Astronomy:X-ray flash

From HandWiki
Jump to: navigation, search

In astronomy, an X-ray flash is a transient emission of X-rays originating in a distant galaxy, probably caused by a hypernova. They have been observed to last 90 to 200 seconds.[1]

Nearly all hypernovae are detected via (higher-energy) gamma-ray photons, at distances too great for any associated X-ray emissions from them to be observed; nevertheless, the two main theories of the nature of an X-ray flash each assume that a hypernova is involved:[1]

  • One theory assumes that an X-ray-flash hypernova does not differ inherently from gamma-ray-emitting hypernovae, but rather in the orientation, relative to the line of sight to the observer, of the narrow beam of gamma radiation from the hypernova.[1] That is, gamma rays are assumed to be emitted, but in each case in a direction away from our instruments for observing them. Thus the only initially observable phenomenon is lower-energy x-rays emitted in a beam that diverges more than the gamma-ray beam does.
  • A competing "dirty fireball" theory suggests that an X-ray flash comes from a hypernova that uses much of the available energy in expelling an unusually large amount of baryonic matter,[1] thus limiting the energy available for electromagnetic radiation, and emitting a much "cooler" spectrum rich in X-rays and very poor in gamma rays.

Further reading


  1. 1.0 1.1 1.2 1.3 "X-ray flash", Centre for Astrophysics and Supercomputing, (n.d.), viewed October 29, 2013

Grammarly Check DataMelt statistical framewwork for data scientists HandWiki ads