Magnetic field amplification in the solar nebula through interaction with the T-Tauri wind

Details Magnetic field amplification in the solar nebula through interaction with the T-Tauri wind Magnetic field amplification in the solar nebula through interaction with the T-Tauri wind

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.312..625i&link_type=abstract

Nature (ISSN 0028-0836), vol. 312, Dec. 13, 1984, p. 625, 626.

Physics

6

Paleomagnetism, Solar Corona, Solar Magnetic Field, Stellar Evolution, T Tauri Stars, Carbonaceous Chondrites, Dynamo Theory, Interplanetary Magnetic Fields, Magnetohydrodynamics, Solar System

Scientific paper

The remnant magnetization of carbonaceous chondrites can be used to estimate the intensity of the magnetic field in the primordial solar nebula. Estimates vary between 0.2 and 1 G, with the possibility that the field may have been as high as 2 - 3 G. This letter presents a possibility for the origin of a strong magnetic field in the early solar system: magnetic field enhancement at the point of stagnation between the solar nebula and the intense solar outflows. This mechanism, which involves the interaction of the T Tauri wind with the solar nebula, is straightforward and is supported by results from recent space research.

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