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By Plummer H. C. 1875
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Extra resources for An Introductory Treatise On Dynamical Astronomy
By requiring a fit to the X-ray counting-rate map and agreement between the computed spectrum and the spectrum observed by other instruments (Davison, Culhane, and Mitchell 1976; Becker et al. 1979), they arrive at a total of ~15 Me. Coupled with the evidence supporting significant preexplosion mass loss, it appears certain that the Cas A progenitor was a massive star. Although several of the other historical remnants are thought to have resulted from Type I supernova explosions and thus to have had lower mass progenitors, their X-ray morphology is rather similar to that of Cas A - circular, limb-brightened shells with strong variations around the shell rim which are often uncorrelated with bright spots in the radio and optical maps.
Nn, L. 1946, Ni-iturwiss, 33, 118. Boesgaard, A. M. 1974, Ap:-:J. ,-188, 567. Bopp, B. H. 1980, in Highlights()f Astronomy, 2, p. 847. Bruner, E. , Jr. , and Roth, M. 1980, Astr. , i:l press. , Snow, T. , and Charles, P. 1979, -Ap-:- J. (Letters), 232, L111. -------Cassine1li, J. P. ::~__ ~~tr. , 12,275. T. P. H;lldron, H. , Vaiana, G. S" and Rosner, R. , 11,775. Castor, J. 1. 1980, privflte cOITJrTIunication. Conti, P. S. and Niemala, V. \ 1976, Ap. J. (tetters), 209, L37. Cram, 1. E. 1978, Astr.
There is no proof for this conclusion yet, but there is strong circumstantial evidence, including: (1) the correlation of largescale photospheric magnetic fields with bright X-ray emission from overlying coronal active regions, (2) the loop-like structure of bright coronal X-ray emission just described, (3) the empirical correlation of magnetic field flux with X-ray emission (Golub et al. 1980a,b), and (4) the empirical correlation of photospheric magn~tic field strength and chromospheric emission line flux in the supergranulcltion network (Skumanich et al.
An Introductory Treatise On Dynamical Astronomy by Plummer H. C. 1875