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String Theory and M-Theory

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568 Black holes in string theory<br />

The five-dimensional metric describing this black-hole can be obtained<br />

from the ten-dimensional type IIB theory by wrapping the corresponding<br />

branes as described above, or it can be constructed directly. In either case,<br />

the resulting metric can be written in Einstein frame in the form<br />

ds 2 = −λ −2/3 dt 2 + λ 1/3 dr 2 + r 2 dΩ 2 3 , (11.46)<br />

where<br />

λ =<br />

3<br />

i=1<br />

<br />

1 +<br />

<br />

ri<br />

2<br />

. (11.47)<br />

r<br />

The relation between the parameters ri <strong>and</strong> the charges Qi is derived below.<br />

This solution describes an extremal three-charge black hole with a vanishing<br />

temperature T = 0. Note that this formula reduces to the extremal<br />

Reissner–Nordström black-hole metric given in Eq. (11.32) in the special<br />

case r1 = r2 = r3, that is, when the three charges are equal. The dilaton<br />

is a constant, so there is a globally well defined string coupling constant gs.<br />

Thus, the string-frame metric differs from the one given above only by a<br />

constant factor.<br />

The horizon of the black hole in Eq. (11.46) is located at r = 0, <strong>and</strong> its<br />

area is<br />

A = 2π 2 r1r2r3. (11.48)<br />

This vanishes when any of the three charges vanishes, which is the reason<br />

that three charges have been considered in the first place. Put differently,<br />

one needs to break 7/8 of the supersymmetry in order to form a horizon<br />

that has finite area in the supergravity approximation, <strong>and</strong> this requires<br />

introducing three different kinds of excitations. When there is only one or<br />

two nonzero charges, there still is a horizon of finite area, but its dependence<br />

on the string scale is such that its area vanishes in the supergravity<br />

approximation. For the supergravity approximation to string theory to be<br />

valid, it is necessary that the geometry is slowly varying at the string scale.<br />

This requires ri ≫ ℓs.<br />

The black hole mass<br />

Using Eq. (11.11) one can read off the mass of the black hole M to be<br />

M = M1 + M2 + M3 where, Mi = πr2 i<br />

4G5<br />

. (11.49)<br />

The fact that the masses are additive in this way is a consequence of the<br />

form of the metric. However, this had to be the case, because the BPS<br />

condition is satisfied, <strong>and</strong> the charges are additive.

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