c. a. Just below the surface of the Sun the temperature is hot enough to have fr

Question

c.

a. Just below the surface of the Sun the temperature is hot enough to have free electrons. The free electrons radiate, producing a continuous spectrum. At the very outer edge of the Sun the temperature is low enough to have bound electrons. These electrons absorb specific energies of light causing the dark lines to appear on the continuous spectrum. In the hot star, which has only a continuous spectrum, it must be the case that there are no elements in the star. The high temperature must have destroyed all elements and turned them into pure energy. That is also why the hot star is more luminous.

Explanation / Answer

first option is correct

Just below the surface of the Sun the temperature is hot enough to have free electrons.

The free electrons radiate, producing a continuous spectrum.

At the very outer edge of the Sun the temperature is low enough to have bound electrons.

These electrons absorb specific energies of light causing the dark lines to appear on the continuous spectrum.

In the hot star, which has only a continuous spectrum,

it must be the case that there are no elements in the star.

The high temperature must have destroyed all elements and turned them into pure energy.

That is also why the hot star is more luminous.

because

here absorption spectrum of the sun called as Fraunhofer lines

and

these are appear that an electron at the photosphere which relatively colder,

and these are cold like inner electrons

and

absorbs perticular wavelengths..

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