The study, led by Patrick Valery (Patrick Vallely), a graduate student at Ohio State University, eventually published a new discovery of supernova observations using TESS and provided new insights into elements left behind by white dwarfs exploding into supernova. Supernova classification can be confusing. For simplicity and simplicity, we will discuss type II and type Ia supernova.
Type II supernovae are those giant stars (eight or more times the mass of the sun) that collide and explode on themselves. Type Ia supernovae involve smaller stars in the near-binary system (two stars are wound around each other) Orbital), at least one of which is a white dwarf. The white dwarf is a dying star that has burned all the fuel (usually leaving only carbon and oxygen), but it is still very hot. It is also very very dense (imagine the quality of our sun, compressed to the size of the earth). However, when a white dwarf is in a tight binary system with another star, it can have a more dramatic ending, in which case a type Ia supernova can be produced, when the white dwarf takes its mass and energy from its star partner. Become too big to stay stable and eventually explode.
Although white dwarfs do not have any remaining hydrogen, their companion stars usually do, which means there should be hydrogen (and other things) in the spectrum. So far, scientists have never seen it. TESS's observation changed everything, finding that a supernova was actually a collision between two white dwarfs, and theoretically there shouldn't be any hydrogen in the spectrum, so where did the observed hydrogen come from? According to Professor Chris Stank, co-author of the paper, hydrogen may have come from a third party cut into a binary system, and he said, based on the curve observed by TESS, they believe that the hydrogen element may come from the third star in the system.