0:00A supernova is a cataclysmic explosion
0:02that occurs at the end of life
0:03of a high-mass star.
0:05The mass of a star
0:06refers to the amount of matter contained in it.
0:09and is one of the most important factors
0:10that determine their evolution and behavior.
0:13Supernovae
0:14are generated from high-mass stars,
0:17which
0:17are significantly larger than that of the sun,
0:20from 9 times the mass of the sun.
0:23High-mass stars
0:24form from molecular clouds
0:26and giant molecular clouds,
0:28which are clouds of interstellar gas and dust.
0:31These clouds fragment into small parts
0:34and due to fragmentation
0:36and together with an external compression event,
0:39creation begins under the influence of gravity.
0:42If the mass accumulated in the core
0:44exceeds a critical threshold,
0:46nuclear fusion begins
0:47and the star begins to shine.
0:49High-mass stars are hotter
0:51and more luminous than low-mass stars.
0:54They also have shorter lives
0:56because they deplete their nuclear fuel
0:58more quickly.
1:00As a high-mass star
1:02consumes hydrogen
1:03at its core,
1:03begins to fuse elements such as helium,
1:07carbon,
1:08and so on until reaching the castle.
1:11When a massive star runs out of fuel,
1:14its central core is compressed
1:16under the influence of its own gravity.
1:18Collapse in the core
1:20is detained
1:20by neutron degeneration pressure,
1:23on degeneration
1:24is similar to the concept of electronic degeneration
1:27that occur white dwarfs,
1:29but in this case,
1:30neutrons
1:31are those subject to degeneracy pressure.
1:35prevents further collapse of the material
1:37in the core of a star
1:39and counteracts the force of gravity.
1:41This means
1:42that a star can maintain its structure
1:44compact and stable
1:46with an incredibly high rating.
1:48The explosion of a supernova
1:50is due to the fact that
1:51the densest part of the star's core
1:53sinks in less than a second,
1:55while the outer zone collapses
1:57at a speed of 60 000km/s,
2:00which is approximately
2:0120 percent of the speed of light.
2:04When the accreted material reaches the center
2:06neutron degenerate,
2:07a rebound occurs
2:09and matter is expelled outwards.
2:11At the same time,
2:12a shock wave is generated
2:14traveling at a speed of 10 000km/s.
2:17The explosion of a supernova is so intense that
2:19for a short period of time,
2:21the star
2:22can become brighter than an entire galaxy.
2:26plays a decisive role in its final destination,
2:29as gravity is the dominant factor
2:31during the collapse.
2:33If the original star does not have sufficient mass,
2:35neutron degeneration pressure
2:38can counteract gravity
2:39and maintain a stable neutron star.
2:42However,
2:43if the mass is large enough,
2:45gravity becomes so intense
2:47that no known force can
2:49Preventing the star from collapsing into a black hole