13557911
Breaking cosmic strings without monopoles.
It is shown that topologically stable cosmic strings can, in fact, appear to end or to break, even in theories without monopoles. This can occur whenever the spatial topology of the universe is nontrivial. For the case of Abelian-Higgs strings, we describe the gauge and scalar field configurations necessary for a string to end on a black hole. We give a lower bound for the rate at which a cosmic string will break via black hole pair production, using an instanton calculation based on the Euclidean C-metric.
23955919
Origin of gauge invariance in string theory.
We present a first quantization of the space-time embedding X/sup ..mu../ and the world-sheet metric rho of the open bosonic string. The world-sheet metric rho decouples from S-matrix elements in 26 dimensions. This formulation of the theory naturally includes 26-dimensional gauge transformations. The gauge invariance of S-matrix elements is a direct consequence of the decoupling of rho. Second quantization leads to a string field Phichemically bondX/sup ..mu../,rhochemically bond with a gauge-covariant equation of motion.
7270273
Pair creation of extremal black holes and Kaluza-Klein monopoles.
Classical solutions describing charged dilaton black holes accelerating in a background magnetic field have recently been found. They include the Ernst metric of the Einstein-Maxwell theory as a special case. We study the extremal limit of these solutions in detail, both at the classical and quantum levels. It is shown that near the event horizon the extremal solutions reduce precisely to the static extremal black hole solutions. For a particular value of the dilaton coupling, these extremal black holes are five-dimensional Kaluza-Klein monopoles. The Euclidean sections of these solutions can be interpreted as instantons describing the pair creation of extremal black holes and/or Kaluza-Klein monopoles in a magnetic field. The action of these instantons is calculated and found to agree with the Schwinger result in the weak-field limit. For the Euclidean Ernst solution, the action for the extremal solution differs from that of the previously discussed wormhole instanton by the Bekenstein-Hawking entropy. However, in many cases quantum corrections become large in the vicinity of the black hole, and the precise description of the creation process is unknown.
15786164
Where is the information stored in black holes
It is shown that many modes of the gravitational field exist only inside the horizon of an extreme black hole in string theory. At least in certain cases, the number of such modes is sufficient to account for the Bekenstein-Hawking entropy. These modes are associated with sources which carry Ramond-Ramond charge, and so may be viewed as the strong coupling limit of D-branes. Although these sources naturally live at the singularity, they are well defined and generate modes which extend out to the horizon. This suggests that the information in an extreme black hole is not localized near the singularity or the horizon, but extends between them.
14670933
Microstates of a neutral black hole in M theory.
We consider vacuum solutions in M theory of the form of a five-dimensional Kaluza-Klein black hole cross T6. In a certain limit, these include the five-dimensional neutral rotating black hole (cross T6). From a type-IIA standpoint, these solutions carry D0 and D6 charges. We show that there is a simple D-brane description which precisely reproduces the Hawking-Bekenstein entropy in the extremal limit, even though supersymmetry is completely broken.
15074147
Photoemission “experiments” on holographic superconductors
We study the effects of a superconducting condensate on holographic Fermi surfaces. With a suitable coupling between the fermion and the condensate, there are stable quasiparticles with a gap. We find some similarities with the phenomenology of the cuprates: in systems whose normal state is a non-Fermi liquid with no stable quasiparticles, a stable quasiparticle peak appears in the condensed phase.
11521966
Parity-violating quasielastic electron scattering.
The parity-violating asymmetry [ital A] is calculated for quasielastic electron scattering. We use a relativistic mean field model of the nuclear matter response. A Lorentz scalar mean field (which reduces the nucleon's mass) decreases [vert bar][ital A][vert bar] by a relatively large amount. This effect must be understood before information on strange quark contributions or weak axial currents can be extracted. Alternatively, very interesting information on isoscalar convection currents could be obtained.
38611028
Density dependence of nuclear neutrino-pair production.
Nuclear decay via neutrino-pair production is found to have a large density dependence because of intermediate electromagnetic couplings to electrons. These are calculated in a relativistic random phase approximation. The decay rate for vector (Fermi) transitions producing electron type neutrino pairs can be enhanced by 10{sup 5} or more at densities relevant for stellar collapse. Axial-vector (Gamow-Teller) transitions are not enhanced.
15357267
Delta excitations in neutrino-nucleus scattering.
We derive the contribution of {Delta}-{ital h} excitations to quasielastic charged-current neutrino-nucleus scattering in the framework of relativistic mean-field theory. We discuss the effect of {Delta} production on the determination of the axial mass {ital M}{sub {ital A}} in neutrino scattering experiments. {copyright} {ital 1996 The American Physical Society.}
37677102
Microscopic relativistic description of proton-nucleus scattering.
Microscopic relativistic optical potentials have been calculated for closed shell nuclei at energies near 200 MeV. These calculations go beyond the simple RIA by resolving ambiguities in the relativistic NN amplitudes and including Pauli blocking corrections.
30531749
Parity violation in heavy nuclei in a relativistic Hartree-Fock approximation.
The parity violating (PV) nucleon self-energy in nuclear matter is calculated in a relativistic Hartree-Fock approximation. Omega meson contributions are enhanced 63% by relativistic effects. However, the total PV self-energy is dominated by [pi] and [rho] contributions, which are relatively insensitive to relativistic effects. These results are used to estimate the 2[ital d][sub 5/2] to 2[ital f][sub 5/2] PV matrix element in [sup 207]Pb.