During star formation, both infall and outflows are present around protostellar cores. Here we show solutions of a self-similar model that study the two flows with only one set of equations. We focus here on the effects of magnetic field and dust on solutions. Unmagnetized solutions have also been found. This shows that magnetic field is not the main driving mechanism of the circulation process. We have found that a reduction of magnetic field produces denser, slower and narrower outflows. When the opacity is less dominated by dust, density increases in the equatorial region, allowing larger accretion rates to occur. The comprehension of massive star formation could be related to this latter effect.
|Number of pages||6|
|Journal||Astrophysics and Space Science|
|State||Published - 2004|
|Event||International Workshop on Magnetic Fields and Star Foramtion - Madrid, Spain|
Duration: Apr 21 2003 → Apr 25 2003
- star formation