## Magnetised protostellar bipolar outflows## I. Self-similar model with Poynting flux
^{1} School of Cosmic Physics, Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland^{2} Department of Physics, Queen's University, Kingston, Ontario, K7L 3N6, Canada^{3} Department of Physics and Astronomy, McMaster University, 1280 Main St. W., Hamilton, Ontario, L8S 4M1, Canada
We study a self-similar circulation model for protostellar bipolar
outflows. The model is axisymmetric and stationary, and now includes
Poynting flux. Compared to an earlier version of the model, this
addition produces faster and more collimated outflows. Moreover the
luminosity needed for the radiative heating is smaller. The solutions
are developed within the context of
This article contains no SIMBAD objects. ## Contents- 1. Introduction
- 2. The analytical model
- 2.1. Self-similar laws
- 2.2. The equations
- 2.3. The zero pressure limit
- 2.4. The critical points
- 3. Numerical analysis
- 3.1. The numerical method
- 3.2. Low-
*µ*protostars - 3.3. High-
*µ*protostars- 3.3.1. The virial-isothermal case
- 3.3.2. The radiative case
- 3.4. Parameter study
- 4. Astrophysical scales
- 5. Observational consequences of the model: Synthetic
^{13}CO spectral lines and maps- 5.1. Low-
*µ*solutions - 5.2. High-
*µ*solutions- 5.2.1. The radiative case
- 5.2.2. The virial-isothermal case
- 5.1. Low-
- 6. Discussion
- 6.1. MHD singularities
- 6.2. Comparison with FH1
- 6.3. Stability considerations
- 7. Conclusions
- Acknowledgements
- Appendices
- References
© European Southern Observatory (ESO) 1999 Online publication: September 24, 1999 |