Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-12T22:20:15.370Z Has data issue: false hasContentIssue false
  • English
  • Français

A companion star in the SED modeling of the HD 142527 stellar system

Published online by Cambridge University Press:  06 January 2014

Erick Nagel
Erick Nagel*
Affiliation:
Departamento de Astronomía, Universidad de Guanajuato, Callejón de Jalisco S/N, Valenciana, 36240, Guanajuato, México 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 discovery of a likely companion of the Herbig Ae/Be star HD 142527 motivates the study of the effect that it produces on the SED. The main change on the system configuration is the formation of a gap in the disk in which the companion is embedded, following the orbit of the secondary star. This results in the formation of a wall (at the outer gap edge), which is illuminated by stellar radiation. We present a model for the SED, taking into account all the components of the system: the two stars, the disk with two gaps (one produced by the stellar companion and the other by potential planets), three walls (two associated with the gaps and the other with dust sublimation), optically thin material in the gaps and in a halo. The size of the modeled spherical halo is smaller than found in a previous study.

Keywords

binaries:generalplanetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 222 - 223
Copyright
Copyright © International Astronomical Union 2013 

References

Biller, B., et al. 2012, ApJ, 753, L38Google Scholar
Casassus, S., Perez, M. S., Jordán, A., Ménard, F., Cuadra, J., Schreiber, M. R., Hales, A. S., & Ercolano, B. 2012, ApJ, 754, L31Google Scholar
D'Alessio, P., et al. 2005, ApJ, 621, 461CrossRefGoogle Scholar
Dullemond, C. P., Dominik, C., & Natta, A. 2001, ApJ, 560, 957CrossRefGoogle Scholar
Fujiwara, H., et al. 2006, ApJ, 644, L133CrossRefGoogle Scholar
Fukagawa, M., Tamura, M., Itoh, Y., Kudo, T., Imaeda, Y., Oasa, Y., Hayashi, S. S., & Hayashi, M. 2006, ApJ, 636, L153Google Scholar
Krijt, S. & Dominik, C. 2011, A&A, 531, 80Google Scholar
Nagel, E., Espaillat, C., D'Alessio, P., & Calvet, N. 2012, ApJ, 747, 139Google Scholar
Nagel, E., D'Alessio, P., Calvet, N., Espaillat, C., & Trinidad, M. A. 2013, Rev. Mexicana AyA, 49, 43Google Scholar
Raymond, S. N. & Armitage, P. J. 2013, MNRAS, 429, L99Google Scholar
Verhoeff, A. P.et al. 2011, A&A, 528, 91Google Scholar