A star has a mass of approximately 1.21.21.2 times that of the Sun.
Describe how the position of this star on a Hertzsprung-Russell (H-R) diagram changes as it evolves from the main sequence to the end of its life cycle.
The diagram below shows a blank H-R diagram on the left, and the relative intensity of light against wavelength for this star on the right.
Explain how the stellar spectrum can be used to determine the surface temperature of the star, and how this helps in identifying its evolutionary stage. Discuss the limitations of relying solely on this spectral data.
