Testing Massive Star Formation Theory in Orion
Abstract
I compare theoretical models of massive star formation with observations of the Orion Hot Core, which harbors one of the closest massive protostars. Although this region is complicated, many of its features (size, luminosity, accretion disk, HII region, outflow) may be understood by starting with a simple model in which the star forms from a massive gas core that is a coherent entity in approximate pressure balance with its surroundings. The dominant contribution to the pressure is from turbulent motions and magnetic fields. The collapse can be perturbed by interactions with other stars in the forming cluster, which may induce sporadic enhancements of the accretion and outflow rate.
Cite
@article{arxiv.astro-ph/0310724,
title = {Testing Massive Star Formation Theory in Orion},
author = {Jonathan C. Tan},
journal= {arXiv preprint arXiv:astro-ph/0310724},
year = {2007}
}
Comments
8 pages, in proceedings of Star Formation in the Interstellar Medium, workshop honoring David Hollenbach, Chris McKee, & Frank Shu, eds. F.C. Adams, D. Johnstone, D.N.C. Lin, & E.C. Ostriker, ASP. An expanded overview of observations of the Orion Hot Core region can be found at http://astro.princeton.edu/~jt/orion/orionhotcore.html