What is the Chandrasekhar limit?

Limit Chandrasekhar is an important value in astrophysics. It is a weight limit in which the non -rotating astral body can no longer be supported by the pressure of electron shells in its atoms and there is a gravitational collapse. The Chandrasekhar limit is approximately 1.4 solar masses or 2.85 x 10 kg. The use of the Chandrasekhar limit is essential in the analysis of the development and extinction of the stars. During the normal life of the star, the pressure out of nuclear reactions counteracts the contractual force of gravity. Finally, he uses all his hydrogen fuel and leaves the main sequence. It's all downhill. The star combines heavier and heavier cores until it reaches the temperature and density in its core to combine anything more, or the core turns on iron, which is the most difficult fusion product that cannot be fused to produce more energy.

During the turbulent last millions of years of their lives, many stars throw most of their matter in the form of solar wind and leave a much smaller core behind. If the core has less HMOYou create a white dwarf, a body of ground, but with a matter similar to the sun. If it is more weight than the Chandrasekhar limit, it collapses to create a neutron star or a black hole, a process with the potential to initiate a supernum.

Neutron star is the aggregation of matter with such a high density that it usually consists only of neutrons pushed directly. Negatively charged electrons and positively charged protons combine and create neutrons of neutrons, which creates the whole thing in the star. The neutron star weighs more than our sun, but only the size of the city with a diameter of about 20 km.

The hardest star -pack is formed black holes, zero volume points and endless density. These objects are adored fans of sci -fi and theoring physics.