PHYSICAL STRUCTURE AND NATURE OF SUPERNOVA REMNANTS IN M101
نویسندگان
چکیده
منابع مشابه
The nature of bilateral supernova remnants
We present high-resolution radio images at 1.4 GHz of two Galactic supernova remnants (SNRs), G003.8–00.3 (formerly G003.7–00.2) and G350.0– 02.0 (formerly G350.0-01.8). Although the two objects are very different in appearance, in both cases the radio emission shows a clear bilateral (or “barrel”) morphology for which the axis is parallel to the Galactic Plane. The majority of Galactic SNRs ha...
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Radio observations of starburst regions in galaxies have revealed groups of compact nonthermal sources that may be radiative supernova remnants expanding in the interclump medium of molecular clouds. Because of the high pressure in starburst regions, the interclump medium may have a density ∼ 10 H atoms cm in a starburst nucleus like M82 and & 10 H atoms cm in an ultraluminous galaxy like Arp 2...
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In the following, we shall briefly summarize some facts and ideas concerning the presence of neutron stars in Supernova remnants. While sources similar to the Crab Nebula require the presence of a central energetic object, shell-type remnants such as Cas A are compatible with the presence of neutron stars releasing a weak relativistic wind. Supernova remnants are usually classified into two ext...
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Massive (>∼8 M ) stars may end their lives in the molecular clouds in which they were born. O-type stars probably have sufficient photoionizing radiation and wind power to clear a region > 15 pc in radius of molecular material. Early B stars (B1–B3 on the main sequence, or 8 − 12 M stars) are not capable of this and may interact directly with molecular gas. Molecular clouds are known to be clum...
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ژورنال
عنوان ژورنال: The Astronomical Journal
سال: 2012
ISSN: 0004-6256,1538-3881
DOI: 10.1088/0004-6256/143/4/85