Hostname: page-component-cd9895bd7-p9bg8 Total loading time: 0 Render date: 2024-12-24T02:03:10.947Z Has data issue: false hasContentIssue false
  • English
  • Français

Herbig Ae/Be stars with TGAS parallaxes in the HR diagram

Published online by Cambridge University Press:  07 March 2018

Miguel Vioque Open the ORCID record for Miguel Vioque [Opens in a new window] ,
René D. Oudmaijer  and
Deborah Baines
Miguel Vioque*
Affiliation:
School of Physics and Astronomy, University of Leeds, Leeds, United Kingdom Isdefe, European Space Astronomy Centre (ESAC), Madrid, Spain
René D. Oudmaijer
Affiliation:
School of Physics and Astronomy, University of Leeds, Leeds, United Kingdom
Deborah Baines
Affiliation:
Isdefe, European Space Astronomy Centre (ESAC), Madrid, Spain
*
*email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The intermediate mass Herbig Ae/Be stars are young stars approaching the Main Sequence and are key to understanding the differences in formation mechanisms between magnetic low mass stars and non-magnetic high mass stars. A large fraction of known Herbig Ae/Be stars have TGAS parallaxes, which were used to derive luminosities and place 107 of these objects in the HR diagram, increasing the number of objects using directly determined parallaxes by a factor of 5. We also studied the characteristics of the infrared excesses of this set of Herbig Ae/Be stars and we linked our results to an evolutionary analysis.

Keywords

stars: formationstars: fundamental parametersHertzsprung-Russell diagramstars: pre–main-sequenceinfrared: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 277 - 278
Copyright
Copyright © International Astronomical Union 2018 

References

van den Ancker, M. E., de Winter, D., & Tjin, A Djie, H. R. E., 1998, A&A, 330, 145 Google Scholar
Bressan, A., Marigo, P., Girardi, L., Salasnich, B., Dal Cero, C., et al., 2012, MNRAS, 427, 127 Google Scholar
Castelli, F. & Kurucz, R. L. 2004, ArXiv Astrophysics e-prints, arXiv:astro-ph/0405087Google Scholar
Chen, P. S., Shan, H. G., & Zhang, P., 2016, New Astron., 44, 1 Google Scholar
Fairlamb, J. R., Oudmaijer, R. D., Mendigutía, I., et al., 2015, MNRAS, 453, 976 Google Scholar
McDonald, I., Zijlstra, A. A., & Boyer, M. L., 2012, MNRAS, 427, 343 Google Scholar
Montesinos, B., Eiroa, C., Mora, A., & Merín, B., 2009, A&A, 495, 901 Google Scholar