2017A&A...607A.127S


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.09CEST07:32:04

2017A&A...607A.127S - Astronomy and Astrophysics, volume 607A, 127-127 (2017/11-1)

The 2014-2017 outburst of the young star ASASSN-13db. A time-resolved picture of a very-low-mass star between EXors and FUors.

SICILIA-AGUILAR A., OPRANDI A., FROEBRICH D., FANG M., PRIETO J.L., STANEK K., SCHOLZ A., KOCHANEK C.S., HENNING T., GREDEL R., HOLOIEN T.W.-S., RABUS M., SHAPPEE B.J., BILLINGTON S.J., CAMPBELL-WHITE J. and ZEGMOTT T.J.

Abstract (from CDS):

Context. Accretion outbursts are key elements in star formation. ASASSN-13db is a M5-type star with a protoplanetary disk, the lowest-mass star known to experience accretion outbursts. Since its discovery in 2013, it has experienced two outbursts, the second of which started in November 2014 and lasted until February 2017.
Aims. We explore the photometric and spectroscopic behavior of ASASSN-13db during the 2014-2017 outburst.
Methods. We use high- and low-resolution spectroscopy and time-resolved photometry from the ASAS-SN survey, the LCOGT and the Beacon Observatory to study the light curve of ASASSN-13db and the dynamical and physical properties of the accretion flow.
Results. The 2014-2017 outburst lasted for nearly 800 days. A 4.15d period in the light curve likely corresponds to rotational modulation of a star with hot spot(s). The spectra show multiple emission lines with variable inverse P-Cygni profiles and a highly variable blue-shifted absorption below the continuum. Line ratios from metallic emission lines (Fe I/Fe II, Ti I/Ti II) suggest temperatures of ∼5800-6000K in the accretion flow.
Conclusions. Photometrically and spectroscopically, the 2014-2017 event displays an intermediate behavior between EXors and FUors. The accretion rate ([M]=1-3x10–7M/yr), about two orders of magnitude higher than the accretion rate in quiescence, is not significantly different from the accretion rate observed in 2013. The absorption features in the spectra suggest that the system is viewed at a high angle and drives a powerful, non-axisymmetric wind, maybe related to magnetic reconnection. The properties of ASASSN-13db suggest that temperatures lower than those for solar-type stars are needed for modeling accretion in very-low-mass systems. Finally, the rotational modulation during the outburst reveals that accretion-related structures settle after the beginning of the outburst and can be relatively stable and long-lived. Our work also demonstrates the power of time-resolved photometry and spectroscopy to explore the properties of variable and outbursting stars.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: pre-main sequence - stars: variables: T Tauri, Herbig Ae/Be - stars: individual: ASASSN-13db - stars: low-mass - protoplanetary disks - techniques: spectroscopic - techniques: spectroscopic

VizieR on-line data: <Available at CDS (J/A+A/607/A127): table1.dat>

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 LDN 1615 DNe 05 05.5 -03 26           ~ 13 0
2 LDN 1616 DNe 05 07 00 -03 21.1           ~ 30 0
3 2MASS J05101100-0328262 Y*O 05 10 11.0009704190 -03 28 26.285115571           ~ 3 0
4 ASASSN -13db ev 05 10 11.08 -03 28 26.3           ~ 11 0
5 2MASS J05101478-0330074 TT* 05 10 14.7717490565 -03 30 07.353356510   12.53 11.74 11.29 10.87 G8 10 0
6 V* V1118 Ori Or* 05 34 44.9889538895 -05 33 41.344187987 15.053 15.378 14.430 15.22 12.701 M1e 126 0
7 V* V1467 Ori Or* 05 34 56.2679691997 -06 04 17.395405778   17.39 15.886   13.802 M0.8 19 0
8 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2056 1
9 NGC 1981 OpC 05 35 09 -04 25.9     4.2     ~ 76 0
10 NAME Ori Complex Cld 05 35.3 -05 23           ~ 361 0
11 2MASS J05424706-0817069 Y*O 05 42 47.067 -08 17 06.93           M5 48 0
12 V* FU Ori Or* 05 45 22.3650208559 +09 04 12.296285806   10.72 9.60     F0Iab 734 1
13 V* V1647 Ori Or* 05 46 13.1370923766 -00 06 04.876812846     18.1     ~ 239 1
14 NAME McNeil Nebula RNe 05 46 14 -00 05.8           ~ 72 2
15 CD-35 10525 Or* 15 49 12.1055573607 -35 39 05.053991067 12.19 12.76 11.66 11.15   K7Ve 256 0
16 HD 325367 Or* 16 03 05.4914377137 -40 18 25.426543472   11.40 8.50     M0 294 0
17 V* S CrA Or* 19 01 08.597088 -36 57 19.89504   11.76 10.91 11.41   G0Ve+K0Ve 262 0

    Equat.    Gal    SGal    Ecl

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2021.05.09-07:32:04

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