04.06.2013 Views

Gravity and Strings

Gravity and Strings

Gravity and Strings

SHOW MORE
SHOW LESS

Create successful ePaper yourself

Turn your PDF publications into a flip-book with our unique Google optimized e-Paper software.

8.1 Coupling a scalar field to gravity <strong>and</strong> no-hair theorems 217<br />

F µ =∇ µ ϕ.Aswill be explained later for the electric charge, this is just the continuity<br />

equation for the current F µ <strong>and</strong> suggests the definition of scalar charge<br />

<br />

d 3 µ∇ µ ϕ, (8.12)<br />

V<br />

which will be locally conserved. The conservation of this current is associated via Noether’s<br />

theorem with the invariance of the action under constant shifts of the scalar.<br />

Second, the Bianchi-type identity ∂[µ∂ν]ϕ = 0can be rewritten in the form ∇µF µνρ = 0,<br />

where we have defined the completely antisymmetric tensor F µνρ = (1/ √ |g|)ɛ µνρσ ∂σ ϕ.<br />

With this definition it is possible to show that the line integral<br />

1<br />

3!<br />

<br />

d<br />

γ<br />

1 µνρ F µνρ =<br />

<br />

γ<br />

dϕ, (8.13)<br />

along the curve γ is conserved. Observe that, if γ is closed, the integral will only be different<br />

from zero if ϕ is multivalued, for instance if ϕ is an axion (a pseudoscalar) that takes values<br />

in a circle.<br />

How should we interpret these charges? We will see later in this chapter that the electromagnetic<br />

field Aµ has a natural coupling to the worldline of a particle with electric charge<br />

q given by Eq. (8.53). The particle’s electric charge is given by the surface integral over a<br />

sphere S 2 of the Hodge dual of the electromagnetic-field-strength 2-form Fµν. The particle’s<br />

magnetic charge is given by the surface integral over a sphere S 2 of the electromagneticfield-strength<br />

2-form. The electric charge is conserved due to the equation of motion <strong>and</strong><br />

the magnetic charge is conserved due to the Bianchi identity. A topologically nontrivial<br />

configuration of the field is needed in order to have magnetic charge.<br />

Potentials that are differential forms of higher rank couple to the worldvolumes of extended<br />

objects: a (p + 1)-form potential A(p+1) naturally couples to p-dimensional objects<br />

with a (p + 1)-dimensional worldvolume (we will explain how this comes about in Chapter<br />

18). The electric charge is the integral over the sphere S d−(p+2) transverse to the object’s<br />

worldvolume of the Hodge dual of the (p + 2)-form field strength F(p+2) = dA(p+1). The<br />

magnetic charge would be the electric charge of the dual (d − p − 4)-dimensional object,<br />

charged under the dual potential whose field strength is the Hodge dual of F(p+2).<br />

Looking now at the above charges, we immediately realize that the charge defined in<br />

Eq. (8.13) is the charge of a one-dimensional object (string) <strong>and</strong> the former Eq. (8.12) is<br />

the charge of a “−1-dimensional object.” Such an object would be an instanton, defined in<br />

Euclidean space <strong>and</strong> with zero-dimensional worldvolume. Then “charge conservation” is<br />

not a concept to be applied to it. In both cases ϕ has to be a pseudoscalar.<br />

Observe that, indeed, a line integral as Eq. (8.13) cannot measure a point-like charge because<br />

we could continuously contract the loop γ to a point without meeting the singularity<br />

at which the charge rests. The line integral has to have a non-vanishing linking number<br />

with the one-dimensional object, which has to have either infinite length or the topology of<br />

S 1 ; otherwise the integral would be zero by the same argument. The behavior of the scalar<br />

field has to be ϕ ∼ ln ρ, where ρ measures the distance to the one-dimensional object in the<br />

two-dimensional plane orthogonal to it.<br />

Similar arguments apply to the definition Eq. (8.12) <strong>and</strong> ϕ ∼ 1/ρ 2 , where now ρ measures<br />

the distance to the instanton in the four-dimensional Euclidean space.

Hooray! Your file is uploaded and ready to be published.

Saved successfully!

Ooh no, something went wrong!