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Titlebook: Supernova Shells and Their Birth Events; Proceedings of a Wor Wolfgang Kundt Conference proceedings 1988 Springer-Verlag Berlin Heidelberg

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书目名称Supernova Shells and Their Birth Events
副标题Proceedings of a Wor
编辑Wolfgang Kundt
视频video
丛书名称Lecture Notes in Physics
图书封面Titlebook: Supernova Shells and Their Birth Events; Proceedings of a Wor Wolfgang Kundt Conference proceedings 1988 Springer-Verlag Berlin Heidelberg
描述For a better understanding of supernova explosions the contributors to this volume provide researchers and graduate students in astrophysics with a broad spectrum of alternatives. The confrontation of different theories in one volume should prompt further exploration of the driving piston for the explosions and deeper understanding of the experimental data. Properties of supernova shells are discussed, such as their kinematics, ages, sizes, temperatures, spectra, polarizations, energetics and morphologies. Special attention is given to a few shells of extreme age, viz. G 70.68+1.20, Kepler‘s SN, and CTB 80, as well as to their statistics.
出版日期Conference proceedings 1988
关键词Supernova; Variation; astrophysics; cosmic ray; galaxy
版次1
doihttps://doi.org/10.1007/3-540-50435-4
isbn_softcover978-3-662-13647-8
isbn_ebook978-3-540-46001-5Series ISSN 0075-8450 Series E-ISSN 1616-6361
issn_series 0075-8450
copyrightSpringer-Verlag Berlin Heidelberg 1988
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Interpretation difficulties of SNR shock spectra,ough shock parameters such as velocity and preshock density are significantly different. If the shocks are radiatively unstable, then it may be possible to observe time variations of line ratios in SNRs over a period of a few years.
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Puppis a and its environment as revealed by infrared observations,used to study the structure of the interstellar medium (ISM) in which the SNR expands, to constrain physical parameters of the SNR and the surrounding medium, and to investigate gas — dust interactions in the shocked x-ray emitting gas and the nature of the IR emitting dust.
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A molecular cloud in the direction of G70.68+1.20,e peak CO intensity of the molecular cloud is displaced only a few areseconds from the apparent centre of G70.68+1.20, strongly suggesting a physical relation between both objects. The kinematic distance of the molecular cloud is most likely 5.5 kpc and the diameter of G70.68+1.20 is about 0.55 pc.
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Kinematics of optical filaments in the Cygnus Loop,[0III]. In both lines a number of different components contributing to the emission are recognized. The [0III] emission indicates that the gas may lie in a thin sheet, while from the Hα emission this indication is much less clear.
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