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An arc second is a measure of angular separation, not of distance. It is therefore an inappropriate unit for measuring the distance to a star.
Use a protractor.Use a protractor.Use a protractor.Use a protractor.
red and yeller
The device that astronomers use to find the angle between the horizon and stars in the sky is called a sextant.
A star's luminosity is the measure of the total energy radiated by the star in one second.
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Luminosity is the total amount of energy emitted by a star per second.
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 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.
Two properties used to characterize a star are its luminosity, which is a measure of the total amount of energy it emits per unit of time, and its temperature, which influences its color and spectral type. These properties are essential for understanding a star's energy output and life cycle.
A supernova is the catastrophic death of a star, characterized by a massive output of energy.
The form of measurement that can be defined as the rate at which a star gives off energy is luminosity. Luminosity is measured in watts and indicates the total amount of energy emitted by a star per unit time.
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 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.
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.
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.