2006/02/13 by Chizuru Akizuki, C. Akizuki, Jun Fukue +2 · 76 citations
Physics and Astronomy · #Acoustics #Advection #Angular velocity #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Classical mechanics #Geometry #Isothermal process #Magnetic field #Mechanics #Physics #Plasma #Pulsars and Gravitational Waves Research #Radial velocity #Rotation (mathematics) #Rotational speed #Speed of sound #Stars #Toroid #astro-ph
paper · pdf · doi:10.1093/pasj/58.2.469
published in Publications of the Astronomical Society of Japan 58(2), 469-475 (Oxford University Press) · 5pages, 2figures, PASJ 58 (2006) in press
arxiv created 2006/02/13 · openalex publication_date 2006/04/25 · arxiv updated 2015/06/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We examined the effect of toroidal magnetic fields on a viscous gaseous disk around a central object under an advection-dominated stage. We found self-similar solutions for the radial infall velocity, rotation velocity, and sound speed, with an additional parameter, β [=cA2/(2 cs2)], where cA is the Alfvén speed and cs is the isothermal sound speed. Compared with the non-magnetic case, in general the disk becomes thick due to the magnetic pressure, and the radial infall velocity and rotation velocity become fast. In a particular case, where the magnetic field is dominant, on the other hand, the disk becomes to be magnetically supported, and the nature of the disk is significantly different from that of the weakly magnetized case.