2016A&A...596A..52K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.09CEST06:52:10

2016A&A...596A..52K - Astronomy and Astrophysics, volume 596A, 52-52 (2016/12-1)

Multiwavelength study of the low-luminosity outbursting young star HBC 722.

KOSPAL A., ABRAHAM P., ACOSTA-PULIDO J.A., DUNHAM M.M., GARCIA-ALVAREZ D., HOGERHEIJDE M.R., KUN M., MOOR A., FARKAS A., HAJDU G., HODOSAN G., KOVACS T., KRISKOVICS L., MARTON G., MOLNAR L., PAL A., SARNECZKY K., SODOR A., SZAKATS R., SZALAI T., SZEGEDI-ELEK E., SZING A., TOTH I., VIDA K. and VINKO J.

Abstract (from CDS):

Context. HBC 722 (V2493 Cyg) is a young eruptive star in outburst since 2010. Spectroscopic evidence suggests that the source is an FU Orionis-type object, with an atypically low outburst luminosity.
Aims. Because it was well characterized in the pre-outburst phase, HBC 722 is one of the few FUors from which we can learn about the physical changes and processes associated with the eruption, including the role of the circumstellar environment.
Methods. We monitored the source in the BVRIJHKS bands from the ground and at 3.6 and 4.5µm from space with the Spitzer Space Telescope. We analyzed the light curves and studied the evolving spectral energy distribution by fitting a series of steady accretion disk models at many epochs covering the outburst. We also analyzed the spectral properties of the source based on our new optical and infrared spectra, comparing our line inventory with those published in the literature for other epochs. We also mapped HBC 722 and its surroundings at millimeter wavelengths.
Results. From the light-curve analysis we conclude that the first peak of the outburst in 2010 September was mainly due to an abrupt increase in the accretion rate in the innermost part of the system. This was followed after a few months by a long-term process, when the brightening of the source was mainly due to a gradual increase in the accretion rate and the emitting area. Our new observations show that the source is currently in a constant plateau phase. We found that the optical spectrum was similar in the first peak and following periods, but around the peak the continuum was bluer and the Hα profile changed significantly between 2012 and 2013. The source was not detected in the millimeter continuum, but we discovered a flattened molecular gas structure with a diameter of 1700 au and mass of 0.3M centered on HBC 722.
Conclusions. While the first brightness peak might be interpreted as a rapid fall of piled-up material from the inner disk onto the star, the later monotonic flux rise suggests the outward expansion of a hot component according to a previously described theory. Our study of HBC 722 demonstrates that accretion-related outbursts can occur in young stellar objects even with very low-mass disks in the late Class II phase.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: formation - circumstellar matter - infrared: stars - stars: individual: HBC 722

Simbad objects: 20

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Number of rows : 20

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 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
2 V* FU Ori Or* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 708 1
3 V* V1647 Ori Or* 05 46 13.1370923766 -00 06 04.876812846     18.1     ~ 231 1
4 V* V960 Mon Or* 06 59 31.5890184824 -04 05 27.764626541   16.11 14.94 13.92 12.67 ~ 25 1
5 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2702 2
6 QSO J2015+371 BLL 20 15 28.72976962 +37 10 59.5148505     21.82 21.4   ~ 243 2
7 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 707 0
8 [DAB2012] MMS6 mm 20 58 15.62 +43 53 18.1           ~ 3 0
9 [DAB2012] MMS5 mm 20 58 16.01 +43 53 22.8           ~ 3 0
10 [DAB2012] MMS4 mm 20 58 16.32 +43 53 25.5           ~ 4 0
11 [DAB2012] MMS1 mm 20 58 16.52 +43 53 53.7           ~ 5 0
12 [DAB2012] MMS2 mm 20 58 16.78 +43 53 36.0           ~ 5 0
13 V* V2493 Cyg Or* 20 58 17.0282353931 +43 53 43.339695195   19.678 18.023 17.67 15.233 K7/M0e 89 0
14 [DAB2012] MMS7 mm 20 58 17.06 +43 53 15.0           ~ 3 0
15 HH 655 HH 20 58 17.1 +43 53 47           ~ 2 0
16 [DAB2012] MMS3 mm 20 58 17.70 +43 53 29.2           ~ 4 0
17 EM* LkHA 188 Or* 20 58 23.8104754955 +43 53 11.391445275     14.65 13.69 13.37 K0e 46 0
18 EM* LkHA 190 Or* 20 58 53.7336698326 +44 15 28.384667940   14.26 12.33 12.13   F7/G3I/IIe 476 0
19 HD 200241 * 21 00 44.5549370599 +44 47 07.323675449   9.24 8.52     G2 7 0
20 NVSS J212031+443433 Rad 21 20 31.77356155 +44 34 34.2605485           ~ 11 1

    Equat.    Gal    SGal    Ecl

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2020.07.09-06:52:10

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