Neutron star collisions can help solve the Hubble constant crisis. The Hubble constant describes the rate of expansion of the universe. The collision of neutron stars can help resolve the crisis because astronomers can analyze the collision to better understand the inconsistency between different measurements of the Hubble constant. 

Astronomers can analyze neutron star collisions by: 

• Listening to how loud the collision is and how the sound changes over time 
• Detecting electromagnetic light from the collision and using redshift to determine how fast the merged stars are receding 

When neutron stars collide, they create perfectly spherical “kilonova” explosions. The stars merge and collapse to form a black hole, while throwing out fragments that produce a perfectly spherical fireball of blue and red. 

Neutron star collisions can also emit up to 100 times more heavy metals than when neutron stars smash into black holes.

When two neutron stars collide, they merge and collapse to form a black hole. The collision is called a kilonova, and it’s one of the most powerful explosions in the universe. The stars move at 100 million meters per second. 

The collision produces a perfectly spherical fireball of blue and red. The fragments of the collision are thrown out. 

The combined mass of the two neutron stars causes the newly formed object to gravitationally collapse further, turning into a black hole. For a short period of time before this happens, the object can become a hypermassive neutron star with an extremely powerful magnetic field. 

Astronomers first detected the collision of two neutron stars on August 17, 2017. They caught the cosmic smashup using both gravitational waves and light. 

The difference between a neutron star and a black hole is the mass of the star’s core. If the core is less than three solar masses, it remains a neutron star. If the core is more than three solar masses, it collapses further to form a black hole. 

The difference is whether or not the stellar core has sufficient gravity to overcome neutron degeneracy pressure. The remnant isn’t massive enough to overcome the pressure exerted by neutrons, so huge stars become neutron stars. However, humongous stars leave remnants capable of overcoming even this pressure, and they collapse into singularities. 

Most of the black holes that we know about have masses above 5 solar masses, whereas all of the neutron stars have mass below 2.5 solar masses

A star’s fate is determined by its mass. Stars with masses between 0.08 and 8 times the mass of the Sun will become white dwarfs. Stars with masses between 8 and 20 times the mass of the Sun will become supergiants. Stars with masses more than 20 times the mass of the Sun will become black holes. 

Stars that are more massive than 8 solar masses will become neutron stars or black holes when they reach the end of their lives. 

Supermassive stars, which have an initial mass greater than about eight times that of the Sun, have the capacity to eventually become neutron stars. 

Extremely heavy stars (more than 25 times heavier than the Sun) have no means to withstand their own gravity as they die. They collapse completely to a black hole. 

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