arXiv subjects

Piljin Yi

Publications and source records attributed to Piljin Yi.

85 records · Page 5Linked to original sources

arXiv1996

The Moduli Space of Many BPS Monopoles for Arbitrary Gauge Groups

We study the moduli space for an arbitrary number of BPS monopoles in a gauge theory with an arbitrary gauge group that is maximally broken to $U(1)^k$. From the low energy dynamics of well-separated dyons we infer the asymptotic form of the metric for the moduli space. For a pair of distinct fundamental monopoles, the space thus obtained is $R^3 \times(R^1\times {\cal M}_0)/Z$ where ${\cal M}_0$ is the Euclidean Taub-NUT manifold. Following the methods of Atiyah and Hitchin, we demonstrate that this is actually the exact moduli space for this case. For any number of such objects, we show that the asymptotic form remains nonsingular for all values of the intermonopole distances and that it has the symmetries and other characteristics required of the exact metric. We therefore conjecture that the asymptotic form is exact for these cases also.

hep-th↗

arXiv1996

Electromagnetic Duality and $SU(3)$ Monopoles

We consider the low-energy dynamics of a pair of distinct fundamental monopoles that arise in the $N=4$ supersymmetric $SU(3)$ Yang-Mills theory broken to $U(1)\times U(1)$. Both the long distance interactions and the short distance behavior indicate that the moduli space is $R^3\times(R^1 \times {\cal M}_0)/Z$ where ${\cal M}_0$ is the smooth Taub-NUT manifold, and we confirm this rigorously. By examining harmonic forms on the moduli space, we find a threshold bound state of two monopoles with a tower of BPS dyonic states built on it, as required by Montonen-Olive duality. We also present a conjecture for the metric of the moduli space for any number of distinct fundamental monopoles for an arbitrary gauge group.

hep-th↗

arXiv1995

Quenched Hawking Radiation and the Black Hole Pair-Creation Rate

The main topic of this talk is the Hawking effect when the black holes in question are undergoing a uniform acceleration. The semiclassical effect of the acceleration is most striking when the Hawking temperature equals the acceleration temperature. Within the usual late-time approximation, the natural black hole vacuum is then equivalent to the asymptotically empty Minkowskian vacuum, and the accelerated black hole becomes semiclassically stable against the familiar thermal evaporation. An important application of this phenomenon is found in the problem of charged black hole pair-creation.

gr-qc↗

arXiv1995

Quantum Stability of Accelerated Black Holes

We study quantum aspects of the accelerated black holes in some detail. Explicitly shown is the fact that a uniform acceleration stabilizes certain charged black holes against the well-known thermal evaporation. Furthermore, a close inspection of the geometry reveals that this is possible only for near-extremal black holes and that most nonextremal varieties continue to evaporate with a modified spectrum under the acceleration. We also introduce a two-dimensional toy model where the energy-momentum flow is easily obtained for general accelerations, and find the behavior to be in accordance with the four-dimensional results. After a brief comparison to the classical system of a uniformly accelerated charge, we close by pointing out the importance of this result in the WKB expansion of the black hole pair-creation rate.

hep-th↗

arXiv1995

Vanishing Hawking Radiation from a Uniformly Accelerated Black Hole

We consider quantum fields around uniformly accelerated black holes. At a particular value of the acceleration, the Bogolubov transformation which would be responsible for the late-time Hawking radiation, is found to be trivial. When this happens, Hawking's thermal radiation, Doppler-shifted or not, is absent to the asymptotic inertial observers despite the nonzero Hawking temperature, while the co-moving observers find the black hole radiance exactly balanced by the acceleration heat bath. After a brief comparison to the classical system of a uniformly accelerated charge, we close with two important comments. (Phys. Rev. Lett. 75 (1995) 382)

gr-qc↗

arXiv1995

The Bogomol'nyi Bound of Lee-Weinberg Magnetic Monopoles

The Lee-Weinberg $U(1)$ magnetic monopoles, which have been reinterpreted as topological solitons of a certain non-Abelian gauged Higgs model recently, are considered for some specific choice of Higgs couplings. The model under consideration is shown to admit a Bogomol'nyi-type bound which is saturated by the configurations satisfying the generalized BPS equations. We consider the spherically symmetric monopole solutions in some detail.

hep-th↗

arXiv1995

SELF-DUAL ANYONS IN UNIFORM BACKGROUND FIELDS

We study relativistic self-dual Chern-Simons-Higgs systems in the presence of uniform background fields that explicitly break CTP. A rich, but discrete vacuum structure is found when the gauge symmetry is spontaneously broken, while the symmetric phase can have an infinite vacuum degeneracy at tree level. The latter is due to the proliferation of neutral solitonic states that cost zero energy. Various novel self-dual solitons, such as these, are found in both the symmetric and the asymmetric phases. Also by considering a similar system on a two-sphere and the subsequent large sphere limit, we isolate sensible and finite expressions for the conserved angular and linear momenta, which satisfy anomalous commutation relations. We conclude with a few remarks on unresolved issues.

hep-th↗

arXiv1994

Toward One-Loop Tunneling Rates of Near-Extremal Magnetic Black Hole Pair-Production

Pair-production of magnetic Reissner-Nordström black holes (of charges $\pm q$) was recently studied in the leading WKB approximation. Here, we consider generic quantum fluctuations in the corresponding instanton geometry given by the Euclidean Ernst metric, in order to simulate the behaviour of the one-loop tunneling rate. A detailed study of the Ernst metric suggests that for sufficiently weak field $B$, the problem can be reduced to that of quantum fluctuations around a single near-extremal Euclidean black hole in thermal equilibrium with a heat bath of finite size. After appropriate renormalization procedures, typical one-loop contributions to the WKB exponent are shown to be inversely proportional to $B$, as $B\rightarrow 0$, indicating that the leading Schwinger term is corrected by a small fraction $\sim \hbar /q^2$. We demonstrate that this correction to the Schwinger term is actually due to a semiclassical shift of the black hole mass-to-charge ratio that persists even in the extremal limit. Finally we discuss a few loose ends.

hep-th↗

arXiv1994

Magnetic Black Hole Pair-Production: One-Loop Tunneling Rate in the Weak Field Limit

Pair-production of magnetic Reissner-Nordström black holes (of charges $\pm q$) is studied in the next-to-leading WKB approximation. We consider generic quantum fluctuations in the corresponding instanton geometry, a detailed study of which suggests that, for sufficiently weak field $B$, the problem can be reduced to that of quantum fluctuations around a single truncated near-extremal Euclidean black hole in thermal equilibrium. Typical one-loop contributions are such that the leading WKB exponent is corrected by a small fraction $\sim \hbar /q^2$. We show that this effect is merely due to a semiclassical shift of the black hole mass-to-charge ratio that persists even in the extremal limit. We close with a few final comments.

gr-qc↗

arXiv1994

Topology of a Nontopological Magnetic Monopole

Certain nontopological magnetic monopoles, recently found by Lee and Weinberg, are reinterpreted as topological solitons of a non-Abelian gauged Higgs model. Our study makes the nature of the Lee-Weinberg monopoles more transparent, especially with regard to their singularity structure.

hep-th↗

arXiv1994

Fermionic $θ$ Vacua and Long-Necked Remnants

We study a vacuum polarization effect in the background of certain dilatonic extremal black hole, known as the cornucopion. Whenever the charged fermions are of any finite mass, the gravitational backreaction to a generic value of a $CP$ nonconserving vacuum angle $θ$ is shown to be important owing to a vacuum energy density which does not vanish deep inside the cornucopion. When this energy density is positive, this effect creates an extremal horizon at finite physical distance, closing off the infinite neck. We study the geometry near this horizon in some detail and find different physical interpretations for small and large fermion mass. Also, we argue that the conclusion is qualitatively correct despite the strong coupling.

hep-th↗

arXiv1993

Mass vs. Charge: Quantum Radiation from Zero Temperature Black Holes

We study the mass-charge relation for the semiclassical extremal black hole of the $S$-wave sector Einstein-Maxwell theory coupled to $N$ conformal scalars. The classical ratio $M/{|Q|}=1$ is shown to be modified to $M/{|Q|} \simeq 1-k/6$ for small $ k \equiv N\hbar/(12πQ^{2})$. Furthermore, numerical study for $k<2$ shows that $M/|Q|$ is a monotonically decreasing function of $k$. We speculate on the consequence of such a modification in the 4-dimensional context.

hep-th↗

arXiv1993

Nonsingular 2-D Black Holes and Classical String Backgrounds

We study a string-inspired classical 2-D effective field theory with {\it nonsingular} black holes as well as Witten's black hole among its static solutions. By a dimensional reduction, the static solutions are related to the $(SL(2,R)_{k}\otimes U(1))/U(1)$ coset model, or more precisely its $O\bigl((α')^{0}\bigr)$ approximation known as the 3-D charged black string. The 2-D effective action possesses a propagating degree of freedom, and the dynamics are highly nontrivial. A collapsing shell is shown to bounce into another universe without creating a curvature singularity on its path, and the potential instability of the Cauchy horizon is found to be irrelevent in that some of the infalling observers never approach the Cauchy horizon. Finally a $SL(2,R)_{k}/U(1)$ nonperturbative coset metric, found and advocated by R. Dijkgraaf et.al., is shown to be nonsingular and to coincide with one of the charged spacetimes found above. Implications of all these geometries are discussed in connection with black hole evaporation.

hep-th↗