2010/01/06 by S. Van Loo, S. A. E. G. Falle, T. W. Hartquist +2
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Astrophysics and Star Formation Studies #Atomic physics #Dust and Plasma Wave Phenomena #Hydrogen #Ion #Ionization #Magnetic field #Magnetohydrodynamic drive #Magnetohydrodynamics #Nuclear physics #Physics #Plasma #Star formation #Stars #physics.plasm-ph
paper · pdf · doi:10.1017/s0022377809990894
17 pages, 3 figures, accepted for publication in the Journal of Plasma Physics special issue in honour of Prof. Padma K. Shukla
arxiv created 2010/01/06 · openalex publication_date 2010/01/22 · arxiv updated 2015/05/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Star formation occurs in dark molecular regions where the number density of hydrogen nuclei n H exceeds 10 4 cm −3 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 less than 1% 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.