Hostname: page-component-77c89778f8-7drxs Total loading time: 0 Render date: 2024-07-25T04:18:49.590Z Has data issue: false hasContentIssue false
  • English
  • Français

A Drag Dominated Model of the Magellanic Stream

Published online by Cambridge University Press:  25 April 2016

Gerhardt R. Meurer ,
G. V. Bicknell  and
R. A. Gingold
Gerhardt R. Meurer
Affiliation:
Mount Stromlo and Siding Spring Observatories Research School of Physical Sciences The Australian National University
G. V. Bicknell
Affiliation:
Mount Stromlo and Siding Spring Observatories Research School of Physical Sciences The Australian National University
R. A. Gingold
Affiliation:
Mount Stromlo and Siding Spring Observatories Research School of Physical Sciences The Australian National University
Get access Rights & Permissions [Opens in a new window]

Abstract

We present here the best of a series of models of the Magellanic stream. The dominant force in these models is gas drag. Gaseous cloudlets are torn from the bridge between the Large and Small Magellanic Clouds as the Magellanic system passes through a hot gaseous halo about our galaxy. The cloudlets are then stretched apart from each other by tidal and drag forces to form the Magellanic stream. Our best model closely reproduces the position of the stream on the sky and the run of radial velocities along the Magellanic stream. The agreement is almost as good as the best purely tidal model. In our best model the Magellanic system is only loosely bound to our galaxy and is on the first encounter with it. This overcomes some of the problems with purely tidal models. Our series of models indicate that there is a wide range of parameters that will produce a reasonable stream under the forces of gas drag and gravity.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 6 , Issue 2 , 1985 , pp. 195 - 198
Copyright
Copyright © Astronomical Society of Australia 1985

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Bruck, M. T., and Hawkins, M. R. S., 1983, Astron. Astrophys., 124, 216.Google Scholar
Dopita, M. A., 1985, private communications.Google Scholar
Fujimoto, M., and Sofue, Y., 1976, Astron. Astrophys., 47, 263.Google Scholar
Gingold, R. A., 1984, Proc. Astron. Soc. Aust., 5, 469.Google Scholar
Gingold, R. A., 1985, Preprint.Google Scholar
Lin, D. N.C, and Lynden-Bell, D., 1982, Mon. Not. R. Astron. Soc., 198, 707.CrossRefGoogle Scholar
Mathewson, D. S., Cleary, M. N., and Murray, J. D., 1974, Astrophys.J., 190, 291.Google Scholar
Mathewson, D. S., 1985, private communications.Google Scholar
Murai, T., and Fujimoto, M., 1980, Pub. Astron. Soc. Jap., 32, 581.Google Scholar
Murai, T., and Fujimoto, M., 1984, preprint.Google Scholar
Roulf, K., 1985, private communications.Google Scholar
Songaila, A., 1981, Astrophys. J., 248, 956.Google Scholar