White dwarfs are found at the lower-left corner of the H-R diagram, characterized by high temperature and low luminosity. They have extremely high densities due to their small sizes. White dwarfs are the end state of low-mass stars and emit a bluish-white color due to their high surface temperatures.
The area of the diagram that represents the white dwarfs is at the lower-left corner of the H-R (Hertzsprung-Russell) diagram. These stars have a unique combination of high temperature and low luminosity, indicating that they are very hot but also very small in total surface area. Not to be confused with faint red main-sequence stars or brown dwarfs, white dwarfs are characterized by their extremely high density and comparatively small size.
According to the works of Indian-American astrophysicist Subrahmanyan Chandrasekhar, white dwarfs have electron-degenerate cores that prevent further contraction, leading to their small, dense state. These stars are the likely end state of low-mass stars. Despite having high surface temperatures, their bluish-white appearance is due to the blending of the colors of the electromagnetic radiation they emit.
In conclusion, white dwarfs occupy a specific area in the H-R diagram that reflects their high temperature and low luminosity, a result of their small size and massive density.