Search results
Results from the WOW.Com Content Network
Central neutron star at the heart of the Crab Nebula Radiation from the rapidly spinning pulsar PSR B1509-58 makes nearby gas emit X-rays (gold) and illuminates the rest of the nebula, here seen in infrared (blue and red). A neutron star is the collapsed core of a massive supergiant star.
Neutron stars can be classified as pulsars if they are magnetized, if they rotate, and if they emit beams of electromagnetic radiation out of their magnetic poles. [4] They may include soft gamma repeaters (SGR) and radio-quiet neutron stars, as well as pulsars such as radio pulsars, recycled pulsars, low mass X-ray pulsars, and accretion ...
Below is a list of high-mass neutron stars. ... Spectroscopic observation and orbital decay due to radiation of gravitational waves. [10] [18] PSR B1516+02B: 1.94 +0.17
An X-ray pulsar is a type of binary star system consisting of a typical star (stellar companion) in orbit around a magnetized neutron star.The magnetic field strength at the surface of the neutron star is typically about 10 8 Tesla, over a trillion times stronger than the strength of the magnetic field measured at the surface of the Earth (60 μT).
The Crab Pulsar (PSR B0531+21 or Baade's Star) is a relatively young neutron star. The star is the central star in the Crab Nebula, a remnant of the supernova SN 1054, which was widely observed on Earth in the year 1054. [8] [9] [10] Discovered in 1968, the pulsar was the first to be connected with a supernova remnant. [11]
Cooling neutron stars have temperatures of order 1 million kelvins and so thermally emit at X-ray wavelengths. Measurement of an x-ray spectrum allows the temperature to be determined, assuming it is thermal emission from the surface of a neutron star. The resulting temperature for RRAT J1819-1458 is much cooler than that found on the surface ...
Neutron radiation is a form of ionizing radiation that presents as free neutrons. Typical phenomena are nuclear fission or nuclear fusion causing the release of free neutrons, which then react with nuclei of other atoms to form new nuclides —which, in turn, may trigger further neutron radiation.
So far, most data about neutron-star oscillations come from the blasts of four specific Soft Gamma Repeaters, SGR, especially the event of 27 December 2004 from SGR 1806-20. Because so few events have been observed, little is known for sure about neutron stars and the physics of their oscillations.