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Supersonic ambipolar diffusion: Estimating the magnetic field strength in protostellar outflows

Smith, M.D., Mac Low, M.-M. (1998) Supersonic ambipolar diffusion: Estimating the magnetic field strength in protostellar outflows. Astrophysics and Space Science, 261 (1-4). pp. 191-192. ISSN 0004-640X. (doi:10.1023/A:1002079928518) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided) (KAR id:50145)

The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided.
Official URL
http://dx.doi.org/10.1023/A:1002079928518

Abstract

The magnetic field plays a crucial role in star formation. It is involved in rotational braking, collapse braking, outflow formation and jet collimation. Direct observations of the field are difficult. However, the field can be indirectly estimated through the field-cushioned C-shocks which produce strong infrared molecular emission lines. In particular, a high field in the outflows will generate the 'shock absorber' signature: very broad H2 lines. Such lines are indeed observed. Here we summarise recent progress in C-shock formation and stability. We demonstrate numerically that the Shock Absorbers are evolutionary and stable. The widths of H2 lines then limit the magnetic field strength. A field of 6 mG is suggested for HH 212.

Item Type: Article
DOI/Identification number: 10.1023/A:1002079928518
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Divisions > Division of Natural Sciences > Physics and Astronomy
Depositing User: Giles Tarver
Date Deposited: 11 Aug 2015 10:24 UTC
Last Modified: 16 Nov 2021 10:20 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/50145 (The current URI for this page, for reference purposes)
Smith, M.D.: https://orcid.org/0000-0002-4289-5952
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