The classic scenario for a Type Ia supernova is: a white dwarf dies as the remnant of a low-mass star and no longer releases any energy by itself. So where should he get the energy for an explosion that could briefly shine as bright as the entire galaxy around it? Answer: From the star companion. A white dwarf can absorb mass from this. If the mass of the white dwarf exceeds the so-called Chandrasekhar limit by about 1.4 solar masses, the gravity becomes very strong and the white dwarf explodes.
But as it turned out in recent years, The exact conditions for such an explosion are more complex than expected. There should be no white dwarves in the game. This is also indicated by the results of the study In the specialized magazine “The Astrophysical Journal Letters”.
As the team reports in the current post, a white dwarf absorbs mass from another white dwarf until it finally explodes in a kind of double detonation. First, the helium shell that surrounds the white dwarf is ruptured. It is said that this first explosion eventually led to the explosion of the carbon core. W: This type of supernova explosion would occur just below the mass limit of the Chandrasekhar boundary.
A supernova can help measure distances
Supernovae are cosmic explosions that come in many forms. If you wait for a huge star at the end of its evolution – like betel gemini – Explode, then this will be one Supernova On the other hand, the second type, a type Ia supernova, is based on a different star system: here, the burnt-out remains of low-mass stars, which consist mostly of only carbon and oxygen, explode. Even white dwarfs.
Astronomers and astrophysicists estimateفيزياء Type I supernovae Not only the celestial spectacle it presents, but also the fact that all of these supernovae should be exploding in a similar manner and thus across the universe with the same absolute brightness. You can use them as standard candlesthat allow cosmic distance measurements.
Previous simulations of such eruptions were based largely on simplification, that is, there is a local thermodynamic equilibrium. This equilibrium indicates, depending on the temperature and intensity of the radiation, for example the ratio of excited particles to unexcited particles. In the end, it is a matter of statistical distribution.