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S=A/4ℓP2S = A/4\ell_P^2

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where the second equality for a Schwarzschild hole follows directly from Hawking’s temperature formula [ 7 ] and S = A/4ℓP2\ell_P^2 is the Bekenstein-Hawking entropy [ 6 ] . For a solar-mass hole, β\beta ≈\approx 1.24×\times10^{-4}\,s\mathrm s and ln⁡\ln S ≈\approx 177 , giving t∗t_* ≈\approx 3.5\,ms\mathrm{ms} — an exact evaluation of the stated formulas, illustrative of the scrambling scale and not a claim about any particular measured hole.

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S=A/4ℓP2S = A/4\ell_P^2

Equation 65 · Evolutionary Physics

The Bit Comes Back Before the Bearing

This equation states an equality: the expressions on both sides have the same value under the article’s assumptions.

where the second equality for a Schwarzschild hole follows directly from Hawking’s temperature formula [ 7 ] and S = A/4ℓP2\ell_P^2 is the Bekenstein-Hawking entropy [ 6 ] . For a solar-mass hole, β\beta ≈\approx 1.24×\times10^{-4}\,s\mathrm s and ln⁡\ln S ≈\approx 177 , giving t∗t_* ≈\approx 3.5\,ms\mathrm{ms} — an exact evaluation of the stated formulas, illustrative of the scrambling scale and not a claim about any particular measured hole.

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