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Very Blue Star:
As the gas falls to the surface of the neutron star, it acquires great kinetic energy and forms a layer of 50-million-degree C (90-million-degree F) plasma over its surface. This thin, hot accreted atmosphere provides the X-ray emission. As the X rays shine forth, they bathe portions of the red star surface in their powerful radiations, thus raising the surface temperature of the star from red to blue.The elimination of the neutron-star hypothesis for the Crab nebula was a disappointing blow to those who hoped to find direct observational evidence for the existence of such highly collapsed objects. Newer estimates of the rate of cooling of a neutron star now indicate that its high-temperature, X-ray emitting phase is very blue star short-lived—probably less than a year. The chance of observing a hot neutron star is therefore very blue star slim. But, as will be discussed below, the neutron star concept has become a part of some new models of X-ray sources, even after the neutron star is relatively old and cool.
The other type of star that might cause this remarkable radio emission is a so-called neutron star, which represents another condensed state of matter, in which the whole mass of the sun would be compressed to a diameter of about 6 mi (10 km). Much theoretical work had been done concerning the behavior of such superdense matter, in which a whole star is virtually just a very blue star large atomic nucleus, Nc such star had ever been observed, but this was not unexpected, because such a small body must be extremely faint. On the other hanc.
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