# Core mass lumosity relationship counseling

### spheroid luminosity relation: Topics by changethru.info

In this lesson, you will learn the important relationship between a main sequence star's mass and its luminosity as well as the relationship. This is usually referred to as the mass-luminosity relationship for Main the nuclear fusion reactions generate energy much faster, so the hotter the core, the . So, we have found that the mass-luminosity relation based on eclipsing binary .. Dividing our sample into core-Sersic and Sersic galaxies, we find that they are is crucial for the promising antitumour activity of doxorubicin-related therapy, .

The Australia Telescope Outreach and Education Web site Given our theory for the structure of stars, you can understand where this relationship comes from.

• Mass–luminosity relation

Stars on the Main Sequence must be using the energy generated via nuclear fusion in their cores to create hydrostatic equilibrium. The condition of hydrostatic equilibrium is that the pressure is balancing gravity. Since higher mass means a larger gravitational force, higher mass must also mean that higher pressure is required to maintain equilibrium.

If you increase the pressure inside a star, the temperature will also increase. So, the cores of massive stars have significantly higher temperatures than the cores of Sun-like stars.

### Mass–luminosity relation - Wikipedia

At higher temperatures, the nuclear fusion reactions generate energy much faster, so the hotter the core, the more luminous the star. If you actually look at the equations that govern stellar structure, you can derive from those equations that: L M n where the exponent varies a bit for stars of different masses, but, in general, is approximately equal to 3. Below is a plot that obeys this relationship and gives the theoretical calculations of a star's luminosity given its initial mass on the Main Sequence.

The metallicity Z is 0. Note that the present-day Sun is more luminous than when it first joined the main sequence.

## Astrophysics

This means that even a slight difference in the mass among stars produces a large difference in their luminosities. For example, an O-type star can be only 20 times more massive than the Sun, but have a luminosity about 10, times as much as the Sun. Putting together the principle of hydrostatic equilibrium and the sensitivity of nuclear reaction rates to temperature, you can easily explain why.

Massive stars have greater gravitational compression in their cores because of the larger weight of the overlying layers than that found in low-mass stars. The massive stars need greater thermal and radiation pressure pushing outward to balance the greater gravitational compression.

The greater thermal pressure is provided by the higher temperatures in the massive star's core than those found in low-mass stars.

### The Mass-Luminosity Relationship | Astronomy Planets, Stars, Galaxies, and the Universe

Massive stars need higher core temperatures to be stable! The nuclear reaction rate is very sensitive to temperature so that even a slight increase in temperature makes the nuclear reactions occur at a MUCH higher rate.

This means that a star's luminosity increases a lot if the temperature is higher. This also means that a slight increase in the mass of the star produces a large increase in the star's luminosity. Mass Cutoff Explained The principle of hydrostatic equilibrium and nuclear fusion theory also explain why stars have a certain range of masses.

The stars have masses between 0. Stars with too little mass do not have enough gravitational compression in their cores to produce the required high temperatures and densities needed for fusion of ordinary hydrogen. The lowest mass is about 0. A star less massive than this does not undergo fusion of ordinary hydrogen but if it is more massive than about 13 Jupiters it can fuse the heavier isotope of hydrogen, deuterium, in the first part of its life.

## The Mass-Luminosity Relationship

Stars in this boundary zone between ordinary stars and gas planets are called brown dwarfs. After whatever deuterium fusion it does while it is young, a brown dwarf then just slowly radiates away the heat from that fusion and that is left over from its formation.

Among the first brown dwarfs discovered is the companion orbiting the star Gliese