High-resolution spectroscopy of Balmer-dominated shocks in the Large Magellanic Cloud

Details High-resolution spectroscopy of Balmer-dominated shocks in the Large Magellanic Cloud High-resolution spectroscopy of Balmer-dominated shocks in the Large Magellanic Cloud

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...420..286s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 420, no. 1, p. 286-293

Astronomy and Astrophysics

Astrophysics

47

Balmer Series, Cosmic Rays, Magellanic Clouds, Shock Waves, Supernova Remnants, Collisionless Plasmas, Emission Spectra, H Alpha Line, Spectrum Analysis, Stellar Spectrophotometry

Scientific paper

We present high-resolution spectra of the four Balmar-dominated supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). These data allow us to measure the width of the narrow component of H alpha emission in the nonradiative filaments present in these SNRs. We find that the widths range from 30 to 50 km/s FWHM, similar to the only previously measured width of a nonradiative shock filament, that of about 30 km/s in the NE Cygnus Loop. The line widths do not appear to scale with shock velocity. These observations severely limit the possible broadening mechanisms. We discuss several possibilities, the most promising of which is a precursor associtated with cosmic rays. Assuming a cosmic-ray precursor, we are able to place constraints on the cosmic-ray diffusion coefficient. Observations such as these may provide the best method currently available to probe cosmic-ray acceleration in SNR shock waves.

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