2010A&A...511A..63A


Query : 2010A&A...511A..63A

2010A&A...511A..63A - Astronomy and Astrophysics, volume 511, A63-63 (2010/2-2)

A multi-wavelength study of the young star V1118 Orionis in outburst.

AUDARD M., STRINGFELLOW G.S., GUEDEL M., SKINNER S.L., WALTER F.M., GUINAN E.F., HAMILTON R.T., BRIGGS K.R. and BALDOVIN-SAAVEDRA C.

Abstract (from CDS):

The accretion history of low-mass young stars is not smooth but shows spikes of accretion that can last from months and years to decades and centuries. Observations of young stars in outbursts can help us understand the temporal evolution of accreting stars and the interplay between the accretion disk and the stellar magnetosphere. The young late-type star V1118 Orionis was in outburst from 2005 to 2006. We followed the outburst with optical and near-infrared photometry. The X-ray emission was further probed with observations taken with XMM-Newton and Chandra during and after the outburst. In addition, we obtained mid-infrared photometry and spectroscopy with Spitzer at the peak of the outburst and in the post-outburst phase. The spectral energy distribution of V1118 Ori varied significantly over the course of the outburst. The optical flux showed the largest variations, most likely caused by enhanced emission by a hot spot. The hot spot dominated the optical and near-infrared emission at the peak of the outburst, while the disk emission dominated in the mid-infrared. The emission silicate feature in V1118 Ori is flat and does not vary in shape, but was slightly brighter at the peak of the outburst compared to the post-outburst spectrum. The X-ray flux correlated with the optical and infrared fluxes, indicating that accretion affected the magnetically active corona and the stellar magnetosphere. The thermal structure of the corona was variable with some indication of a cooling of the coronal temperature in the early phase of the outburst with a gradual return to normal values. Color-color diagrams in the optical and infrared showed variations during the outburst, with no obvious signature of reddening caused by circumstellar matter. Using Monte-Carlo realizations of star+disk+hotspot models to fit the spectral energy distributions in ``quiescence'' and at the peak of the outburst, we determined that the mass accretion rate varied from about 2.5x10–7M/yr to 1.0x10–6M/yr; in addition, the fractional area of the hotspot increased significantly. The multi-wavelength study of the V1118 Ori outburst helped us to understand the variations in spectral energy distributions and demonstrated the interplay between the disk and the stellar magnetosphere in a young, strongly accreting star.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - infrared: stars - circumstellar matter - stars: coronae - stars: pre-main-sequence - X-rays: stars

VizieR on-line data: <Available at CDS (J/A+A/511/A63): tablea2.dat tablea3.dat>

Simbad objects: 24

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Number of rows : 24
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* V1213 Tau Or* 04 31 37.5055489536 +18 12 24.383952396           K7 546 0
2 LDN 1415 DNe 04 42.0 +54 26           ~ 13 0
3 V* V1981 Ori Or* 05 34 33.9561432288 -05 34 51.317206644 18.577 17.117 15.931 14.74 13.205 K8 35 0
4 Brun 311 Y*O 05 34 35.1487847520 -05 32 10.400448912 15.141 14.151 13.301 12.46 11.467 K2IV 35 0
5 2MASS J05343568-0535520 TT* 05 34 35.6800236096 -05 35 52.181756484 20.203 18.561 17.415 16.16 14.462 M2.8e 23 0
6 V* V759 Ori TT* 05 34 36.5416312824 -05 36 17.127425232 18.203 16.644 15.520 14.32 12.693 M1.0e 41 0
7 V* IV Ori Or* 05 34 37.4650405320 -05 34 51.950558388 17.088 16.413 15.455 13.97 13.264 K2-K5e 45 0
8 DENIS J053441.6-053425 * 05 34 41.5873856352 -05 34 24.974250888   20.951 19.683   16.33 M4 12 0
9 V* V2011 Ori Or* 05 34 42.1941491496 -05 33 03.605277132   20.871 19.865   15.830 M3.0e 16 0
10 V* V1175 Ori Or* 05 34 44.3785382712 -05 32 18.666315960 18.093 16.426 15.327 14.19 13.075 M1 25 0
11 V* V1118 Ori Or* 05 34 44.9889538895 -05 33 41.344187987 15.053 15.378 14.430 15.22 12.701 M1e 134 0
12 Parenago 1606 TT* 05 34 46.9222394616 -05 35 07.881243432 18.790 16.995 15.764 14.38 12.859 M1.5 30 0
13 HD 36917 Or* 05 34 46.9822530528 -05 34 14.583314568   8.13 8.03     B9III/IV 145 0
14 V* V2034 Ori Or* 05 34 47.9130343872 -05 35 43.885615596   21.323 19.860 17.76 15.113 M4.5 29 0
15 2MASS J05344828-0532351 Y*O 05 34 48.2840776632 -05 32 35.105174340   20.539 19.260 17.37 14.762 M2.5 30 0
16 2MASS J05344881-0533330 TT* 05 34 48.8195453928 -05 33 33.059127996   19.812 18.608 17.09 14.977 M2.5 31 0
17 BD-05 1307 Em* 05 34 52.2399438744 -05 33 08.495625096   11.29 10.19 9.78 9.25 K2III-IV 27 0
18 M 42 HII 05 35 01.5 -05 26 24           ~ 3953 0
19 V* FU Ori Or* 05 45 22.3647842544 +09 04 12.291320064   10.72 9.60     F0Iab 770 1
20 V* V1647 Ori Or* 05 46 13.1370578472 -00 06 04.885093296     18.1     ~ 260 1
21 V* Z CMa Ae* 07 03 43.1599411656 -11 33 06.209065836 10.51 9.99 8.80     B5/8eq+F5/7 557 3
22 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1774 1
23 HD 325367 Or* 16 03 05.4915085848 -40 18 25.426727676   11.40 8.50     M0 316 0
24 V* V1735 Cyg Or* 21 47 20.6628414360 +47 32 03.857457372           ~ 155 0

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2022.12.07-04:36:18

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