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Their brevity made them difficult to trace. Once their direction could be determined, it was found that they were evenly spread across the sky.
Thus they were not originating in the Milky Way or nearby galaxies, but from deep space. The usage of the term hypernova from the late 20th century has since been refined to refer to those supernovae with unusually large kinetic energy.
Other scientists prefer to call these objects simply broad-lined type Ic supernovae. These are typically of type Ic, and some are associated with long-duration gamma-ray bursts.
The electromagnetic energy released by these events varies from comparable to other type Ic supernova, to some of the most luminous supernovae known such as SN as.
Its spectrum showed no hydrogen and no clear helium features, but strong silicon lines identified it as a type Ic supernova. The main absorption lines were extremely broadened and the light curve showed a very rapid brightening phase, reaching the brightness of a type Ia supernova at day Unusually bright radio supernovae have been observed as counterparts to hypernovae, and have been termed radio hypernovae.
Models for hypernova focus on the efficient transfer of energy into the ejecta. It is thought that rotation of the supernova progenitor drives a jet that accelerates material away from the explosion at close to the speed of light.
Binary systems are increasingly being studied as the best method for both stripping stellar envelopes to leave a bare carbon-oxygen core, and for inducing the necessary spin conditions to drive a hypernova.
The collapsar model describes a type of supernova that produces a gravitationally collapsed object, or black hole. The word "collapsar", short for "collapsed star ", was formerly used to refer to the end product of stellar gravitational collapse , a stellar-mass black hole.
The word is now sometimes used to refer to a specific model for the collapse of a fast-rotating star. If such a star is rotating slowly, then it will produce a faint supernova, but if the star is rotating quickly enough, then the fallback to the black hole will produce relativistic jets.
The energy that these jets transfer into the ejected shell renders the visible outburst substantially more luminous than a standard supernova.
The jets also beam high energy particles and gamma rays directly outward and thereby produce x-ray or gamma-ray bursts; the jets can last for several seconds or longer and correspond to long-duration gamma-ray bursts, but they do not appear to explain short-duration gamma-ray bursts.
The mechanism for producing the stripped progenitor, a carbon-oxygen star lacking any significant hydrogen or helium, of type Ic supernovae was once thought to be an extremely evolved massive star, for example a type WO Wolf-Rayet star whose dense stellar wind expelled all its outer layers.
Observations have failed to detect any such progenitors. It is still not conclusively shown that the progenitors are actually a different type of object, but several cases suggest that lower-mass "helium giants" are the progenitors.
These stars are not sufficiently massive to expel their envelopes simply by stellar winds, and they would be stripped by mass transfer to a binary companion.
Helium giants are increasingly favoured as the progenitors of type Ib supernovae, but the progenitors of type Ic supernovae is still uncertain.
One proposed mechanism for producing gamma-ray bursts is induced gravitational collapse, where a neutron star is triggered to collapse into a black hole by the core collapse of a close companion consisting of a stripped carbon-oxygen core.
The induced neutron star collapse allows for the formation of jets and high-energy ejecta that have been difficult to model from a single star. From Wikipedia, the free encyclopedia.
A supernova which ejects a large mass at unusually high velocity. For a completely collapsed star, see stellar black hole.
Astronomy portal. Bibcode : STIN Annual Review of Nuclear and Particle Science. Astronomy and Astrophysics. Bibcode : Natur.