 Stringy Things

# Notes on string theory: NG action – equations of motion, Dp-branes, and the slope parameter

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In the last entry we explored the relativistic string and arrived at the Nambu-Goto action,

[ S_{NG} = – frac{T_0}{c} int_{tau_i}^{tau_f} d tau int_{0}^{sigma_1} dsigma sqrt{(dot{X} cdot X^{prime^2}) – dot{X}^2 X^{prime^{2}}} ]

[ implies mathcal{L} (dot{X}^{mu}, X^{prime mu}) = – frac{T_0}{c}
sqrt{(dot{X} cdot X^{prime^2}) – dot{X}^2 X^{prime^2}} ]

Equations of motion

We can obtain the EoM by setting the variation of the action equal to 0. So, we vary the action

[ delta S = int_{tau_i}^{tau_f} d tau int_{0}^{sigma_1} dsigma [frac{partial mathcal{L}}{partial dot{X}^{mu}} frac{partial (delta X^{mu})}{partial tau} + frac{partial mathcal{L}}{partial X^{mu prime}} frac{partial (delta X^{mu})}{partial sigma}] ]

Where \$delta dot{X}^{mu} = delta (frac{partial X^{mu}}{partial tau} = frac{partial delta X^{mu}}{partial tau})\$ and likewise in terms of the analogue for \$X^{prime mu}\$.

However, notice or think about how complicated things become when we look to compute \$frac{partial mathcal{L}}{partial dot{X}^{mu}}\$ and \$frac{partial mathcal{L}}{partial X^{prime mu}}\$. The result we obtain for both terms is below,

[ frac{partial mathcal{L}}{partial dot{X}^{mu}} = frac{(dot{X} cdot X^{prime}) X_{mu}^{prime} – (X^{prime^{2}} dot{X}_{mu})}{sqrt{(dot{X} cdot X^{prime^{2}}) – dot{X}^2 X^{prime^{2}}}} ]

[ frac{partial mathcal{L}}{partial X^{prime mu}} = frac{(dot{X} cdot X^{prime}) X_{mu}^{prime} – (dot{X})^{2} X_{mu}^{prime}}{sqrt{(dot{X} cdot X^{prime^{2}} – dot{X}^2 X^{prime^{2}}}} ]

So, to put it succinctly, we want to try to simplify things a bit. To do so, let’s set \$frac{partial mathcal{L}}{partial dot{X}^{mu}} = mathcal{P}_{mu}^{tau}\$ and \$frac{partial mathcal{L}}{partial X^{mu}prime} = mathcal{P}_{mu}^{sigma}\$. Now we can perform a very direct and explicit substitution,

[ delta S = int_{tau_i}^{tau_f} d tau int_{0}^{sigma_1} dsigma [
mathcal{P}_{mu}^{tau} frac{partial (delta X^{mu})}{partial tau} +
mathcal{P}_{mu}^{sigma} frac{partial (delta X^{mu}}{partial sigma} – delta X^{mu} (frac{partial mathcal{P}_{mu}^{tau}}{partial tau} +
frac{partial mathcal{P}_{mu}^{sigma}}{partial sigma})] ]

Tidying things up,

[ delta S = int_{tau_i}^{tau_f} d tau int_{0}^{sigma_1} dsigma [ frac{partial}{partial tau}(delta X^{mu} mathcal{P}_{mu}^{tau}) + frac{partial}{partial sigma}(delta X^{mu} mathcal{P}_{mu}^{sigma}) –
delta X^{mu} (frac{partial mathcal{P}_{mu}^{tau}}{partial tau} +
frac{partial mathcal{P}_{mu}^{sigma}}{partial sigma})] ]

At this point, the main thing is that we’re going to restrict the variation such that \$delta X^{mu}(tau_{f}, 0) = delta X^{mu}(tau_{i}, sigma) = 0\$.

[ implies delta S = int_{tau_i}^{tau_f} dtau [delta X^{mu}
mathcal{P}_{mu}^{sigma} ]_{0}^{sigma_1} – int_{tau_i}^{tau_f} dtau int_{0}^{sigma_1} dsigma delta X^{mu} (frac{partial mathcal{P}_{mu}^{tau}}{partial tau} + frac{partial mathcal{P}_{mu}^{sigma}}{partial sigma}) ]

We know the second term on the right-hand side must vanish for all variations \$delta X^{mu}\$ of the motion. Therefore,

[ frac{partial mathcal{P}_{mu}^{tau}}{partial tau} + frac{partial mathcal{P}_{mu}^{sigma}}{partial sigma} = 0 ]

Thus, we arrive at the EoM for a free relativistic string. This holds for open or closed strings. But the main thing to notice is that, again, it is extremely complicated. For example, consider taking the second derivative of \$mathcal{P}_{mu}^{tau}\$ with respect to \$tau\$. It’s just not very nice.

To simplify matters further, emphasis is placed on the choice of \$(tau , sigma)\$ coordinates. In a very direct way, we need to put constraints on the solutions to the above equation.

Boundary conditions, enter Dp-branes

Let’s reconsider the following result,

[ delta S_{NG} = int_{tau_i}^{tau_f} dtau [delta X^{mu}
mathcal{P}_{mu}^{sigma} ]_{0}^{sigma_1} – int_{tau_i}^{tau_f} dtau int_{0}^{sigma_1} dsigma delta X^{mu} (frac{partial mathcal{P}_{mu}^{tau}}{partial tau} + frac{partial mathcal{P}_{mu}^{sigma}}{partial sigma}) ]

The first term on the the right-hand side concerns the string endpoints. If one were to expand this out they would arrive at a collection of terms for each index, \$mu\$. Ultimately, we need boundary conditions for each term. With that goal in mind, we can impose two sorts of boundary conditions at the endpoints of the string: Dirichlet boundary conditions or Neumann boundary conditions. We actually have quite a bit of freedom when it comes to our choice, thanks to the construction of the action.

One way to think of this is by denoting \$sigma_{*} = { 0, sigma_{1} } rightarrow mathcal{P}_{mu}^{sigma} (tau, sigma_{*})delta X^{mu}(tau, sigma_{*})\$. Here, \$sigma_{*}\$ represents some \$sigma\$-coordinate at the endpoints, which, as we’ve already established, will equal either 0 or \$sigma_{1}\$.

For Neumann boundary conditions,

[ frac{partial mathcal{L}}{partial X^{prime mu}} = mathcal{P}_{mu}^{sigma} (tau, sigma_{*}) rightarrow mathcal{P}_{mu}^{sigma} rvert_{sigma_{1}} = (0, pi) = 0 ]

Neumann boundaries, otherwise known as free boundaries, mean that for open strings the ends can move freely. The physics of the endpoints is interesting and worth review if one is not familiar (see Zwiebach, 2009), as the endpoints of an open string always move with the speed of light. This also means their worldlines are lightlike. Additionally, it can also be shown that the momentum is conserved at the end of the string.

(For periodic boundary conditions in the case of closed strings, where the string does not have timelike boundaries: \$ X(sigma_{1}) = X(sigma_1 + pi)\$.)

Fixing \$sigma_{*}\$, the Dirichlet boundary condition \$frac{partial X^{mu}}{partial tau}(tau, sigma_{*}) = 0\$, where \$mu neq 0\$. Here the string endpoint is fixed in time, and so the \$tau\$ derivative vanishes.

The EoM can then be written as,

[ partial_0 frac{partial mathcal{L}}{partial dot{X}^{mu}} + partial_1 frac{partial mathcal{L}}{partial X^{partial mu}} ]

Or, equivalently, \$partial^{alpha} mathcal{P}_{alpha}^{mu}\$.

What is nice about this discussion is that we arrive at an intuitive introduction to the concept of the spacelike surfaces of D-branes or, more concisely, Dp-branes, with p-dimensionality. (For example, a D0-brane is a particle like object. A D2-brane is like a hyperplane).

To approach it differently: from the case of classical mechanics, we know that if a string has Dirichlet boundary conditions then the ends of the string are fixed. But this raises the obvious question: to what, in this case, might the ends be fixed? The objects that constrain the motion of the endpoints are D-branes. More elaborately, with Neumann boundary conditions of \$p\$ timelike and spacelike conditions and D-p Dirichlet boundary conditions, we can say that the ends of the string are fixed on some p-dimensional D-brane.

As this post only serves as a brief introduction, D-branes will be discussed in more detail another time. A few comments in the meantime: 1) I think that while limited the above description some intuition about branes which are quite complex objects in ST. 2) Dp-branes do not break Lorentz invariance on the grounds that they are space filling objects. However many higher-dimensions are theorised – say, 10-dimensions for example – the D-brane would fill 3D space and also some of the extra dimensions. 3) Momentum is not conserved at the ends of the string in the Dirichlet directions (translation invariance is broken).

Generalising p-brane action

As an aside, recall the action for a point particle,

[ S_{PP} = -m int dtau (- dot{X}^{mu} dot{X}_{mu})^{frac{1}{2}} ]

Though a slight distraction from the early pages of Polchinski, it should be noted that this action can be generalised, as we have seen, not only to the case of a string sweeping out a (1+1)-dim worldsheet, but also to a p-brane sweeping out a (p+1)-dimensional world-volume. We can parameterise the brane by, again, invoking timelike and spacelike coordinates. In that we’re considering D-dimensional spacetime, \$p<D\$, we can picture a D2-brane sweeping a world-volume in higher dimensional spacetime.

The generalised action is,

[ S_{p} = -T_{p} int d{mu}_p ]

Where \$T_p\$ is the brane tension. As for \$d{mu}_p\$, this is the volume element. It is (p+1)-dimensional and looks like this,

[ d{mu}_p = sqrt{- det G_{alpha beta}} d^{p+1} sigma ]

Here, the induced metric is given by,

[ G_{alpha beta} = g_{mu nu} (X) partial_{alpha} X^{mu} partial_{beta} X^{nu} ]

Slope parameter \$alpha^{prime}\$

There is one last comment to be made here, this time in reference to p. 11 in Polchinski. Recall the string tension in the NG action.

An alternative parameter to the tension is \$alpha^{prime}\$. This parameter has been used since the early days in string theory. It is a proportionality constant, and, if one is already familiar with the Regge trajectories, they will understand \$alpha^{prime}\$ in terms of the relation between the angular momentum, \$J\$, of a rotating string and the square of the energy \$E\$. (For a bit of history and intuition, see this lecture by Leonard Susskind). In that \$alpha^{prime}\$ is a famous constant in string theory, as Polchinski notes, and in that it has units of spacetime-length-squared, which is the Regge slope, we observe:

[ T = frac{1}{2 pi alpha prime} ]

Where \$hbar = c = 1\$. From this another famous result can be arrived at regarding the string length, \$l_s\$. It is written as follows,

[ l_s = sqrt{alpha prime} ]

In closing, the general convention then is write the Nambu-Goto action in this form,

[ S_{NG} = – frac{1}{2 pi alpha prime} int_{sum} dtau dsigma mathcal{L}_{NG} ]

Where \$sum\$ is the worldsheet that we’ve already considered, and \$mathcal{L}\$ is the Lagrangian.

References

Katrin Becker, Melanie Becker, John H. Schwarz. (2006). “String Theory and M-Theory: A Modern Introduction”.

Barton Zwiebach. (2009). “A First Course in String Theory”.

Standard Stringy Things

# Notes on string theory: The Nambu-Goto action for the relativistic string

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*Edited 13/02/19 for clarity of language.

Following a brief study of the relativistic point particle, this entry focuses on an introductory study of the relativistic string. More particularly, we’re going to work our way toward deriving the Nambu-Goto action. The Nambu-Goto action is first mentioned on p. 11 in Polchinski’s “String Theory“. For Polchinski, or at least this is my reading of the text, the driving focus early on is to begin with the Nambu-Goto action and arrive almost immediately at the Polyakov action before launching very directly into the subject of stringy Conformal Field Theory. The nuances of open and closed strings, light cone quantisation, the string specturm, among other introductory topics are entertained along the way. As a generalisation of the Nambu-Goto action that we’re about to derive, the Polyakov formulation that will be studied in a separate entry will prove very important when it comes to the quantum theory of strings, keeping in mind that currently we’re working in bosonic string theory.

In following Polchinski, one of the advantages of building the picture of bosonic string theory from the relativistic free point particle and its classical action to the relativistic (free and open) string, is that for a description of the relativistic string we repeat much of what we’ve already done in a more or less analogous way when studying the point particle.

It is worthwhile focusing on describing the relativistic string, the Nambu-Goto action \$S_{NG}\$ and its 2-dimensional worldsheet before we ultimately set ourselves on the Polyakov action \$S_{P}\$ (sometimes called the string sigma model action) because, again, we will be able to compile an extensive list of analogies to rely on for the purposes pedagogical clarity, intuition and conceptual cohesion. Or, at least in my own studies in ST, this was how I liked to build the picture. It is an approach that I think allows for one to flesh out a lot of the lovely subtleties and nuances of the theory, ultimately enabling a fairly deep and substantive understanding from the ground-up.

With the preamble out of the way, let’s start.

***

The mission here is to begin piecing together a description of a string propagating in d-dimensional spacetime. This includes defining the classical action, beginning, indeed, with what is called the Nambu-Goto action.

If a 0-dimensional point particle (0-brane) traces out a (0+1)-dimensional worldline, a 1-dimensional string (1-brane) sweeps out a (1+1)-dimensional surface that is called the string worldsheet. (Note we have yet to define the concept of branes, but we will begin to do so in the next few entries).

Additionally, just as we can parameterise the relativistic point particle’s (0+1)-dimensional worldline, we can parameterise the the (1+1)-dimensional worldsheet (WS) traced by the relativistic string. Let’s begin with this, as it will enable us to build an early picture.

Infinitesimal area element and area functional [Before proceeding, I would like to emphasise that there is a much more elegant way to think about the embedding of the string surface in the background spacetime. Indeed, there is a much more concise way to think about the following parameterisations. Instead, this discussion builds, in a sense, from first principles and it does so for pedagogical purposes].

We need an action to describe the dynamics of the string. One of the nice qualities of the Nambu-Goto action for the relativistic string is that it is constructed in such a way to be proportional to the proper area of the worldsheet. It is also standard in the literature to parameterise the position along the string by the spatial coordinate, \$sigma\$. Generally, we say that \$sigma\$ can take the values in the range \$0 leq sigma leq l\$.

To make sense of all this, begin by invoking the concept of area in a parameter space, as illustrated above. What we’re working toward defining here is what is called the “string map”, which enables us to embed the WS in the ambient or background space. Note that the parameterised surface can be described by the coordinate functions,

[ vec{x}(xi^1 , xi^2) = x^1 (xi^1 , xi^2), x^2 (xi^1 , xi^2), x^3 (xi^1 , xi^2) ]

The area to which we want to give mathematical description, as pictured, is more accurately an infinitesimal area element. Since we begin working in a parameter space, our very small square is mapped onto the surface in target space. Here spacetime is referred to as the target space, because we want to distinguish between this surface and the string worldsheet. When we map this ‘very small’ area to the surface, we achieve a parallelogram in which the sides may be denoted as \$dvec{v}_1\$ and \$dvec{v}_2\$.

[ d vec{v}_1 = frac{partial vec{x}}{partial xi^1} dxi^1 ]
[ d vec{v}_2 = frac{partial vec{x}}{partial xi^2} dxi^2 ]

Notice, again, the illustration above. One may have guessed that the main objective here is to compute the area of this parallelogram. Of course, again, by “area” I mean an infinitesimal area element. To achieve this we simply need to invoke a basic formula and perform some simple calculations,

[ dA = mid dvec{v}_1 times dvec{v}_2 mid ]
[ dA^2 = (dvec{v}_1 times dvec{v}_2) cdot (dvec{v}_1 times dvec{v}_2) = (dvec{v}_1)^2 (dvec{v})^2 – (dvec{v}_1 cdot dvec{v}_2)^2 ]

Note, for pedagogical purposes, it should be featured that this last line comes from the identity \$(vec{A} times vec{B}) cdot (vec{A} times vec{B}) = mid A mid^2 mid B mid^2 – (A cdot B)^2 \$. It follows that what we get is this expression for dA,

[ therefore dA = sqrt{(frac{partial vec{x}}{partial xi^1} cdot frac{partial vec{x}}{partial xi^1})(frac{partial vec{x}}{partial xi^2} cdot frac{partial vec{x}}{partial xi^2}) – (frac{partial vec{x}}{partial xi^1} cdot frac{partial vec{x}}{partial xi^2})^2} dxi^1 dxi^2 ]

And so we achieve some general expression for the area element, which has exactly the same structure in Euclidean space. But this is not the area functional that we require. What we need to do is integrate,

[ A = int sqrt{(frac{partial vec{x}}{partial xi^1} cdot frac{partial vec{x}}{partial xi^1})(frac{partial vec{x}}{partial xi^2} cdot frac{partial vec{x}}{partial xi^2}) – (frac{partial vec{x}}{partial xi^1} cdot frac{partial vec{x}}{partial xi^2})^2} dxi^1 dxi^2 ]

From this, what we have accomplished is the parameterisation of the surface by way of developing a description for the area element. One problem: this result is not very nice. Although it is reparameterisation invariant, it reparameterises in a messy way. We need to simplify, but how? Well, we can make a gauge choice, employ an induced metric, and this formula for the area will simplify greatly.

Induced metric

Suppose you have some vector \$dvec{x}\$ on the surface. It follows we can compute,

[ ds^2 = dvec{x} cdot dvec{x} ]

[ dvec{x} = frac{partial vec{x}}{partial xi^1} dxi^1 + frac{partial vec{x}}{partial xi^2} dxi^2 implies frac{partial vec{x}}{partial xi^i} dxi^i ]

From this we can plug \$dvec{x}\$ back into our expression for \$ds^2\$.

[ ds^2 = (frac{partial vec{x}}{partial xi^i} dxi^i) cdot (frac{partial vec{x}}{partial xi^j} dxi^j) ]
[ = frac{partial vec{x}}{partial xi^i} frac{partial vec{x}}{partial xi^j} dxi^i dxi^j ]
[ = g_{ij}(xi)dxi^i dxi^j ]
[ implies g_{ij}(xi) = frac{partial vec{x}}{partial xi^i} frac{partial vec{x}}{partial xi^j} ]

We now arrive at our induced metric, \$g_{ij}(xi)\$, which is the pullback of the ambient space metric onto the worldsheet. It is worth highlighting in matrix form,

[ g_{ij} = begin{pmatrix}
frac{partial vec{x}}{partial xi^1} cdot frac{partial vec{x}}{partial xi^1} & frac{partial vec{x}}{partial xi^1} cdot frac{partial vec{x}}{partial xi^2} \

frac{partial vec{x}}{partial xi^2} cdot frac{partial vec{x}}{partial xi^1} & frac{partial vec{x}}{partial xi^2} cdot frac{partial vec{x}}{partial xi^2} \
end{pmatrix} ]

Now, carrying on, let’s substitute the appropriate matrix elements into our earlier expression for the infinitesimal area. Notice,

[ dA = sqrt{(g_{11})g_{22} – g_{12}^2} dxi^1 dxi^2 ]
[ = sqrt{det g} dxi^1 dxi^2 ]
[ therefore dA = sqrt{g} dxi^1 dxi^2 ]

Where, in this final result, \$g equiv det g_{ij} (xi)\$.

This implies,

[ A = int dxi^1 dxi^2 sqrt{g} ]

This new way to express the area, \$A\$, is given in terms of the determinant of the induced metric. The wonderful thing about this is that we can now describe the reparameterisation invariance by way of how this metric transforms. Moreover, we can show this new form for the area is manifestly reparameterisation invariant.

Reparameterisation invariance

We can show manifest reparameterisation invariance of the area through a number of steps.

[ ds^2 = g_{ij}(xi) dxi^i dxi^j = tilde{g}_{ij}(tilde{xi}) dtilde{xi}_1 dtilde{xi}_2 ]
[ = tilde{g}_{pq}(tilde{xi}) frac{partial tilde{xi}^p}{partial xi^i} frac{partial tilde{xi}^q}{partial xi^j} dxi^i dxi^j ]
[ therefore g_{ij} = g_{pq} (tilde{xi}) frac{partial tilde{xi}^p}{partial xi^i} frac{partial tilde{xi}^q}{partial xi^j} ]

[ implies int dxi^1 dxi^2 sqrt{g} = int dtilde{xi}_1 dtilde{xi}_2 sqrt{tilde{g}}]

There is a more elegant way to put this, which I could upload in a separate entry should it be required. But for now, one should focus on how similar this is to a metric transformation in GR inasmuch that \$int dxi^1 dxi^2 sqrt{g}\$ transforms via a Jacobian determinant of \$xi\$ with respect to \$tilde{xi}\$ as \$int dtilde{xi}_1 dtilde{xi}_2 sqrt{tilde{g}}\$.

To conclude these opening considerations, we want to derive the action. So we bracket our result for the infinitesimal area on the manifold for just as moment. Now we focus on the string.

String in spacetime

We have found a way to calculate the area of the surface. But since we are interested in the relativistic string action, we need to look to a description of the string (1-brane) as it moves in d-dimensional flat Minkowski spacetime.

Our concern for now is an open string (as opposed to a closed one) that, as described above, sweeps out a 2-dim surface or worldsheet. Again, as described above, we want to embed the string worldsheet in spacetime. Think, in other words, of spacetime surface. We will now also adopt the string theory convention of \$X^{mu}\$ coordinates such as in \$X^{mu}(tau, sigma)\$, where \$(tau, sigma) equiv xi^{a}\$. Oftentimes it  is also written that the WS, \$sum\$, parameterised by \$tau\$ and \$sigma\$ defines the map \$sum : (tau, sigma) mapsto X^{mu}(tau, sigma) in mathbb{R}^{1, d-1}\$. This is, more concisely, the string map mentioned earlier. And so what we’re doing now is parameterising the WS with one timelike coordinate, \$tau\$, and one spacelike coordinate, \$sigma\$. To continue in a very explicit tone, it is this mapping that enables us to embed the WS in the ambient space. Moreover, the function \$X^{mu}(tau, sigma)\$ will allow us to describe this embedding, while the endpoints of the string are parameterised by \$tau\$ such that \$frac{partial X^{mu}}{partial tau} (tau, sigma) neq 0\$.

We begin by writing the area as,

[ dA = dtau dsigma sqrt{(frac{partial X^{mu}}{partial tau} frac{partial X_{mu}}{partial tau})(frac{partial X^{nu}}{partial sigma} frac{partial X_{nu}}{partial sigma}) – (frac{partial X^{mu}}{partial tau} frac{partial X_{mu}}{partial sigma})^2} ]

[ = dtau dsigma sqrt{(frac{partial X}{partial tau} cdot frac{partial X}{partial tau})(frac{partial X}{partial sigma} cdot frac{partial X}{partial sigma}) – (frac{partial X}{partial tau} cdot frac{partial X}{partial sigma})^2} ]

[ = sqrt{(dot{X})^2 (Xprime)^2 – (dot{X} cdot Xprime)^2} ]

Here we invoked the relativistic dot product. One further comment: notice the sign under the square root. I don’t always see this nuance emphasised, but it should be highlighted that for a surface with a timelike vector and a spacelike vector the square root is always positive such that Cauchy-Schwarz inequality flips (for proof of this see Zwiebach, 2009, p. 110). This means,

[ (dot{X}^2 cdot X^{prime})^2 – (dot{X})^2 (X^{prime})^2 > 0 ] It follows from this the Nambu-Goto action, whereby we integrate over the area element.

[ therefore S_{NG} = -frac{T_0}{c} int_{tau_i}^{tau_f} dtau int_{0}^{sigma_1} dsigma sqrt{(dot{X} cdot Xprime)^2 – dot{X}^2 cdot Xprime^2} ]

Where \$dot{X} = frac{partial X^{mu}}{partial tau}\$ and \$Xprime^{mu} = frac{partial X^{mu}}{partial sigma}\$. Notice the \$frac{T_0}{c}\$ out front is a constant of proportionality to ensure units of action. It also turns out to be true that this \$T_0\$ term is precisely describes the tension in the string.

Further comments: NG action as manifestly reparameterisation invariant

Similar to what we did before, we can write the NG action in a manifestly reparameterisation form. First, we need our target space Minkowski metric. \$alpha\$ and \$beta\$ are from 1 and 2. \$xi^1 = tau\$ and  \$xi^2 = sigma\$.

[ -ds^2 = dX^{mu} dX_{mu} = eta_{mu nu} dX^{mu} dX^{nu} = eta_{mu nu} frac{partial X^{mu}}{partial xi^{alpha}} frac{partial X^{nu}}{partial xi^{beta}} dxi^{alpha} dxi^{beta} ]

If the string worldsheet is a curved surface embedded in spacetime, we can define an induced metric \$gamma_{alpha beta}\$ on the worldsheet. It was stated above that this induced metric is the pullback of the ambient space metric, \$eta_{mu nu}\$, and perhaps this comment will now become more clear. Moreover, we can say that \$gamma_{alpha beta}\$ is the worldsheet metric induced by the target space Minkowski metric. Notice, then, for the induced metric we can compute,

[ gamma_{alpha beta} = eta_{mu nu} frac{partial X^{mu}}{partial xi^{alpha}} frac{partial X^{nu}}{partial xi^{beta}} = frac{partial X}{partial xi^{alpha}} cdot frac{partial X}{partial xi^{beta}} ]

The worldsheet metric induced by the Minkowski metric can be written in matrix form,

[ gamma_{alpha beta} = begin{pmatrix}
dot{X}^2 & dot{X} cdot X^{prime} \

dot{X} cdot X^{prime} & X^2 prime \

end{pmatrix} ]

Therefore, we arrive at the NG action as the area element in spacetime:

[ S_{NG} = – frac{T_0}{c} int dtau int dsigma sqrt{gamma_{12}^2 – gamma_{11} gamma_{22}} ]

[ = – frac{T_0}{c} int dtau dsigma sqrt{- det gamma} ]

[ = – frac{T_0}{c} int dtau dsigma sqrt{- gamma} ]

Where \$gamma = det(gamma_{alpha beta})\$.

In the post to immediately follow we will look at the equations of motion.

References

Barton Zwiebach. (2009). “A First Course in String Theory”, 2nd edition.

Standard