arXiv subjects

K. Maeda

Publications and source records attributed to K. Maeda.

157 records · Page 9Linked to original sources

arXiv2000

The Properties of Hypernovae: SNe Ic 1998bw, 1997ef, and SN IIn 1997cy

We discuss the properties of the hyper-energetic Type Ic supernovae (SNe Ic) 1998bw and 1997ef and Type IIn supernova (SN IIn) 1997cy. SNe Ic 1998bw and 1997ef are characterized by their large luminosity and the very broad spectral features. Their observed properties can be explained if they are very energetic SN explosions with the kinetic energy of $E_{\rm K} \gsim 1\times10^{52}$ erg, originating probably from the core collapse of the bare C+O cores of massive stars ($\sim 30-40$M$_\odot$). At late times, both the light curves and the spectra suggest that the explosions may have been asymmetric; this may help us understand the claimed connection with GRB's. The Type IIn SN 1997cy is even more luminous than SN 1998bw and the light curve declines more slowly than $^{56}$Co decay. We model such a light curve with circumstellar interaction, which requires the explosion energy of $\sim 5 \times 10^{52}$ erg. Because these kinetic energies of explosion are much larger than in normal core-collapse SNe, we call objects like these SNe "hypernovae". The mass of $^{56}$Ni in SN 1998bw is estimated to be as large as 0.5 - 0.7 $M_\odot$ from both the maximum brightness and late time emission spectra, which suggests that the asymmetry may not be extreme.

astro-ph↗

arXiv2000

Probing the DeltaNN component of 3He

The 3He(gamma,pi^+/- p) reactions were measured simultaneously over a tagged photon energy range of 800<E_gamma<1120 MeV, well above the Delta resonance region. An analysis was performed to kinematically isolate Delta knockout events from conventional Delta photoproduction events, and a statistically significant excess of pi+p events was identified, consistent with Delta++ knockout. Two methods were used to estimate the DeltaNN probability in the 3He ground state, corresponding to the observed knockout cross section. The first gave a lower probability limit of 1.5+/-0.6+/-0.5%; the second yielded an upper limit of about 2.6%.

nucl-ex↗

arXiv1999

Preheating of the nonminimally coupled inflaton field

We investigate preheating of an inflaton field $ϕ$ coupled nonminimally to a spacetime curvature. In the case of a self-coupling inflaton potential $V(ϕ)=λϕ^4/4$, the dynamics of preheating changes by the effect of the negative $ξ$. We find that the nonminimal coupling works in two ways. First, since the initial value of inflaton field for reheating becomes smaller with the increase of $|ξ|$, the evolution of the inflaton quanta is delayed for fixed $λ$. Second, the oscillation of the inflaton field is modified and the nonadiabatic change around $ϕ=0$ occurs significantly. That makes the resonant band of the fluctuation field wider. Especially for strong coupling regimes $|ξ| \gg 1$, the growth of the inflaton flutuation is dominated by the resonance due to the nonminimal coupling, which leads to the significant enhancement of low momentum modes. Although the final variance of the inflaton fluctuation does notchange significantly compared with the minimally coupled case, we have found that the energy transfer from the homogeneous inflaton to created particles efficiently occurs for $ξ<-60$.

hep-ph↗

arXiv1999

Preheating with non-minimally coupled scalar fields in higher-curvature inflation models

In higher-curvature inflation models ($R+α_n R^n$), we study a parametric preheating of a scalar field $χ$ coupled non-minimally to a spacetime curvature $R$ ($ξR χ^2$). In the case of $R^2$-inflation model, efficient preheating becomes possible for rather small values of $ξ$, i.e. $|ξ|< several. Although the maximal fluctuation $\sqrt{< χ^2 >}_{max} \approx 2 \times10^{17}$ GeV for $ξ\approx -4$ is almost the same as the chaotic inflation model with a non-minimally coupled $χ$ field, the growth rate of the fluctuation becomes much larger and efficient preheating is realized. We also investigate preheating for $R^4$ model and find that the maximal fluctuation is $\sqrt{< χ^2 >}_{max} \approx 8 \times 10^{16}$ GeV for $ξ\approx -35$.

hep-ph↗

arXiv1999

Resonant particle production with non-minimally coupled scalar fields in preheating after inflation

We investigate a resonant particle production of a scalar field $χ$ coupled non-minimally to a spacetime curvature $R$ ($ξR χ^2$) as well as to an inflaton field $ϕ$ ($g^2ϕ^2χ^2$). In the case of $g < 3 \times 10^{-4}$, $ξ$ effect assists $g$-resonance in certain parameter regimes. However, for $g > 3 \times 10^{-4}$, $g$-resonance is not enhanced by $ξ$ effect because of $ξ$ suppression effect as well as a back reaction effect. If $ξ\approx -4$, the maximal fluctuation of produced $χ$-particle is $\sqrt{< χ^2 >}_{max} \approx 2 \times 10^{17}$ GeV for $g < 1 \times 10^{-5}$, which is larger than the minimally coupled case with $g \approx 1 \times 10^{-3}$.

hep-ph↗

arXiv1998

Subthreshold rho^0 photoproduction on 3He

A large reduction of the rho^0 mass in the nuclear medium is reported, inferred from dipion photoproduction spectra in the 1 GeV region, for the reaction 3He(gamma,pi+ pi-)X with a 10% duty factor tagged-photon beam and the TAGX multi-particle spectrometer. The energy range covered (800 < E(gamma) < 1120 MeV) lies mostly below the free rho^0 production threshold, a region which is believed sensitive to modifications of light vector-meson properties at nuclear-matter densities. The rho^0 masses extracted from the MC fitting of the data, m*(rho^0) = 642 +/- 40, 669 +/- 32, and 682 +/- 56 MeV/c^2 for E(gamma) in the 800-880, 880-960, and 960-1040 MeV regions respectively, are independently corroborated by a measured, assumption-free, kinematical observable. This mass shift, far exceeding current mean-field driven theoretical predictions, may be suggestive of rho^0 decay within the range of the nucleonic field.

nucl-ex↗

arXiv1998

Renormalization Group Approach in Newtonian Cosmology

We apply the renormalization group (RG) method to examine the observable scaling properties in Newtonian cosmology. The original scaling properties of the equations of motion in our model are modified for averaged observables on constant time slices. In the RG flow diagram, we find three robust fixed points: Einstein-de Sitter, Milne and Quiescent fixed points. Their stability (or instability) property does not change under the effect of fluctuations. Inspired by the inflationary scenario in the early Universe, we set the Einstein-de Sitter fixed point with small fluctuations, as the boundary condition at the horizon scale. Solving the RG equations under this boundary condition toward the smaller scales, we find generic behavior of observables such that the density parameter $Ω$ decreases, while the Hubble parameter $H$ increases for smaller averaging volume. The quantitative scaling properties are analyzed by calculating the characteristic exponents around each fixed point. Finally we argue the possible fractal structure of the Universe beyond the horizon scale.

gr-qc↗

arXiv1996

Chaos in Static Axisymmetric Spacetimes I : Vacuum Case

We study the motion of test particle in static axisymmetric vacuum spacetimes and discuss two criteria for strong chaos to occur: (1) a local instability measured by the Weyl curvature, and (2) a tangle of a homoclinic orbit, which is closely related to an unstable periodic orbit in general relativity. We analyze several static axisymmetric spacetimes and find that the first criterion is a sufficient condition for chaos, at least qualitatively. Although some test particles which do not satisfy the first criterion show chaotic behavior in some spacetimes, these can be accounted for the second criterion.

gr-qc↗

arXiv1994

Non-Abelian Black Holes and Catastrophe Theory II: Charged Type

We reanalyze the gravitating monopole and its black hole solutions in the Einstein-Yang-Mills-Higgs system and we discuss their stabilities from the point of view of catastrophe theory. Although these non-trivial solutions exhibit fine and complicated structures, we find that stability is systematically understood via a swallow tail catastrophe. The Reissner-Nordström trivial solution becomes unstable from the point where the non-trivial monopole black hole appears. We also find that, within a very small parameter range, the specific heat of a monopole black hole changes its sign .

gr-qc↗

arXiv1994

Analysis of the Wheeler-DeWitt Equation beyond Planck Scale and Dimensional Reduction

We solve the Wheeler-DeWitt equation for {\it four}-dimensional Einstein gravity as an expansion in powers of the Planck mass by means of a heat kernel regularization. Our results suggest that in the universe with a very small radius or with a very large curvature beyond a Planck scale expectation values of operators are reduced to calculations in a path integral representation of {\it three}-dimensional Einstein gravity.

hep-th↗

arXiv1993

Stability of Non-Abelian Black Holes

Two types of self-gravitating particle solutions found in several theories with non-Abelian fields are smoothly connected by a family of non-trivial black holes. There exists a maximum point of the black hole entropy, where the stability of solutions changes. This criterion is universal, and the changes in stability follow from a catastrophe-theoretic analysis of the potential function defined by black hole entropy.

gr-qc↗

arXiv1993

Canonical treatment of two dimensional gravity as an anomalous gauge theory

The extended phase space method of Batalin, Fradkin and Vilkovisky is applied to formulate two dimensional gravity in a general class of gauges. A BRST formulation of the light-cone gauge is presented to reveal the relationship between the BRST symmetry and the origin of $SL(2,R)$ current algebra. From the same principle we derive the conformal gauge action suggested by David, Distler and Kawai.

hep-th↗

arXiv1992

A new insight into BRST anomalies in string theory

Using the generalized hamiltonian method of Batalin, Fradkin and Vilkovisky, we investigate the algebraic structure of anomalies in the Polyakov string theory that appear as the Schwinger terms in super-commutation relations between BRST charge and total hamiltonian. We obtain the most general form of the anomalies in the extended phase space, without any reference to a two dimensional metric. This pregeometri- cal result, refered to as the genelarized Virasoro anomaly, independent of the gauge and the regularization under a minor assumption, is a non-perturbative result, and valid for any space-time dimension. In a configuration space, in which the two dimensional metric can be identified, we can geometrize the result without assuming the weak gravitational field, showing that the most general anomaly exactly exhibits the Weyl anomaly.

hep-th↗