arXiv subjects

Katsuhiko Sato

Publications and source records attributed to Katsuhiko Sato.

At least 55 records · Page 3Linked to original sources

arXiv2005

On the Distribution of State Values of Reproducing Cells: the General Evolution Equation and its Applications

Fluctuations of cell state, e.g., abundances of some proteins, have attracted much attention both theoretically and experimentally. The distribution of such state over cells, however, is not only a result of intracellular stochastic process, but is also influenced by the growth in cell numbers that depends on the state. By incorporating the growth-death process into the standard Fokker--Planck equation for the probability distribution, a nonlinear temporal evolution equation of distribution is obtained that includes a self-consistent growth term. The derived equation is generally solved analytically by means of eigenfunction expansions. By focusing on the case with linear relaxation, two examples are considered as applications of the proposed general formalism. First, by assuming that the growth rate of a cell increases linearly with the state value $x$, the shift of the average state value $x$ due to the growth effect is shown to be proportional to the variance of the state $x$ and the relaxation time, similarly with the biological fluctuation- response relationship. Second, when there is a gap in the growth rate at some threshold value for the state $x$, existence of a critical gap value is demonstrated, beyond which the average growth rate starts to increase. This critical value is again obtained in terms of the relaxation time and the variance of $x$, all of which are experimentally measurable quantities. The relevance of the results to the analysis of biological data on the distribution of cell states, as obtained for example by flow cytometry, is discussed.

physics.bio-ph↗

arXiv2005

Explosion Mechanism, Neutrino Burst, and Gravitational Wave in Core-Collapse Supernovae

Core-collapse supernovae are among the most energetic explosions in the universe marking the catastrophic end of massive stars. In spite of rigorous studies for several decades, we still don't understand the explosion mechanism completely. Since they are related to many astrophysical phenomena such as nucleosynthesis, gamma-ray bursts and acceleration of cosmic rays, understanding of their physics has been of wide interest to the astrophysical community. In this article, we review recent progress in the study of core-collapse supernovae focusing on the explosion mechanism, supernova neutrinos, and the gravitational waves. As for the explosion mechanism, we present a review paying particular attention to the roles of multidimensional aspects, such as convection, rotation, and magnetic fields, on the neutrino heating mechanism. Next, we discuss supernova neutrinos, which is a powerful tool to probe not only deep inside of the supernovae but also intrinsic properties of neutrinos. For this purpose, it is necessary to understand neutrino oscillation which has been established recently by a lot of experiments. Gravitational astronomy is now also becoming reality. We present an extensive review on the physical foundations and the emission mechanism of gravitational waves in detail, and discuss the possibility of their detections.

astro-ph↗

arXiv2005

Quadrupole formula for Kaluza-Klein modes in the braneworld

The quadrupole formula in four-dimensional Einstein gravity is a useful tool to describe gravitational wave radiation. We derive the quadrupole formula for the Kaluza-Klein (KK) modes in the Randall-Sundrum braneworld model. The quadrupole formula provides transparent representation of the exterior weak gravitational field induced by localized sources. We find that a general isolated dynamical source gives rise to the 1/r^2 correction to the leading 1/r gravitational field. We apply the formula to an evaluation of the effective energy carried by the KK modes from the viewpoint of an observer on the brane. Contrary to the ordinary gravitational waves (zero mode), the flux of the induced KK modes by the non-spherical part of the quadrupole moment vanishes at infinity and only the spherical part contributes to the flux. Since the effect of the KK modes appears in the linear order of the metric perturbations, the effective energy flux observed on the brane is not always positive, but can become negative depending on the motion of the localized sources.

gr-qc↗

arXiv2005

R-Process Nucleosynthesis in MHD Jet Explosions of Core-Collapse Supernovae

We investigate $r$-process nucleosynthesis during the magnetohydrodynamical (MHD) explosion of supernova in a massive star of 13 $M_{\odot}$. Contrary to the case of the spherical explosion, jet-like explosion due to the combined effects of the rotation and magnetic field lowers the electron fraction significantly inside the layers above the iron core. We find that the ejected material of low electron fraction responsible for the $r$-process comes out from the silicon rich layer of the presupernova model. This leads to the production up to the third peak in the solar $r$-process elements. We examine whether the fission affects the $r$-process paths by using the full nuclear reaction network with both the spontaneous and $β$-delayed fission included. Moreover, we pay particular attention how the mass formula affects the $r$-process peaks with use of two mass formulae. It is found that both formulae can reproduce the global abundance pattern up to the third peak though detailed distributions are rather different. We point out that there are variations in the $r$-process nucleosynthesis if the MHD effects play an important role in the supernova explosion.

astro-ph↗

arXiv2005

Sub-GeV galactic cosmic-ray antiprotons from primordial black holes in the Randall-Sundrum braneworld

We investigate cosmic-ray antiprotons emitted from the galactic primordial black holes in the Randall-Sundrum type-2 braneworld. The recent results of the BESS antiproton observation implies the existence of exotic primary sub-GeV antiprotons, one of whose most probable origin is PBHs in Our Galaxy. We show that the magnitude of antiproton flux from PBHs in the RS braneworld is proportional to negative power of the AdS radius, and immediately find that a large extra-dimension can relax upper-limits on the abundance of the Galactic PBHs. If actually there are more PBHs than the known upper-limit obtained in the pure 4D case, they set a lower bound on the size of the extra dimension above at least 10^{20} times 4D Planck-length to avoid inconsistency. On completion of the numerical studies, we show that these constraints on the AdS radius is comparable to those obtained from the diffuse photon background by some of the authors in the previous paper. Moreover, in the low accretion-rate case, only antiprotons can constrain the braneworld. We show that we will detect signatures of the braneworld as a difference between the flux of the antiprotons predicted in 4D and 5D by future observations in sub-GeV region with a few percent precision.

astro-ph↗

arXiv2005

Affleck-Dine Baryogenesis and heavy elements production from Inhomogeneous Big Bang Nucleosynthesis

We study the impact of possible high density baryonic bubbles on the early formed QSO, IGM, and metal poor stars. Such bubbles could be created, under certain conditions, in Affleck-Dine model of baryogenesis and may occupy a relatively small fraction of space, while the dominant part of the cosmological volume has the normal observed baryon-to-photon ratio $η= 6\cdot 10^{-10}$. The value of $η$ in the bubbles, could be much larger than the usually accepted one (it might be even close to unity) without contradicting the existing data on light element abundances and the observed angular spectrum of CMBR. We find upper bounds on $η$ by comparing heavy elements' abundances produced in BBN and those of metal poor stars. We conclude that $η$ should be smaller than $10^{-5}$ in some metal poor star regions.

astro-ph↗

arXiv2005

Simulation of Transitions between "Pasta" Phases in Dense Matter

Calculations of equilibrium properties of dense matter predict that at subnuclear densities nuclei can be rodlike or slablike. To investigate whether transitions between phases with non-spherical nuclei can occur during the collapse of a star, we perform quantum molecular dynamic simulations of the compression of dense matter. We have succeeded in simulating the transitions between rodlike and slablike nuclei and between slablike nuclei and cylindrical bubbles. Our results strongly suggest that non-spherical nuclei can be formed in the inner cores of collapsing stars.

nucl-th↗

arXiv2004

Relic neutrino background from cosmological supernovae

Present and future observations of supernova relic neutrinos (SRNs), i.e., a cosmological neutrino background from past core-collapse supernova explosions, potentially give us useful information concerning various fields of astrophysics, cosmology and particle physics. We review recent progress of theoretical and observational studies of SRNs, particularly focusing on the detectability and also on implications for cosmic star formation history and neutrino physics.

astro-ph↗

arXiv2004

North-South Neutrino Heating Asymmetry in Strongly Magnetized and Rotating Stellar Cores

We perform a series of two-dimensional magnetohydrodynamic simulations of supernova cores. Since the distributions of the angular momentum and the magnetic fields of strongly magnetized stars are quite uncertain, we systematically change the combinations of the strength of the angular momentum, the rotations law, the degree of differential rotation, and the profiles of the magnetic fields to construct the initial conditions. By so doing, we estimate how the rotation-induced anisotropic neutrino heating are affected by the strong magnetic fields through parity-violating effects and first investigate how the north-south asymmetry of the neutrino heating in a strongly magnetized supernova core could be. As for the microphysics, we employ a realistic equation of state based on the relativistic mean field theory and take into account electron captures and the neutrino transport via the neutrino leakage scheme. With these computations, we find that the parity-violating corrections reduce $ \lesssim 0.5 %$ of the neutrino heating rate than that without the magnetic fields in the vicinity of the north pole of a star, on the other hand, enhance about $ \lesssim 0.5 %$ in the vicinity of the south pole. If the global asymmetry of the neutrino heating in the both of the poles develops in the later phases, the newly born neutron star might be kicked toward the north pole in the subsequent time.

astro-ph↗

arXiv2004

Magneto-driven Shock Waves in Core-Collapse Supernova

We perform a series of two-dimensional magnetohydrodynamic simulations of the rotational core-collapse of a magnetized massive star. We employ a realistic equation of state and take into account the neutrino cooling by the so-called leakage scheme. In this study we systematically investigate how the strong magnetic field and the rapid rotation affect the propagation of the shock waves. Our results show that in the case of the strong initial poloidal magnetic field, the toroidal magnetic field amplified by the differential rotation, becomes strong enough to generate a tightly collimated shock wave along the rotational axis. On the other hand, in the case of the weak initial magnetic field, although the differential rotation amplifies toroidal magnetic field over the long rotational period, the launched shock wave is weak and the shape of it becomes wider. The former case is expected to be accompanied by the formation of the so-called magnetar. Our models with rapid rotation and strong magnetic field can create a nozzle formed by the collimated shock wave. This might be the analogous situation of the collapsar that is plausible for the central engine of the Gamma-Ray Bursts.

astro-ph↗

arXiv2004

Modeling of the Peeling Process of Pressure-sensitive Adhesive Tapes with the Combination of Maxwell Elements

A simple model for the peeling process of pressure-sensitive adhesive tape is presented. The model consists of linear springs and dashpots and can be solved analytically. Based on the modeling, the curved profile of the peeling tape is spontaneously determined in terms of viscoelastic properties of adhesives. Using this model, two experimental results are discussed: critical peel rates in the peel force and the peel rate dependence of the detachment process of adhesive from the substrate.

cond-mat.other↗

arXiv2004

Statistical Significance of Small Scale Anisotropy in Arrival Directions of Ultra-High Energy Cosmic Rays

Recently, the High Resolution Fly's Eye (HiRes) experiment claims that there is no small scale anisotropy in the arrival distribution of ultra-high energy cosmic rays (UHECRs) above $E>10^{19}$ eV contrary to the Akeno Giant Air Shower Array (AGASA) observation. In this paper, we discuss the statistical significance of this discrepancy between the two experiments. We calculate arrival distribution of UHECRs above $10^{19}$ eV predicted by the source models constructed using the Optical Redshift Survey galaxy sample. We apply the new method developed by us for calculating arrival distribution in the presence of the galactic magnetic field. The great advantage of this method is that it enables us to calculate UHECR arrival distribution with lower energy ($\sim 10^{19}$ eV) than previous studies within reasonable time by following only the trajectories of UHECRs actually reaching the earth. It has been realized that the small scale anisotropy observed by the AGASA can be explained with the source number density $\sim 10^{-5 \sim -6}$ Mpc$^{-3}$ assuming weak extragalactic magnetic field ($B \le 1$ nG). We find that the predicted small scale anisotropy for this source number density is also consistent with the current HiRes data. We thus conclude that the statement by the HiRes experiment that they do not find small scale anisotropy in UHECR arrival distribution is not statistically significant at present. We also show future prospect of determining the source number density with increasing amount of observed data.

astro-ph↗

arXiv2004

Gravitational Radiation from Rotational Core Collapse: Effects of Magnetic Fields and Realistic Equation of States

We perform a series of two-dimensional, axisymmetric, magnetohydrodynamic simulations of the rotational collapse of a supernova core. In order to calculate the waveforms of the gravitational wave, we derive the quadrupole formula including the contributions from the electromagnetic fields. Recent stellar evolution calculations imply that the magnetic fields of the toroidal components are much stronger than those of the poloidal ones at the presupernova stage. Thus, we systematically investigate the effects of the toroidal magnetic fields on the amplitudes and waveforms. Furthermore, we employ the two kinds of the realistic equation of states, which are often used in the supernova simulations. Then, we investigate the effects of the equation of states on the gravitational wave signals. With these computations, we find that the peak amplitudes are lowered by an order of 10% for the models with the strongest toroidal magnetic fields. However, the peak amplitudes are mostly within sensitivity range of laser interferometers such as TAMA and the first LIGO for a source at a distance of 10 kpc. Furthermore, we point out that the amplitudes of second peaks are still within the detection limit of the first LIGO for the source, although the characteristics of second peaks are reduced by the magnetic fields. We stress the importance of the detection, since it will give us information about the angular momentum distribution of massive evolved stars. When we compare the gravitational waves from the two realistic equation of states, significant differences are not found, except that the typical frequencies of the gravitational wave become slightly higher for the softer equation of state.

astro-ph↗

arXiv2003

Constraints on the mass spectrum of primordial black holes and braneworld parameters from the high-energy diffuse photon background

We investigate the spectral shape of a high-energy diffuse photon emitted by evaporating primordial black holes (PBHs) in the Randall-Sundrum type II (RS2) braneworld. In their braneworld scenario, the nature of small PBHs is drastically modified from the ordinary four-dimensional case for the following two reasons. (i) dropping Hawking temperature, which equivalently lengthens the lifetime of the individual PBH due to the change of space-time topology and (ii) the effective increase of the total amount of PBHs caused by accretion during the earliest part of the radiation-dominated epoch, the brane high-energy phase. From studies of the expected spectral shape and its dependence on braneworld parameters, we obtain two qualitatively distinctive possibilities of constraints on the braneworld PBHs from the observations of diffuse high-energy photon background. If the efficiency of accretion in the high-energy phase exceeds a critical value, the existence of the extra dimension gives a more stringent upper bound on the abundance of PBHs than the 4D case and a small length scale for the extra dimension is favored. On the contrary, in the case below the critical accretion efficiency, we find that the constraint on the PBH abundance can be relaxed by a few orders of magnitude in exchange for the existence of the large extra dimension; its size may be even bounded in the region above 10^{19} times 4D Planck length scale provided the rest mass energy density of the PBHs relative to energy density of radiation is actually larger than 10^{-27} (4D upper bound) at their formation time. The above analytical studies are also confirmed numerically, and an allowed region for braneworld parameters and PBH abundance is clearly obtained.

astro-ph↗

arXiv2003

Nuclear pasta structure in hot neutron stars

Structure of cold and hot dense matter at subnuclear densities is investigated by quantum molecular dynamics (QMD) simulations. Obtained phase diagrams show that the density of the phase boundaries between the different nuclear structures decreases with increasing temperature due to the thermal expansion of nuclear matter region.

astro-ph↗

arXiv2003

A comprehensive study of neutrino spin-flavour conversion in supernovae and the neutrino mass hierarchy

Resonant spin-flavour (RSF) conversions of supernova neutrinos, which is induced by the interaction between the nonzero neutrino magnetic moment and supernova magnetic fields, are studied for both normal and inverted mass hierarchy. As the case for the pure matter-induced neutrino oscillation (Mikheyev--Smirnov--Wolfenstein (MSW) effect), we find that the RSF transitions are strongly dependent on the neutrino mass hierarchy as well as the value of $θ_{13}$. Flavour conversions are solved numerically for various neutrino parameter sets, with presupernova profile calculated by Woosley and Weaver. In particular, it is very interesting that the RSF-induced $ν_\rme\to\barν_\rme$ transition occurs, if the following conditions are all satisfied: the value of $μ_νB$ ($μ_ν$ is the neutrino magnetic moment, and $B$ is the magnetic field strength) is sufficiently strong, the neutrino mass hierarchy is inverted, and the value of $θ_{13}$ is large enough to induce adiabatic MSW resonance. In this case, the strong peak due to original $ν_\rme$ emitted from neutronization burst would exist in time profile of the neutrino events detected at the Super-Kamiokande detector. If this peak were observed in reality, it would provide fruitful information on the neutrino properties. On the other hand, characters of the neutrino spectra are also different between the neutrino models, but we find that there remains degeneracy among several models. Dependence on presupernova models is also discussed.

hep-ph↗

arXiv2003

Structure of cold nuclear matter at subnuclear densities by Quantum Molecular Dynamics

Structure of cold nuclear matter at subnuclear densities for the proton fraction $x=0.5$, 0.3 and 0.1 is investigated by quantum molecular dynamics (QMD) simulations. We demonstrate that the phases with slablike and rodlike nuclei, etc. can be formed dynamically from hot uniform nuclear matter without any assumptions on nuclear shape, and also systematically analyze the structure of cold matter using two-point correlation functions and Minkowski functionals. In our simulations, we also observe intermediate phases, which has complicated nuclear shapes. It is found out that these phases can be characterized as those with negative Euler characteristic. Our result implies the existence of these kinds of phases in addition to the simple ``pasta'' phases in neutron star crusts and supernova inner cores. In addition, we investigate the properties of the effective QMD interaction used in the present work to examine the validity of our results. The resultant energy per nucleon $ε_{n}$ of the pure neutron matter, the proton chemical $μ_{p}^{(0)}$ in pure neutron matter and the nuclear surface tension $E_{\rm surf}$ are generally reasonable in comparison with other nuclear interactions.

nucl-th↗

arXiv2003

Gravitational Radiation from Axisymmetric Rotational Core Collapse

We have done a series of two-dimensional hydrodynamic simulations of the rotational collapse of a supernova core in axisymmetry. We have employed a realistic equation of state (EOS) and taken into account electron captures and neutrino transport by the so-called leakage scheme. It is an important progress to apply the realistic EOS coupled with the microphysics to 2-D simulations for computing gravitational radiation in rotational core collapse. We have used the quadrupole formula to calculate the amplitudes and the waveforms of gravitational wave assuming the Newtonian gravity. From these computations, we have extended the conventional category of the gravitational waveforms. Our results have shown that the peak amplitudes of gravitational wave are mostly within the sensitivity range of the laser interferometers such as TAMA and first LIGO for a source at a distance of 10 kpc. Furthermore we have found that the amplitudes of the second peaks are within the detection limit of first LIGO for the source and first pointed out the importance of the detections, since they will give us the information as to the angular momentum distribution of evolved massive stars.

astro-ph↗