The star's mass determines the temperature in its core. A stars mass will also determined it size and the amount of gravitational pull it will have.
The temperature determines the color of the star!:)
The core of a star is primarily responsible for determining its temperature, luminosity, and diameter. In the core, nuclear fusion occurs, generating immense heat and energy, which influences the star's overall temperature and luminosity. Additionally, the balance between the inward gravitational force and the outward pressure from fusion reactions dictates the star's size or diameter. Thus, the processes and conditions within the core play a crucial role in defining these key characteristics of a star.
A star becomes a star - "is born" - when the process of nuclear fusion begins in the core of the star.
Mainly its temperature.
Temperatures in the star's core can reach 3x109 K.
The temperature of the core of a star can reach millions of degrees Kelvin due to nuclear fusion reactions that generate immense heat and light. This intense heat and pressure in the core are what sustain a star's energy output.
Depends on the age of the neutron star. As a neutron star no longer has any method to produce heat, it will slowly cool over time. A young neutron star will have a core temperature of about 106 kelvin.
The temperature in the core of a star is determined by the balance between the force of gravity compressing the gas and the nuclear fusion reactions happening inside the core. The energy released from these fusion reactions generates heat and maintains a high core temperature.
The temperature in the core of a star depends, to a great extent, on:* The star's mass. The general tendency is that high-mass stars are hotter. * Where the star is in its life cycle. The star's core temperature will vary over time. On the other hand, the star's surface temperature also depends on its size. Thus, it is possible that PRECISELY because a star is hotter in the core, it gets bigger, and the surface temperature DECREASES (though its total energy output increases).
The core.
If the core temperature of a star decreases, it will contract, causing the core to become denser. This contraction may lead to an increase in temperature in the outer layers, causing the star to expand its radius to re-establish equilibrium.
The rate of nuclear fusion in a star is highly sensitive to its core temperature, typically following the relationship that fusion rates increase sharply with temperature. For a rough estimate, the rate of fusion can be proportional to (T^4) to (T^{10}), depending on the specific fusion process. If star B's core temperature is three times that of star A (3T), the fusion rate in star B would be significantly higher—potentially up to 81 to 1000 times greater than that of star A, depending on the exact exponent used in the temperature dependence. Thus, star B's fusion rate would be dramatically greater than star A’s.