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Resolving the origin of hydrogen-line emission in YSOs with near-infrared interferometry

Published online by Cambridge University Press:  13 January 2020

Alexander Kreplin Open the ORCID record for Alexander Kreplin [Opens in a new window] ,
Edward Hone ,
Larisa Tambovtseva ,
Karl-Heinz Hofmann  and
Stefan Kraus
Alexander Kreplin
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, Exeter EX4 4QL, UK email: [email protected],
Edward Hone
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, Exeter EX4 4QL, UK email: [email protected],
Larisa Tambovtseva
Affiliation:
Pulkovo Observatory of RAS, Pulkovskoe Shosse 65, St Petersburg 196140, Russia
Karl-Heinz Hofmann
Affiliation:
Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Stefan Kraus
Affiliation:
Department of Physics and Astronomy, University of Exeter, Stocker Road, Exeter EX4 4QL, UK email: [email protected],
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Abstract

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The origin of the Brγ-line emission in Herbig Ae/Be stars is still an open question and might be related e.g., to a disc wind or the stellar magnetosphere. The study of the continuum and Brγ-emitting region of Herbig Ae/Be stars with high-spectral and high-spatial resolution gives great insights into the sub-au scale hydrogen gas distribution.

We observed the Herbig Be star MWC 120 with the VLTI/AMBER instrument in different spectral channels across the Brγ line with a spectral resolution of R~1500. Using radiative transfer modeling we found a radius of the line emitting region of ~0.4 au that is only two times smaller than the K-band continuum region. This is consistent with a disc wind scenario rather than an origin of magnetospheric emission.

We present near-infrared AMBER (R~12000) observations of the Herbig B[e] star MWC297 in the Brγ-line. We found that the near-infrared continuum emission is ~3.6 times more compact than the expected dust-sublimation radius, possibly indicating the presence of highly refractory dust grains or optically thick gas emission in the inner disk. Our velocity-resolved channel maps marking the first time that kinematic effects in the sub-AU inner regions of a protoplanetary disk could be directly imaged.

Keywords

stars: individual (MWC 120MWC 297)pre–main-sequencestars: imagingstars: windsoutflowsaccretionaccretion disksradiative transfertechniques: high angular resolutiontechniques: interferometriccircumstellar matterstars: emission-lineBe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 257 - 258
Copyright
© International Astronomical Union 2020 

References

Kreplin, A., Tambovtseva, L., Grinin, V., Kraus, S., Weigelt, G., & Wang, Y. 2018, MNRAS, 476, 4520 CrossRefGoogle Scholar
Hone, E., Kraus, S., Kreplin, A., Hofmann, K.-H., Weigelt, G., Harries, T., & Kluska, J. 2018, A&A, 607, 17 Google Scholar
Hofmann, K.-H., Weigelt, G., & Schertl, D. 2014, A&A, 565, 48 Google Scholar