2011A&A...527A.133K


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.16CET11:27:51

2011A&A...527A.133K - Astronomy and Astrophysics, volume 527A, 133-133 (2011/3-1)

The outburst and nature of two young eruptive stars in the North America/Pelican Nebula Complex.

KOSPAL A., ABRAHAM P., ACOSTA-PULIDO J.A., AREVALO MORALES M.J., CARNERERO M.I., ELEK E., KELEMEN J., KUN M., PAL A., SZAKATS R. and VIDA K.

Abstract (from CDS):

The sudden optical brightening of two young stellar objects, HBC722 and VSXJ205126.1+440523, located in the North America/Pelican Nebula Complex, was announced in August 2010. Early photometric and spectroscopic observations of these objects indicated that they may belong to the FUor or EXor class of young eruptive stars. The eruptions of FUors and EXors are often explained by enhanced accretion of material from the circumstellar disk to the protostar. In order to determine the true nature of these two objects, we started an optical and near-infrared monitoring program, and complemented our data with archival observations and data from the literature. We plot and analyze pre-outburst and outburst spectral energy distributions (SEDs), multi-filter light curves, and color-color diagrams. The quiescent SED of HBC722 is consistent with that of a slightly reddened normal TTauri-type star. The source brightened monotonically in about two months, and the SED obtained during maximum brightness indicates the appearance of a hot, single-temperature blackbody. The current fading rate implies that the star will return to quiescence in about a year, which questions its classification as a bone fide FUor. The quiescent SED of VSXJ205126.1+440523 looks like that of a highly embedded Class I source. The outburst of this source happened more gradually, but reached an unprecedentedly high amplitude. Its light curves showed a deep minimum two and a half months after the peak, when the object was close to its pre-outburst optical brightness. Further monitoring indicates that it is still far from being quiescent. The shape of the light curves as well as the bolometric luminosities and accretion rates suggest that these objects do not fit into the classic FUor group. Although HBC722 exhibits all spectral characteristics of a bona fide FUor, its luminosity and accretion rate is too low and its timescale is too fast compared with classical FUors. VSXJ205126.1+440523 seems to be an example where quick extinction changes modulate the light curve.

Abstract Copyright:

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

Simbad objects: 19

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Number of rows : 19

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 Dark Cloud SFR 04 41.0 +25 52           ~ 3338 0
2 V* DR Tau TT* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 462 0
3 V* FU Ori FU* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 690 1
4 V* V1647 Ori FU* 05 46 13.1370923766 -00 06 04.876812846     18.1     ~ 221 1
5 HD 325367 TT* 16 03 05.4914377137 -40 18 25.426543472   11.40 8.50     M0 270 0
6 NGC 6823 OpC 19 43 09 +23 18.0   7.71 7.1     ~ 247 2
7 V* V1515 Cyg FU* 20 23 48.0159810586 +42 12 25.780858811   13.470 12.530 11.210   G0/G2Ib 206 0
8 HH 569 HH 20 50 29.5 +44 02 40           ~ 6 0
9 IC 5070 HII 20 51.0 +44 22           ~ 172 1
10 UCAC2 46962009 * 20 51 02.9495285936 +44 09 27.704074821     14.684 13.856 13.198 ~ 1 0
11 V* V1598 Cyg Fl* 20 51 03.9205607490 +44 11 40.671143880   15.0       ~ 5 0
12 UCAC2 46962024 * 20 51 11.9453805723 +44 07 21.373408011     14.268 12.400 10.968 ~ 1 0
13 UCAC2 46962032 * 20 51 17.6968286058 +44 02 41.191800836     14.981 14.146 13.307 ~ 1 0
14 V* V2492 Cyg Or* 20 51 26.2368444519 +44 05 23.866104173   20.2   18.3   F-GII/MI 62 0
15 2MASS J20513057+4403449 Y*O 20 51 30.578 +44 03 44.92     15.924 14.864 14.236 ~ 3 0
16 UCAC2 46962071 * 20 51 41.4330473110 +44 03 03.262078483     15.300 14.790 13.816 ~ 1 0
17 V* V2493 Cyg FU* 20 58 17.0282353931 +43 53 43.339695195   19.678 18.023 17.67 15.233 K0-M7 87 0
18 NGC 7000 HII 20 58 47 +44 19.8           ~ 357 1
19 EM* LkHA 190 FU* 20 58 53.7336698326 +44 15 28.384667940     15.6     F7/G3I/IIe 467 0

    Equat.    Gal    SGal    Ecl

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2019.12.16-11:27:51

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