Abstract
A high velocity radiative shock, or one moving into high-metallicity gas, provides an efficient means to generate a strong local UV photon field. The optical emission from the shock and precursor region is dominated by the photoionised gas, rather than by the cooling region, and the total optical + UV emission scales as the mechanical energy flux through the shock. In this paper, such models are applied to oxygen-rich supernova remnants and AGN. For AGN, the degree of magnetic support in the post-shock gas is an important parameter. LINER and cooling flow spectra can be understood as resulting from high velocity shocks without precursors, while Seyfert 1.5–2 galaxy emission line ratios result from high velocity shocks with their photoionised precursor HII regions. This model explains the problem of the high electron temperatures observed in both classes of object.
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Dopita, M.A. (1995). Photoionising Shocks in SNRS and AGN. In: Millar, T.J., Raga, A.C. (eds) Shocks in Astrophysics. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-1624-1_29
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DOI: https://doi.org/10.1007/978-94-009-1624-1_29
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