String theory


Fundamental objects


Perturbative theory


Nonperturbative results


Phenomenology


Mathematics






In string theory, Dbranes are a class of extended objects upon which open strings can end with Dirichlet boundary conditions, after which they are named. Dbranes were discovered by Dai, Leigh and Polchinski, and independently by Hořava in 1989. In 1995, Polchinski identified Dbranes with black pbrane solutions of supergravity, a discovery that triggered the Second Superstring Revolution and led to both holographic and Mtheory dualities.
Dbranes are typically classified by their spatial dimension, which is indicated by a number written after the D. A D0brane is a single point, a D1brane is a line (sometimes called a "Dstring"), a D2brane is a plane, and a D25brane fills the highestdimensional space considered in bosonic string theory. There are also instantonic D(1)branes, which are localized in both space and time.
Contents

Theoretical background 1

Braneworld cosmology 2

Dbrane scattering 3

Gauge theories 4

Black holes 5

History 6

See also 7

References 8
Theoretical background
The equations of motion of string theory require that the endpoints of an open string (a string with endpoints) satisfy one of two types of boundary conditions: The Neumann boundary condition, corresponding to free endpoints moving through spacetime at the speed of light, or the Dirichlet boundary conditions, which pin the string endpoint. Each coordinate of the string must satisfy one or the other of these conditions. There can also exist strings with mixed boundary conditions, where the two endpoints satisfy NN, DD, ND and DN boundary conditions. If p spatial dimensions satisfy the Neumann boundary condition, then the string endpoint is confined to move within a pdimensional hyperplane. This hyperplane provides one description of a Dpbrane.
Although rigid in the limit of zero coupling, the spectrum of open strings ending on a Dbrane contains modes associated with its fluctuations, implying that Dbranes are dynamical objects. When N Dbranes are nearly coincident, the spectrum of strings stretching between them becomes very rich. One set of modes produce a nonabelian gauge theory on the worldvolume. Another set of modes is an N \times N dimensional matrix for each transverse dimension of the brane. If these matrices commute, they may be diagonalized, and the eigenvalues define the position of the N Dbranes in space. More generally, the branes are described by noncommutative geometry, which allows exotic behavior such as the Myers effect, in which a collection of Dpbranes expand into a D(p+2)brane.
Tachyon condensation is a central concept in this field. Ashoke Sen has argued that in Type IIB string theory, tachyon condensation allows (in the absence of NeveuSchwarz 3form flux) an arbitrary Dbrane configuration to be obtained from a stack of D9 and anti D9branes. Edward Witten has shown that such configurations will be classified by the Ktheory of the spacetime. Tachyon condensation is still very poorly understood. This is due to the lack of an exact string field theory that would describe the offshell evolution of the tachyon.
Braneworld cosmology
This has implications for physical cosmology. Because string theory implies that the Universe has more dimensions than we expect—26 for bosonic string theories and 10 for superstring theories—we have to find a reason why the extra dimensions are not apparent. One possibility would be that the visible Universe is in fact a very large Dbrane extending over three spatial dimensions. Material objects, made of open strings, are bound to the Dbrane, and cannot move "at right angles to reality" to explore the Universe outside the brane. This scenario is called a brane cosmology. The force of gravity is not due to open strings; the gravitons which carry gravitational forces are vibrational states of closed strings. Because closed strings do not have to be attached to Dbranes, gravitational effects could depend upon the extra dimensions orthogonal to the brane.
Dbrane scattering
When two Dbranes approach each other the interaction is captured by the one loop annulus amplitude of strings between the two branes. The scenario of two parallel branes approaching each other at a constant velocity can be mapped to the problem of two stationary branes that are rotated relative to each other by some angle. The annulus amplitude yields singularities that correspond to the onshell production of open strings stretched between the two branes. This is true irrespective of the charge of the Dbranes. At nonrelativistic scattering velocities the open strings may be described by a lowenergy effective action that contains two complex scalar fields that are coupled via a term \phi^2\chi^2. Thus, as the field \phi (separation of the branes) changes, the mass of the field \chi changes. This induces open string production and as a result the two scattering branes will be trapped.
Gauge theories
The arrangement of Dbranes constricts the types of string states which can exist in a system. For example, if we have two parallel D2branes, we can easily imagine strings stretching from brane 1 to brane 2 or vice versa. (In most theories, strings are oriented objects: each one carries an "arrow" defining a direction along its length.) The open strings permissible in this situation then fall into two categories, or "sectors": those originating on brane 1 and terminating on brane 2, and those originating on brane 2 and terminating on brane 1. Symbolically, we say we have the [1 2] and the [2 1] sectors. In addition, a string may begin and end on the same brane, giving [1 1] and [2 2] sectors. (The numbers inside the brackets are called ChanPaton indices, but they are really just labels identifying the branes.) A string in either the [1 2] or the [2 1] sector has a minimum length: it cannot be shorter than the separation between the branes. All strings have some tension, against which one must pull to lengthen the object; this pull does work on the string, adding to its energy. Because string theories are by nature relativistic, adding energy to a string is equivalent to adding mass, by Einstein's relation E = mc^{2}. Therefore, the separation between Dbranes controls the minimum mass open strings may have.
Furthermore, affixing a string's endpoint to a brane influences the way the string can move and vibrate. Because particle states "emerge" from the string theory as the different vibrational states the string can experience, the arrangement of Dbranes controls the types of particles present in the theory. The simplest case is the [1 1] sector for a Dpbrane, that is to say the strings which begin and end on any particular Dbrane of p dimensions. Examining the consequences of the NambuGoto action (and applying the rules of quantum mechanics to quantize the string), one finds that among the spectrum of particles is one resembling the photon, the fundamental quantum of the electromagnetic field. The resemblance is precise: a pdimensional version of the electromagnetic field, obeying a pdimensional analogue of Maxwell's equations, exists on every Dpbrane.
In this sense, then, one can say that string theory "predicts" electromagnetism: Dbranes are a necessary part of the theory if we permit open strings to exist, and all Dbranes carry an electromagnetic field on their volume.
Other particle states originate from strings beginning and ending on the same Dbrane. Some correspond to massless particles like the photon; also in this group are a set of massless scalar particles. If a Dpbrane is embedded in a spacetime of d spatial dimensions, the brane carries (in addition to its Maxwell field) a set of d  p massless scalars (particles which do not have polarizations like the photons making up light). Intriguingly, there are just as many massless scalars as there are directions perpendicular to the brane; the geometry of the brane arrangement is closely related to the quantum field theory of the particles existing on it. In fact, these massless scalars are Goldstone excitations of the brane, corresponding to the different ways the symmetry of empty space can be broken. Placing a Dbrane in a universe breaks the symmetry among locations, because it defines a particular place, assigning a special meaning to a particular location along each of the d  p directions perpendicular to the brane.
The quantum version of Maxwell's electromagnetism is only one kind of gauge theory, a U(1) gauge theory where the gauge group is made of unitary matrices of order 1. Dbranes can be used to generate gauge theories of higher order, in the following way:
Consider a group of N separate Dpbranes, arranged in parallel for simplicity. The branes are labeled 1,2,...,N for convenience. Open strings in this system exist in one of many sectors: the strings beginning and ending on some brane i give that brane a Maxwell field and some massless scalar fields on its volume. The strings stretching from brane i to another brane j have more intriguing properties. For starters, it is worthwhile to ask which sectors of strings can interact with one another. One straightforward mechanism for a string interaction is for two strings to join endpoints (or, conversely, for one string to "split down the middle" and make two "daughter" strings). Since endpoints are restricted to lie on Dbranes, it is evident that a [1 2] string may interact with a [2 3] string, but not with a [3 4] or a [4 17] one. The masses of these strings will be influenced by the separation between the branes, as discussed above, so for simplicity's sake we can imagine the branes squeezed closer and closer together, until they lie atop one another. If we regard two overlapping branes as distinct objects, then we still have all the sectors we had before, but without the effects due to the brane separations.
The zeromass states in the openstring particle spectrum for a system of N coincident Dbranes yields a set of interacting quantum fields which is exactly a U(N) gauge theory. (The string theory does contain other interactions, but they are only detectable at very high energies.) Gauge theories were not invented starting with bosonic or fermionic strings; they originated from a different area of physics, and have become quite useful in their own right. If nothing else, the relation between Dbrane geometry and gauge theory offers a useful pedagogical tool for explaining gauge interactions, even if string theory fails to be the "theory of everything".
Black holes
Another important use of Dbranes has been in the study of black holes. Since the 1970s, scientists have debated the problem of black holes having entropy. Consider, as a thought experiment, dropping an amount of hot gas into a black hole. Since the gas cannot escape from the hole's gravitational pull, its entropy would seem to have vanished from the universe. In order to maintain the second law of thermodynamics, one must postulate that the black hole gained whatever entropy the infalling gas originally had. Attempting to apply quantum mechanics to the study of black holes, Stephen Hawking discovered that a hole should emit energy with the characteristic spectrum of thermal radiation. The characteristic temperature of this Hawking radiation is given by

T_{\rm H} = \frac{\hbar c^3}{8\pi GM k_B} \;\quad(\approx {1.227 \times 10^{23}\; kg \over M}\; K),
where G is Newton's gravitational constant, M is the black hole's mass and k_{B} is Boltzmann's constant.
Using this expression for the Hawking temperature, and assuming that a zeromass black hole has zero entropy, one can use thermodynamic arguments to derive the "Bekenstein entropy":

S_{\rm B} = \frac{k_B 4\pi G}{\hbar c} M^2.
The Bekenstein entropy is proportional to the black hole mass squared; because the Schwarzschild radius is proportional to the mass, the Bekenstein entropy is proportional to the black hole's surface area. In fact,

S_{\rm B} = \frac{A k_B}{4 l_{\rm P}^2},
where l_{\rm P} is the Planck length.
The concept of black hole entropy poses some interesting conundra. In an ordinary situation, a system has entropy when a large number of different "microstates" can satisfy the same macroscopic condition. For example, given a box full of gas, many different arrangements of the gas atoms can have the same total energy. However, a black hole was believed to be a featureless object (in John Wheeler's catchphrase, "Black holes have no hair"). What, then, are the "degrees of freedom" which can give rise to black hole entropy?
String theorists have constructed models in which a black hole is a very long (and hence very massive) string. This model gives rough agreement with the expected entropy of a Schwarzschild black hole, but an exact proof has yet to be found one way or the other. The chief difficulty is that it is relatively easy to count the degrees of freedom quantum strings possess if they do not interact with one another. This is analogous to the ideal gas studied in introductory thermodynamics: the easiest situation to model is when the gas atoms do not have interactions among themselves. Developing the kinetic theory of gases in the case where the gas atoms or molecules experience interparticle forces (like the van der Waals force) is more difficult. However, a world without interactions is an uninteresting place: most significantly for the black hole problem, gravity is an interaction, and so if the "string coupling" is turned off, no black hole could ever arise. Therefore, calculating black hole entropy requires working in a regime where string interactions exist.
Extending the simpler case of noninteracting strings to the regime where a black hole could exist requires supersymmetry. In certain cases, the entropy calculation done for zero string coupling remains valid when the strings interact. The challenge for a string theorist is to devise a situation in which a black hole can exist which does not "break" supersymmetry. In recent years, this has been done by building black holes out of Dbranes. Calculating the entropies of these hypothetical holes gives results which agree with the expected Bekenstein entropy. Unfortunately, the cases studied so far all involve higherdimensional spaces — D5branes in ninedimensional space, for example. They do not directly apply to the familiar case, the Schwarzschild black holes observed in our own universe.
History
Dirichlet boundary conditions and Dbranes had a long "prehistory" before their full significance was recognized. Mixed Dirichlet/Neumann boundary conditions were first considered by Warren Siegel in 1976 as a means of lowering the critical dimension of open string theory from 26 or 10 to 4 (Siegel also cites unpublished work by Halpern, and a 1974 paper by Chodos and Thorn, but a reading of the latter paper shows that it is actually concerned with linear dilation backgrounds, not Dirichlet boundary conditions). This paper, though prescient, was littlenoted in its time (a 1985 parody by Siegel, "The Superg String," contains an almost deadon description of braneworlds). Dirichlet conditions for all coordinates including Euclidean time (defining what are now known as Dinstantons) were introduced by Michael Green in 1977 as a means of introducing pointlike structure into string theory, in an attempt to construct a string theory of the strong interaction. String compactifications studied by Harvey and Minahan, Ishibashi and Onogi, and Pradisi and Sagnotti in 198789 also employed Dirichlet boundary conditions.
The fact that Tduality interchanges the usual Neumann boundary conditions with Dirichlet boundary conditions was discovered independently by Horava and by Dai, Leigh, and Polchinski in 1989; this result implies that such boundary conditions must necessarily appear in regions of the moduli space of any open string theory. The Dai et al. paper also notes that the locus of the Dirichlet boundary conditions is dynamical, and coins the term Dirichletbrane (Dbrane) for the resulting object (this paper also coins orientifold for another object that arises under string Tduality). A 1989 paper by Leigh showed that Dbrane dynamics are governed by the DiracBornInfeld action. Dinstantons were extensively studied by Green in the early 1990s, and were shown by Polchinski in 1994 to produce the e^{1⁄g} nonperturbative string effects anticipated by Shenker. In 1995 Polchinski showed that Dbranes are the sources of electric and magnetic Ramond–Ramond fields that are required by string duality, leading to rapid progress in the nonperturbative understanding of string theory.
See also
References

Bachas, C. P. "Lectures on Dbranes" (1998). arXiv:hepth/9806199.

Giveon, A. and Kutasov, D. "Brane dynamics and gauge theory", Rev. Mod. Phys. 71, 983 (1999). arXiv:hepth/9802067.

Hashimoto, Koji, DBrane: Superstrings and New Perspective of Our World. Springer (2012). ISBN 9783642235733

Johnson, Clifford (2003). Dbranes. Cambridge: Cambridge University Press.

Polchinski, Joseph, TASI Lectures on Dbranes, arXiv:hepth/9611050. Lectures given at TASI '96.

Polchinski, Joseph, Phys. Rev. Lett. 75, 4724 (1995). An article which established Dbranes' significance in string theory.

Zwiebach, Barton. A First Course in String Theory. Cambridge University Press (2004). ISBN 0521831431.
This article was sourced from Creative Commons AttributionShareAlike License; additional terms may apply. World Heritage Encyclopedia content is assembled from numerous content providers, Open Access Publishing, and in compliance with The Fair Access to Science and Technology Research Act (FASTR), Wikimedia Foundation, Inc., Public Library of Science, The Encyclopedia of Life, Open Book Publishers (OBP), PubMed, U.S. National Library of Medicine, National Center for Biotechnology Information, U.S. National Library of Medicine, National Institutes of Health (NIH), U.S. Department of Health & Human Services, and USA.gov, which sources content from all federal, state, local, tribal, and territorial government publication portals (.gov, .mil, .edu). Funding for USA.gov and content contributors is made possible from the U.S. Congress, EGovernment Act of 2002.
Crowd sourced content that is contributed to World Heritage Encyclopedia is peer reviewed and edited by our editorial staff to ensure quality scholarly research articles.
By using this site, you agree to the Terms of Use and Privacy Policy. World Heritage Encyclopedia™ is a registered trademark of the World Public Library Association, a nonprofit organization.