Other Functions
![[Graphics:Images/index_gr_46.gif]](hawk_Images/index_gr_46.gif)
Using this relation, we can construct further relations--all of which are quite simple. First we start with the luminosity-time relation.
![[Graphics:Images/index_gr_47.gif]](hawk_Images/index_gr_47.gif)
By simply plugging in the mass-time relation for the value of M we get a luminosity-time relation.
![[Graphics:Images/index_gr_48.gif]](hawk_Images/index_gr_48.gif)
By simply plugging in all constants we then get the luminosity as a function of time
![[Graphics:Images/index_gr_49.gif]](hawk_Images/index_gr_49.gif)
![[Graphics:Images/index_gr_56.gif]](hawk_Images/index_gr_56.gif)
Where L is a function defined by
![[Graphics:Images/index_gr_57.gif]](hawk_Images/index_gr_57.gif)
To simplify we can rewrite the constant as K
![[Graphics:Images/index_gr_58.gif]](hawk_Images/index_gr_58.gif)
Thus providing us with
![[Graphics:Images/index_gr_59.gif]](hawk_Images/index_gr_59.gif)
Pulling out the constant yields
![[Graphics:Images/index_gr_60.gif]](hawk_Images/index_gr_60.gif)
And taking the derivative gives us
![[Graphics:Images/index_gr_61.gif]](hawk_Images/index_gr_61.gif)
Reducing to
![[Graphics:Images/index_gr_62.gif]](hawk_Images/index_gr_62.gif)
But we take away the negative sign because we know that this energy is the energy released by the blackhole. Plugging in K finally gives us
![[Graphics:Images/index_gr_63.gif]](hawk_Images/index_gr_63.gif)
![[Graphics:Images/index_gr_50.gif]](hawk_Images/index_gr_50.gif)
Plug in the function describing the mass of the blackhole
![[Graphics:Images/index_gr_51.gif]](hawk_Images/index_gr_51.gif)
Then plug in constants and reduce to form
![[Graphics:Images/index_gr_52.gif]](hawk_Images/index_gr_52.gif)
![[Graphics:Images/index_gr_53.gif]](hawk_Images/index_gr_53.gif)
Input the mass as a function of time
![[Graphics:Images/index_gr_54.gif]](hawk_Images/index_gr_54.gif)
Then reduce constants and obtain the relation
![[Graphics:Images/index_gr_55.gif]](hawk_Images/index_gr_55.gif)