The high-mass star enters a phase called "core helium burning" where energy production in the core increases due to the fusion of heavier elements such as helium into carbon and oxygen. The increase in energy production counterbalances the higher energy loss through radiation, maintaining a relatively constant luminosity. This equilibrium regulates the star's luminosity despite the increased energy output.
At a higher temperature, the star will shine more brightly for each square meter of surface. The total luminosity per square meter is approximately proportional to the fourth power of its absolute temperature. This refers to the energy output, considering all types of electromagnetic waves, not just visible light.
Energy output, as absolute brightness (magnitude) is taken at a standard distance of 10 parsecs.
A blue star is hotter than a red star. The color of a star indicates its surface temperature, with blue stars having temperatures exceeding 10,000 degrees Celsius, while red stars typically have temperatures around 2,500 to 3,500 degrees Celsius. The higher energy output and temperature of blue stars result from their larger mass and more intense nuclear fusion processes occurring in their cores.
The idea is that a larger star may be cooler - emit less energy per square meter of surface. The total energy emitted is equal to the surface area, multiplied by the energy emitted per unit area.
heat
The energy output of a star comes from its core, where nuclear fusion reactions take place. During fusion, hydrogen atoms combine to form helium, releasing a tremendous amount of energy in the process.
The surface temperature is not a reliable indicator about how long a star will last. However, the total energy output is. If a star produces a lot of energy, it will burn through its fuel faster.
The same as everywhere else. Every mass has associated energy. Every energy has associated mass. Possibly this question is about the energy output of stars. Usually, the more mass a star has the higher its rate of energy output.
A supernova is the catastrophic death of a star, characterized by a massive output of energy.
Ankaa, the brightest star in the Phoenix constellation, has a surface temperature of approximately 7,400 degrees Celsius (13,352 degrees Fahrenheit). This high temperature is due to the intense nuclear reactions happening in its core, which sustain the star's brightness and energy output.
Energy in a star's core is generated through nuclear fusion, where hydrogen atoms combine to form helium releasing a massive amount of energy in the process. The extreme temperature and pressure in the core of a star make this fusion process possible, sustaining the star's energy output.
The measure of energy output from a star per second is referred to as its luminosity. Luminosity is typically expressed in watts (W) or in terms of the Sun's luminosity, denoted as L☉. This value quantifies the total amount of energy radiated by the star across all wavelengths in a given time period, reflecting its intrinsic brightness.
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 temperature of a yellow star's photo sphere is hotter than that of and orange star. However the total energy output of an orange star may be greater than that of a yellow star.
The star with the highest surface temperature is the blue star called O-type stars. These stars can have surface temperatures exceeding 50,000 degrees Celsius.
As a star exhausts its hydrogen fuel and increases in temperature and pressure, it needs to start fusing helium to produce energy and maintain equilibrium against the inward force of gravity. This process is necessary to sustain the star's energy output and prevent collapse.