Hostname: page-component-586b7cd67f-t8hqh Total loading time: 0 Render date: 2024-11-28T03:02:20.442Z Has data issue: false hasContentIssue false
  • English
  • Français

A Model for R Aqr from HST

Published online by Cambridge University Press:  07 August 2017

Denis Burgarella ,
Manfred Vogel  and
Francesco Paresce
Denis Burgarella
Affiliation:
1 STScI, 3700 San Martin Drive, Baltimore, Md 21218
Manfred Vogel
Affiliation:
2 Institute of Astronomy, ETH Zürich, Switzerland
Francesco Paresce
Affiliation:
1 STScI, 3700 San Martin Drive, Baltimore, Md 21218 3 Affiliated to the Astrop. Division, Space Science Department, ESA

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.

High spatial resolution observations R Aqr have been carried out with the HST/FOC. R Aqr is the nearest symbiotic star, i.e. an interacting system consisting of a cool giant star and a hot ionizing source embedded in a larger and complex nebula. We suggest, here, that the binary system is composed of a Mira and a hot stellar source with a radiation temperature of T * ≈ 40 000 K, a luminosity of L ≈ 10L⊙ and a radius R ≲ 0.1 R⊙. Mass transfer between the two components of the system occurs via capture of the Mira wind. Of the plausible mechanisms that may produce the R Aqr jet, an accretion/ejection scenario or the collision of winds seem to be unlikely, but spectral observations of the core are needed to conclude. Another possible origin is based on a spherically symmetric stellar wind that sweeps out a cavity in an ambient medium. This bubble elongates in the directions of least resistance, and matter eventually flows out through two symmetric nozzles. Comparison with models shows that the emission in the NE and SW outer features of the jets is due to a radiative shock but the pre-shock gas must be partially photoionized by the central hot stellar source.

Type
Oral and Contributed Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 425 - 428
Copyright
Copyright © Kluwer 1992 

References

Burgarella, D. and Paresce, F. 1991, Ap. J. , 370, 590 Google Scholar
Hartigan, P., Raymond, J. and Hartmann, L. 1987, Ap. J. , 316, 323 Google Scholar
Hollis, J.M., Oliversen, R.J., Kafatos, M., Michalitsianos, A.G. and Wagner, R. M. and 1991, Ap. J. (in press) Google Scholar
Kenyon, S.J. 1985, “Interacting Binaries” in Eggleton, P.P. and Pringle, J.E. (eds.), Reidel Pub. Comp., Dordrecht, p. 179 CrossRefGoogle Scholar
Livio, M. 1988, “The Symbiotic Phenomenon”, in Mikolajewska, J., Friedjung, M., Kenyon, S. C. and Viotti, R. (eds.), Kluwer Academic Pub., Dordrecht, p. 249 Google Scholar
Nussbaumer, H. and Vogel, M. 1987, Astr. Ap. , 213, 137 Google Scholar
Paresce, F. et al. 1991, Ap. J. , (in press) Google Scholar
Raga, and Cantó, 1989 Ap. J. , 344, 404 CrossRefGoogle Scholar
Solf, J. and Ulrich, H. 1985, Ap. J. , 148, 274 Google Scholar
Vogel, M.: 1990, , Google Scholar
Whitelock, P. A. 1987, Pub. A.S.P. , 99, 573 CrossRefGoogle Scholar