Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-24T03:10:18.268Z Has data issue: false hasContentIssue false
  • English
  • Français

Study of environment and photosphere of 51 Oph

Published online by Cambridge University Press:  23 January 2015

N. Jamialahmadi ,
Ph. Berio ,
B. Lopez ,
A. Meilland  and
Ph. Stee
N. Jamialahmadi
Affiliation:
Laboratoire D.-L. Lagrange, UMR 7293 UNS-CNRS-OCA, Boulevard de l'Observatoire, CS 34229, 06304 NICE Cedex 4, France email: [email protected]
Ph. Berio
Affiliation:
Laboratoire D.-L. Lagrange, UMR 7293 UNS-CNRS-OCA, Boulevard de l'Observatoire, CS 34229, 06304 NICE Cedex 4, France email: [email protected]
B. Lopez
Affiliation:
Laboratoire D.-L. Lagrange, UMR 7293 UNS-CNRS-OCA, Boulevard de l'Observatoire, CS 34229, 06304 NICE Cedex 4, France email: [email protected]
A. Meilland
Affiliation:
Laboratoire D.-L. Lagrange, UMR 7293 UNS-CNRS-OCA, Boulevard de l'Observatoire, CS 34229, 06304 NICE Cedex 4, France email: [email protected]
Ph. Stee
Affiliation:
Laboratoire D.-L. Lagrange, UMR 7293 UNS-CNRS-OCA, Boulevard de l'Observatoire, CS 34229, 06304 NICE Cedex 4, France 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 main objective of this work is to improve our understanding of young fast-rotating stars evolving from the Herbig Ae/Be class to the Vega-like one. We observed with the VEGA instrument on CHARA one object so-called 51 Oph that is probably in such an evolutionary phase, allowing us to measure a mean stellar radius for the first time for this star and to show that the Hα emission was produced in a Keplerian rotating disc. However, additional observations are needed to improve our (u,v) plan coverage in order to measure the flattening of this close-to-critically rotating star and to probe the inner region of its circumstellar gaseous disc. These studies will help to disentangle the gas and dust emission around this late young star and will finally improve our understanding of the planet formation conditions in the inner regions of protoplanetary discs.

Keywords

stars: atmospheresstars: fundamental parametersstars: emission-linestars: Bestars: kinematics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 111 - 112
Copyright
Copyright © International Astronomical Union 2015 

References

Bonneau, D., Clausse, J.-M., Delfosse, X., et al. 2006, A&A 456, 789Google Scholar
Mendigutía, I., Mora, A., Montesinos, B., et al. 2012, A&A 543, A59Google Scholar
Mourard, D., Clausse, J. M., Marcotto, A., et al. 2009, A&A 508, 1073Google Scholar
Perryman, M. A. C., Lindegren, L., Kovalevsky, J., et al. 1997, A&A 323, L49Google Scholar
Tatulli, E., Malbet, F., Ménard, F., et al. 2008, A&A 489, 1151Google Scholar
ten Brummelaar, T. A., McAlister, H. A., Ridgway, S. T., et al. 2005, ApJ 628, 453Google Scholar
Thi, W.-F., van Dalen, B., Bik, A., & Waters, L. B. F. M. 2005, A&A 430, L61Google Scholar
van den Ancker, M. E., de Winter, D., & Tjin, A., Djie, H. R. E. 1998, A&A 330, 145Google Scholar