Reference: Moore, Thomas A., *A General Relativity Workbook*, University Science Books (2013) – Chapter 16; Problem P16.5.

We’ve seen that a temperature can be defined for a black hole that radiates particles (mainly photons) due to quantum pair creation:

This is the temperature as seen by an observer at infinity. If we take the temperature to be proportional to the observed energy of the emitted particles, we can get the temperature as measured by an observer at rest at some finite distance from the black hole. The energy of the photons is

where is the energy at infinity. Using the proportionality of and , we get

The temperature thus becomes infinite at . For a solar mass black hole, we have

We have to get extraordinarily close to a black hole to see the temperature rise significantly. Solving 3 for we get

For example, if we want (around room temperature), then

Since , we need to approach to within of the event horizon. This is smaller than the radius of a proton (around ).

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Chris KranenbergEq. 6 value of 8.46 x 10^-20 is off by a factor of 2. The calculated value when T(infinity) = 6.17 x10^-8 (one solar mass blackhole) is 4.23 x 10^-20.

growescienceFixed now. Thanks.