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.
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.
The critical temperature for nuclear fusion in a star's core is around 10 million degrees Celsius. At this temperature, hydrogen nuclei can overcome their mutual repulsion and fuse to form helium, releasing energy in the process. This energy production is what causes a star to shine.
When the temperature in the core reaches 10 million degrees Kelvin.
The temperature of an expanding star can vary depending on its size and stage of evolution. Generally, as a star expands, its surface temperature decreases due to the increased surface area over which the energy is distributed. However, the core temperature of the star can increase as it undergoes fusion reactions.
Temperatures in the star's core can reach 3x109 K.
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.
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 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.
The temperature at which hydrogen fuses is 10,000,000 degrees Kelvin. This is the minimum temperature the core of a proto star has to have to become a true star.
The star with a surface temperature closest to the boundary between Earth's mantle and core would be the Sun, with a surface temperature of about 5,500 degrees Celsius. The temperature at the boundary between Earth's mantle and core is estimated to be around 3,000-4,000 degrees Celsius.
actually, it depends on the color of it's chromosphere. as you get deeper into a star, it may change color due to it's temperature, but what you see on the outside would be a different color. The chromosphere would hide the inner core of the star.
In a newborn star, the fusion reactions occur primarily in its core, where the temperature and pressure are high enough to trigger nuclear fusion. This process generates the energy that powers the star and allows it to shine bright.
Basically, the amount of hydrogen (mass). The more mass a star has, the greater the pressure in the core. The greater the pressures in the core, the higher the temperature, the higher the temperature, the hotter the star will be, the hotter the star, the blighter the envelope will be.