On the Propinquity of Shock-Excited and Photoionized Plasma:The Supernova Remnant and the H II Region of N63A

Details On the Propinquity of Shock-Excited and Photoionized Plasma:The Supernova Remnant and the H II Region of N63A On the Propinquity of Shock-Excited and Photoionized Plasma:The Supernova Remnant and the H II Region of N63A

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....110..739l&link_type=abstract

Astronomical Journal v.110, p.739

Astronomy and Astrophysics

Astronomy

22

Supernova Remnants, Shock Waves, Hii Regions, Plasmas

Scientific paper

We present spectra covering the range λ3400-λ10100 of nebula N63A in the Large Magellanic Cloud. This object contains a supernova remnant adjacent to an H II region and thus illustrates vividly the optical and near-infrared differences between shock-ionized and photoionized emission nebulae. Species of low ionization potential, such as [S II] and [C I], predominate and emit strongly in the shock-heated region, while these elements are more highly ionized in the H II region. The gas-phase abundance of elements also affects their emission line strengths, and this depends on the particular excitation mechanism. A supernova shock can liberate calcium that is bound to interstellar grains, while photoionization does not reduce gas-phase depletion. In addition to providing a laboratory for comparison of the effects of shocks and photons on the interstellar medium, N63A is a bright object, which enables the measurement of lines that are typically too weak to observe elsewhere. In the shocked region we identify five lines of the 1F multiplet of Cr II and measure lines of [Cl II] and [C I].

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