The mass could either be a red giant or a super giant, they both evolve into different ways, after a star runs out of fuel, it becomes a white dwarf, a neutron star, or a black hole.
The mass of a star determines its fate in the end stages of its life. Higher-mass stars will undergo a more violent explosion called a supernova, leaving behind a dense core known as a neutron star or black hole. Lower-mass stars will shed their outer layers, forming a planetary nebula, and eventually cool down to become a white dwarf.
The mass could either be a red giant or a super giant, they both evolve into different ways, after a star runs out of fuel, it becomes a white dwarf, a neutron star, or a black hole.
The mass could either be a red giant or a super giant, they both evolve into different ways, after a star runs out of fuel, it becomes a white dwarf, a neutron star, or a black hole.
As stars burn, they shed matter, becoming less massive slowly throughout their life cycle. This reduction in mass necessarily lessens their gravity, causing the stars' diameter to increase. So, many end-stage stars will be huge and bloated. Massive red giant stars are examples of this.
well the relationship between mass and force is..........*relationship... Force=mass x acceleration
No, not all stars go through all stages of stellar evolution. The evolutionary path of a star depends on its mass. Low-mass stars like the Sun will go through stages like main sequence, red giant, and white dwarf, while high-mass stars can go through stages like supernova and neutron star or black hole formation.
Describe the relationship between mass and weight.
The relationship between acceleration and mass is that acceleration is inversely proportional to mass. This means that as mass increases, acceleration decreases, and vice versa.
The radius of a star is generally proportional to its mass. More massive stars tend to have larger radii compared to less massive stars. This relationship is governed by the balance between the gravitational force pulling the star inward and the pressure from nuclear fusion reactions pushing outward.
The mass could either be a red giant or a super giant, they both evolve into different ways, after a star runs out of fuel, it becomes a white dwarf, a neutron star, or a black hole.
There is no simple relation. The color does not depend only on the mass. The same star can change color, without a significant change in mass. For example, our Sun is currently yellow; in a few billion years, it is expected to get much larger, becoming a red giant. However, if we limit the sample of stars to those on the "main sequence" of the "HR diagram", there is something of a relation between mass and color. The most massive stars are blue or white. They are also hottest and most luminous. The least massive are the red dwarf stars, which are relatively cool and dim. Our Sun, which is a "main sequence" star at present, is somewhere in between those extremes. (There is a strong relationship between mass and luminosity for main sequence stars. The HR diagram, of course, shows there is a relationship between luminosity and color for the main sequence stars.)
Main sequence stars best obey the mass-luminosity relation. This empirical relation states that there is a direct relationship between a star's mass and its luminosity. In general, the more massive a main sequence star is, the more luminous it will be.