2009/08/26 by N. Turner, N. J. Turner, J. F. Drake
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Astrophysics and Star Formation Studies #Galaxy #Interstellar medium #Mechanics #Nuclear physics #Physics #Radionuclide #Stellar, planetary, and galactic studies #Supernova #Turbulence #astro-ph.EP #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/703/2/2152
Accepted for the Astrophysical Journal
arxiv created 2009/08/26 · openalex publication_date 2009/09/16 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We calculate the location of the magnetically inactive dead zone in the minimum-mass protosolar disk, under ionization scenarios including stellar X-rays, long- or short-lived radionuclide decay, and energetic protons arriving from the general interstellar medium, from a nearby supernova explosion, from the disk corona, or from the corona of the young star. The disk contains a dead zone in all scenarios except those with small dust grains removed and a fraction of the short-lived radionuclides remaining in the gas. All the cases without exception have an "undead zone" where intermediate resistivities prevent magneto-rotational turbulence while allowing shear-generated large-scale magnetic fields. The mass column in the undead zone is typically greater than the column in the turbulent surface layers. The results support the idea that the dead and undead zones are robust consequences of cold, dusty gas with mass columns exceeding 1000 g cm −2 .