文档介绍：M 1. The red and green, fi lamentary structure is the debris of the supernova progenitor star. Bluish, by contrast, is the haze of synchrotron
emitting nebulosity. Philipp Keller.
M 1 can be studied throughout the ic spectrum: in sweeping radiation beams, a sharp pulse is observed every revolution,
1948, strong radio emission was found, and X-rays were detected in and hence this type of neutron star is called a “pulsar.”
1964. Hence, the Crab Nebula has additional designations as the Tau- The M 1 pulsar measures only 10 km in diameter but has an ab-
rus A or 3C 144 radio source and as Tau X-1. Its radiated X-ray fl ux solute magnitude of +, slightly brighter than the Sun. A cubic
exceeds its optical fl ux by more than a hundredfold, and the total centimeter of its matter would weigh a thousand million tons – so
energy output has been quoted as 5×1011 joules per second. much has it pressed in the gravitational collapse of the su-
The collapsed core of the star that caused the supernova is still pernova!
present in the center of the nebula. In its intense ic fi eld, The pulsar in M 1 was the fi rst of its kind for which an optical
charged particles get accelerated near the fi eld poles and emit col- counterpart was found. This 16th-magnitude star, registered as CM
limated radiation along the ic fi eld axis, which is tilted with Tauri, sends pulses of light with the same period as the radio pulses,
respect to the rotation axis of the rapidly spinning neutron star. As milliseconds. This makes it a valuable object for scientifi c stu-
Earth happens to be in the right direction to be hit by one of these dy, as very few other optical pulsars are yet known.
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Modern X-ray observations and high-resolution images from
the Hubble Space Telescope show rings of highly energetic particles
around the pulsar of M 1, at distances of to 1 light-year, and jets
emerging perpendicular to the ring plane. Fine structure resolved by
Hubble in 199