A likely progenitor of a Type Ia supernova is a white dwarf star in a binary system, accreting material from a companion star until it reaches a critical mass, triggering a thermonuclear explosion.
A Type Ia supernova is created by the merger of two white dwarfs. This type of supernova occurs when the combined mass of the white dwarfs exceeds a critical limit, leading to a thermonuclear explosion that destroys the star.
Type Ia supernovae [See Link] follow a characteristic light curve. This luminosity is generated by the radioactive decay of certain elements. The peak luminosity of the light curve was believed to be consistent across Type Ia supernovae as having a maximum absolute magnitude of about -19.3. This would allow them to be used as a secondary "standard candle" [See Link] to measure the distance to their host galaxies
A supernova can't occur on any planet. A supernova occurs when a very large star, at least 8 times more massive than the sun dies.
Betelgeuse is expected to end its life in a supernova explosion, likely as a Type II supernova due to its massive size and age. This type of supernova occurs when a massive star exhausts its nuclear fuel and collapses under its own gravity.
SN 1572 or Tycho's Supernova was a supernova type Ia, in the constellation Cassiopeia
A likely progenitor of a Type Ia supernova is a white dwarf star in a binary system, accreting material from a companion star until it reaches a critical mass, triggering a thermonuclear explosion.
A Type Ia supernova is created by the merger of two white dwarfs. This type of supernova occurs when the combined mass of the white dwarfs exceeds a critical limit, leading to a thermonuclear explosion that destroys the star.
It becomes a Type Ia supernova [See Link]
Supernova Ia?
Type Ia supernovae [See Link] follow a characteristic light curve. This luminosity is generated by the radioactive decay of certain elements. The peak luminosity of the light curve was believed to be consistent across Type Ia supernovae as having a maximum absolute magnitude of about -19.3. This would allow them to be used as a secondary "standard candle" [See Link] to measure the distance to their host galaxies
Very few stars have a mass above the Chandrasekhar limit of about 1.4 solar masses. Stars accumulate matter from gas clouds and companion stars. Most stars will become white dwarves in time. When their mass reaches the Chandraskhar limit, a type Ia supernova occurs. This generates enough raw materials to create about half a million planets with large iron cores and thick surface oceans. The primary elements produced by a type Ia supernova are oxygen, silicon and iron. In summary, the building blocks of future planets match the composition of type Ia supernova ejecta.
A supernova can't occur on any planet. A supernova occurs when a very large star, at least 8 times more massive than the sun dies.
Betelgeuse is expected to end its life in a supernova explosion, likely as a Type II supernova due to its massive size and age. This type of supernova occurs when a massive star exhausts its nuclear fuel and collapses under its own gravity.
A supernova occurs when a star exhausts its nuclear fuel, typically hydrogen and helium, leading to a collapse under its own gravity. In the case of a massive star (Type II supernova), the core collapses after fusing heavier elements up to iron, which cannot produce energy through fusion. For a white dwarf (Type Ia supernova), it accumulates material from a companion star until it reaches a critical mass and undergoes a thermonuclear explosion. Thus, the "fuel" for a supernova is the remnants of nuclear fusion processes in a star's life cycle.
Supernovas [See Link] are classified according to the absorption lines of different chemical elements that appear in their spectra. The classification can be simplified to Type I or Type II Type II - If a supernova's spectrum contains a line of hydrogen in the visual portion of the spectrum. Type I - all the rest. These are broken down even further. Type:- Ia - When a white dwarf merges with another star. Ib & Ic are formed by massive stars running out of fuel but have lost the outer layer of hydrogen and helium like Wolf-Rayet stars Type II are the "normal" types of supernova, where massive stars can no longer maintain hydrostatic equilibrium and the core collapses IIP Reaches a "plateau" in its light curve IIL Displays a "linear" decrease in its light curve Supernova [See Link] classifications are based on chemical composition.
A Chandrasekhar mass is the maximum mass limit (about 1.4 times the mass of the Sun) that a white dwarf star can have before it collapses under its own gravity and triggers a supernova explosion. When a white dwarf accretes matter from a companion star or merges with another white dwarf, exceeding the Chandrasekhar mass, it can collapse and explode as a Type Ia supernova.