Dusty Magnetohydrodynamics in Star Forming Regions

Details Dusty Magnetohydrodynamics in Star Forming Regions Dusty Magnetohydrodynamics in Star Forming Regions

2010-01-06

arxiv.org/abs/1001.0929v1

Physics

Plasma Physics

17 pages, 3 figures, accepted for publication in the Journal of Plasma Physics special issue in honour of Prof. Padma K. Shukl

Scientific paper

Star formation occurs in dark molecular regions where the number density of hydrogen nuclei, nH, exceeds 10^4 cc and the fractional ionization is 10^-7 or less. Dust grains with sizes ranging up to tenths of microns and perhaps down to tens of nanometers contain just under one percent of the mass. Recombination on grains is important for the removal of gas phase ions, which are produced by cosmic rays penetrating the dark regions. Collisions of neutrals with charged grains contribute significantly to the coupling of the magnetic field to the neutral gas. Consequently, the dynamics of the grains must be included in the magnetohydrodynamic models of large scale collapse, the evolution of waves and the structures of shocks important in star formation.

Affiliated with

Also associated with

No associations

Rating

Dusty Magnetohydrodynamics in Star Forming Regions does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Dusty Magnetohydrodynamics in Star Forming Regions, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Dusty Magnetohydrodynamics in Star Forming Regions will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-164487