Interaction-powered supernova

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An interaction-powered supernova is the final explosion of a star, whereby the light curve of the supernova is influenced by the interaction between the ejected gas envelope and circumstellar matter.

Stars can no longer avert a gravitational collapse if, through thermonuclear reactions, they no longer generate enough energy inside them to maintain a pressure that effectively counteracts the gravitational forces of the outer layers. Before this event, the stars lost part of their atmosphere via stellar winds in massive stars or in interacting binary stars . If the star subsequently explodes as a supernova, then there is an interaction between the circumstellar matter and the shell accelerated during the supernova explosion.

During this interaction, part of the kinetic energy is converted into electromagnetic radiation, which can be detected in the optical and infrared . Interaction-powered supernovae include:

  • The IIn type supernova. This is a subspecies of the hydrogen-rich core collapse supernovae , which show narrow lines of hydrogen in their spectra. The narrow lines are assigned to the hydrogen of the circumstellar matter, which is moving away from the star at a significantly slower speed than the outer shell of the star accelerated during the supernova explosion.
  • A subclass of the hypernovae . This form of superluminous supernovae reaches bolometric brightnesses of at least −21 magnitudine and represents only 0.01 percent of all core collapse supernovae. Their maximum is very broad and shows a spectral course similar to the supernovae of type IIn. They probably arise in dense circumstellar shells of yellow hypergiant or luminous blue variables , whose rates of mass loss can reach values ​​of up to a tenth of the solar masses per year.
  • The Ia-CSM type supernovae. This subgroup of thermonuclear supernovae shows in their spectra shortly after the maximum signs of narrow hydrogen lines similar to the supernovae of type IIn. The type Ia-CSM supernovae probably arise in symbiotic binary star systems in which a white dwarf accretes mass from its companion and the degenerative pressure can no longer prevent the collapse of gravity.

The supernova impositors do not belong to the interaction-powered supernovae . Most of the electromagnetic radiation in these explosions also arises from interactions between an ejected envelope and a circumstellar envelope. The impositors (dt. Jugglers) can achieve luminosity that correspond to those of a core collapse supernova. However, it is not a supernova explosion, but a large eruption of a luminous blue variable.

In the interaction-powered supernovae, the supernova shock breakout is easier to observe because it is not the eruption from the photosphere that only lasts a few hours. Because the circumstellar matter slowed the shock wave and because of its inhomogeneity, the Supernova Shock Breakout lasts for several days and was probably detected in the Interaction-Powered Supernova SN 2010jl. Interaction-powered supernova are also considered to be the place where part of the cosmic radiation is generated .

literature

  • Eran O. Ofek et al .: INTERACTION-POWERED SUPERNOVAE: RISE-TIME VS. PEAK-LUMINOSITY CORRELATION AND THE SHOCK-BREAKOUT VELOCITY . In: Astrophysics. Solar and Stellar Astrophysics . 2014, arxiv : 1404.4085v1 .
  • Kohta Murase, Todd A. Thompson and Eran O. Ofek: Probing cosmic-ray ion acceleration with radio-submm and gamma-ray emission from interaction-powered supernovae . In: Astrophysics. Solar and Stellar Astrophysics . 2013, arxiv : 1311.6778v2 .
  • Takashi J. Moriya, Keiichi Maeda, Francesco Taddia, Jesper Sollerman, Sergei I. Blinnikov, Elena I. Sorokina: An Analytic Bolometric Light Curve Model of Interaction-Powered Supernovae and its Application to Type IIn Supernovae . In: Astrophysics. Solar and Stellar Astrophysics . 2013, arxiv : 1307.2644v2 .