Answer:
The period of orbit in an eclipsing binary system can be determined by measuring the time interval between successive eclipses. This interval is then used to calculate the period of the binary system. Additionally, the radial velocity of the stars can also be used to detect binary stars and measure their orbital period.
Step-by-step explanation:
- A star follows a predictable path of evolution that can be divided into stages. These stages are determined by the star's mass and the amount of fuel left in its core.
- The first stage is the Protostar stage. During this stage the star is composed of gas and dust that is undergoing gravitational collapse. As the gas and dust collapses, it begins to heat up and eventually forms a protostar.
- The second stage is the Main Sequence stage. During this stage a star has reached equilibrium between the outward pressure of its core and the inward pull of its gravity. This is the longest stage of a star's life and is where most of the star's energy is produced.
- The third stage is the Red Giant stage. During this stage a star has exhausted its hydrogen fuel in its core and starts to cool. As the star cools, it begins to expand and becomes a red giant.
- The fourth stage is the White Dwarf stage. During this stage the star has shed most of its outer layers and has become a small, dense star. This stage is the final stable stage of a star's life and is the remnant of the star.
- The fifth stage is the Supernova stage. During this stage a star undergoes a catastrophic explosion and is typically the end of a star's life. This stage is only observed in the most massive stars.
- Finally, the sixth stage is the Neutron Star or Black Hole stage. During this stage a star has collapsed and become either a neutron star or a black hole. This is the final stage of a star's life and is typically only observed in the most massive stars.