96 0
36 ROXs 43A TT* 16 31 20.1191847456 -24 30 05.057116128   11.89 10.93     G5IVe 48 0
37 2MASS J16335560-2442049 Y*O 16 33 55.6148566800 -24 42 05.002391016           K7 51 0
38 V* AK Sco Ae* 16 54 44.8491575376 -36 53 18.566586456 9.80 9.63 9.00     F5V 274 1
39 HD 319139 SB* 18 14 10.4818675368 -32 47 34.516836060   11.47 10.68   9.11 K5+K7 359 0

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