Abstract
We have used Hα + [N II] and [S II] interference filter photography to identify nebulosities which we believe to be supernova remnants in M31. Spectrophotometry has been used to confirm this identification for 12 of the candidates. Since all the remnants are at the same distance, they can be directly compared. Using the measured diameter and an estimate of the pressure in the optical filaments, an initial energy for each remnant has been calculated. However, this energy appears to be correlated to the remnant’s diameter, an effect which may be related to magnetic pressure in the filaments.
The spectra have also been used in conjunction with shock model calculations to study abundance gradients in M31. Comparison of these results to abundance gradients obtained from H II regions allows an appraisal of the accuracy of the two methods. We find gradients in nitrogen and oxygen abundances that are comparable to those seen in other intermediate to late type spiral galaxies.
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Blair, W.P. (1982). Supernova Remnants in M31. In: Rees, M.J., Stoneham, R.J. (eds) Supernovae: A Survey of Current Research. NATO Advanced Study Institutes Series, vol 90. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7876-8_28
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DOI: https://doi.org/10.1007/978-94-009-7876-8_28
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