Journal ArticleDOI
Accretion by rotating magnetic neutron stars. II. Radial and vertical structure of the transition zone in disk accretion.
Pranab Ghosh,Frederick K. Lamb +1 more
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TLDR
The radial and vertical structure of the transition zone at the magnetospheric boundary of an aligned rotating neutron star accreting matter from a Keplerian disk is calculated in this article, where the inner edge of the disk is located where the integrated magnetic stress acting on the disk plasma becomes comparable to the integrated material stress associated with its inward radial drift and orbital motion.Abstract:
The radial and vertical structure of the transition zone at the magnetospheric boundary of an aligned rotating neutron star accreting matter from a Keplerian disk are calculated. The results obtained indicate that: (1) the inner edge of the disk is located where the integrated magnetic stress acting on the disk plasma becomes comparable to the integrated material stress associated with its inward radial drift and orbital motion; (2) the stellar magnetic field threads the disk near its inner edge via the Kelvin-Helmholtz instability, turbulent diffusion, and reconnection, producing a broad transition zone between the unperturbed disk flow and corotating magnetosphere; (3) the transition zone consists of two qualitatively different regions, viz., a broad outer transition zone where the motion is Keplerian and a narrow inner zone, or boundary layer, where the departure from Keplerian motion is substantial; (4) the stellar magnetic field is largely but not entirely screened by currents flowing in the boundary layer; and (5) there are no steady-flow solutions for sufficiently fast stellar rotation.read more
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Disk accretion rates for T tauri stars
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The Structure and Emission of the Accretion Shock in T Tauri Stars
TL;DR: In this article, the structure and spectral energy distribution of the emergent continuum emission from a shock at the base of the magnetospheric accretion column were analyzed for T Tauri stars, and it was shown that the spectral shape of the excess can be understood as optically thick emission from the heated photosphere below the shock, appearing mostly on the Paschen and Brackett continua, and optically thin emission from preshock and attenuated postshock regions, dominating at wavelengths shorter than the Balmer threshold.
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Accretion Disks around Young Objects. I. The Detailed Vertical Structure
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