2016MNRAS.456..156G


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.19CEST18:23:10

2016MNRAS.456..156G - Mon. Not. R. Astron. Soc., 456, 156-170 (2016/February-2)

Investigating the origin and spectroscopic variability of the near-infrared HI lines in the Herbig star VV Ser.

GARCIA LOPEZ R., KUROSAWA R., CARATTI O GARATTI A., KREPLIN A., WEIGELT G., TAMBOVTSEVA L.V., GRININ V.P. and RAY T.P.

Abstract (from CDS):

The origin of the near-infrared (NIR) HI emission lines in young stellar objects are not yet understood. To probe it, we present multi-epoch LBT-LUCIFER spectroscopic observations of the Paδ, Paβ, and Brγ lines observed in the Herbig star VV Ser, along with Very Large Telescope Interferometer-AMBER Brγ spectro-interferometric observations at medium resolution. Our spectroscopic observations show line profile variability in all the HI lines. The strongest variability is observed in the redshifted part of the line profiles. The Brγ spectro-interferometric observations indicate that the Brγ line emitting region is smaller than the continuum emitting region. To interpret our results, we employed radiative transfer models with three different flow configurations: magnetospheric accretion, a magnetocentrifugally driven disc wind, and a schematic bipolar outflow. Our models suggest that the HI line emission in VV Ser is dominated by the contribution of an extended wind, perhaps a bipolar outflow. Although the exact physical process for producing such outflow is not known, this model is capable of reproducing the averaged single-peaked line profiles of the HI lines. Additionally, the observed visibilities, differential and closure phases are best reproduced when a wind is considered. Nevertheless, the complex line profiles and variability could be explained by changes in the relative contribution of the magnetosphere and/or winds to the line emission. This might indicate that the NIR HI lines are formed in a complex inner disc region where inflow and outflow components might coexist. Furthermore, the contribution of each of these mechanisms to the line appears time variable, suggesting a non-steady accretion/ejection flow.

Abstract Copyright: © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2015)

Journal keyword(s): techniques: interferometric - circumstellar matter - stars: protostars - stars: variables: T Tauri, Herbig Ae/Be - stars: winds, outflows - infrared: stars

Simbad objects: 9

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Number of rows : 9

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 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 652 1
2 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 635 0
3 V* UX Ori Ae* 05 04 29.9881676817 -03 47 14.288047238 10.25 10.93 8.70 9.62 9.43 A4IVe 334 1
4 V* RY Lup Or* 15 59 28.3852522995 -40 21 51.255321659   12.62 9.90     G8/K1IV-V 170 0
5 HD 163272 PM* 17 56 24.4330995581 -26 46 24.211517980   7.99 7.39     G2/3V 41 0
6 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 229 0
7 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 926 2
8 * 61 Ser * 18 31 56.9934603664 -01 00 10.708368257   6.080 5.936     A5IV/V 32 0
9 EM* LkHA 120 Or* 21 01 09.2068364908 +50 21 44.803310926 13.37 13.09 11.99 11.75   F0/F4-G5 187 1

    Equat.    Gal    SGal    Ecl

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2020.10.19-18:23:10

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