arXiv subjects

K. Sato

Publications and source records attributed to K. Sato.

159 records · Page 9Linked to original sources

arXiv2002

Gamma-Ray Burst Neutrino Background and Star Formation History in the Universe

We estimate the flux of the GRB neutrino background and compute the event rate at SK and TITAND in the collapsar model, assuming that GRB formation rate is proportional to the star formation rate. We find that the flux and the event rate depend sensitively on the mass-accretion rate. Although the detection of signals from GRBs seems to be difficult by SK, we find that we can detect them by TITAND (optimistically about 20 events per year in the energy range where the energy of anti-electron neutrino is larger than 50 MeV). Therefore, we show that we will obtain the informations on the mass-accretion rate of collapsar by observing the GRB neutrino background, which, in turn, should give us informations on the total explosion energy of GRBs.

astro-ph↗

arXiv2002

Earth effects on supernova neutrinos and their implications for neutrino parameters

We perform a detailed study of the Earth matter effects on supernova neutrinos with neutrino oscillation parameter LMA and small $θ_{13}$. The Earth effects show significant dependences on the neutrino path length inside the Earth and the value of $Δm^{2}_{12}$. We investigate rather optimistically a possibility that we can probe the value of $Δm^{2}_{12}$ by the Earth effects. We assume that $θ_{12}$ and the direction of the supernova are known with enough accuracy and that the resonance that occurs at higher density in supernova envelope is completely nonadiabatic. Further the neutrino spectra before neutrinos go through the Earth are assumed to be known. Then we show that making use of these dependences, we can obtain implication for the value of $Δm^{2}_{12}$ by comparing the observed energy spectrum to the predicted one. When SK detects neutrinos from supernova at 10kpc which traveled through the Earth (nadir angle $<$ 80 degree), $Δm^{2}_{12}$ can be determined with an accuracy of $\sim 10%$. In much of the neutrino-detection-time-$Δm^{2}_{12}$ plane, $Δm^{2}_{12}$ might be determined with an accuracy equal to or better than $\pm 0.5 \times 10^{-5} {\rm eV}^{2}$.

hep-ph↗

arXiv2001

Effects of Neutrino Oscillation on the Supernova Neutrino Spectrum

The effects of three-flavor neutrino oscillation on the supernova neutrino spectrum are studied. We calculate the expected event rate and energy spectra, and their time evolution at the Superkamiokande (SK) and the Sudbury Neutrino Observatory (SNO), by using a realistic neutrino burst model based on numerical simulations of supernova explosions. We also employ a realistic density profile based on a presupernova model for the calculation of neutrino conversion probability in supernova envelopes. These realistic models and numerical calculations allow us to quantitatively estimate the effects of neutrino oscillation in a more realistic way than previous studies. We then found that the degeneracy of the solutions of the solar neutrino problem can be broken by the combination of the SK and SNO detections of a future Galactic supernova.

hep-ph↗

arXiv2001

Propagation of UHECRs from the Sources in the Super-Galactic Plane

We have performed the detailed numerical simulations on the propagation of the UHE protons in the energy range $E=(10^{19.5} - 10^{22.0}$) eV in the relatively strong extra-galactic magnetic field with strength $B= (10, 100)$ nG within about 40 Mpc. In this case, the deflection angles of UHECRs become so large that the no counterparts problem is simply solved. As for the source distribution, we assumed that it is proportional to the number distribution of galaxies within the GZK sphere. We have found many clusters, which mean the small-scale anisotropy, in our simulations. It has been also shown that the observed energy spectrum is well reproduced in our models without any fine-tuned parameter. We have used the correlation value in order to investigate statistically the similarity between the distribution of arrival directions of UHECRs and that of galaxies. We have found that each correlation value for each parameter set begins to converge when the number of the detected events becomes ${\large O}(10^3)$. Since the expected number counts by the experiment of the next generation such as TA, HiRes, Auger, and EUSO are thought to be the order of $10^3$, we will be able to determine the source distribution and values of the parameters in this study in the very near future. Compared with the AGASA data, the significant anisotropy on the arrival directions of UHECRs are found in the analysis of first and second harmonics. This may originate from the incompleteness of the ORS database. This problem may be also solved if the source distribution is slightly changed. For example, this problem may be solved if we assume that UHECRs come from some of the galaxies such as AGNs and radio galaxies.

astro-ph↗

arXiv2001

Integration of GRACE and PYTHIA

We have successfully developed a technique to integrate an automatic event-generator generation system GRACE and a general-purpose event generator framework PYTHIA. The codes generated by GRACE are embedded in PYTHIA in the created event generator program. The embedded codes give information on parton-level hard interactions directly to PYTHIA. The choice of PDF is controlled by the ordinary parameter setting in PYTHIA. This technique enables us to create easy-to-handle event generators for any processes in hadron collisions. Especially, in virtue of large capability of GRACE, we can easily deal with those processes containing many (four or more) partons in the final state, such as multiple heavy particle productions. This project is being carried out as a collaboration between the Japanese Atlas group and the Minami-Tateya group, aiming at developing event generators for Tevatron and LHC experiments.

hep-ph↗

arXiv2001

The Earth effects on the supernova neutrino spectra

The Earth effects on the energy spectra of supernova neutrinos are studied. We analyze numerically the time-integrated energy spectra of neutrino in a mantle-core-mantle step function model of the Earth's matter density profile. We consider a realistic frame-work in which there are three active neutrinos whose mass squared differences and mixings are constrained by the present understanding of solar and atmospheric neutrinos. We find that the energy spectra change for some allowed mixing parameters. Especially, the expected number of events at SNO shows characteristic behavior with respect to energy, i.e. a great dip and peak. We show that observations of the Earth effect allow us to identify the solar neutrino solution and to probe the mixing angle $θ_{2}$.

hep-ph↗

arXiv2001

Implications of the Discovery of Millisecond Pulsar in SN 1987A

From the observation of a millisecond pulsar in SN 1987A, the following implications are obtained. 1) The pulsar spindown in SN 1987A is caused by radiating gravitational waves rather than by magnetic dipole radiation and/or relativistic pulsar winds. 2) A mildly deformed shock wave would be formed at the core-collapse and explosion in SN 1987A, which is consistent with the conclusion given in Nagataki (2000). 3) The gravitational waves from the pulsar should be detected in several years using a Fabry-Perot-Michelson interferometer as the gravitational detector, such as LIGO and TAMA. 4) The neutrino oscillation model is not a promising model for the explanation of the kick velocity of the pulsar in SN 1987A. The hydrodynamical instability model is more favored.

astro-ph↗

arXiv2001

Vacuum Brane and the Bulk Dynamics in Dilatonic Brane World

We investigate the dynamics of vacuum brane and the bulk in dilatonic brane world. We present exact dynamical solutions which describe the vacuum dilatonic brane world. We find that the solution has initial singularity and singularity at spatial infinity.

hep-th↗

arXiv1998

Contribution of Type Ia and Type II Supernovae for Intra-Cluster Medium Enrichment

The origin of the chemical composition of the intracluster medium (ICM) is discussed in this paper. In particular, the contribution from Type Ia supernovae (SNe Ia) to the ICM enrichment is shown to exist by adopting the fitting formulas which have been used in the analysis of the solar system abundances. Our analysis means that we can use the frequency of SNe Ia relative to SNe II as the better measure than $M_{Fe, SN Ia}/M_{Fe, total}$ for estimating the contribution of SNe Ia. Moreover, the chemical compositions of ICMs are shown to be similar to that of the solar system abundances. We can also reproduce the sulfur/iron abundance ratio within a factor of 2, which means that the abundance problem of sulfur needs not to be emphasized too strongly. We need more precise observations to conclude whether ICMs really suffer the shortage problem of sulfur or not.

astro-ph↗

arXiv1998

High Ratio of 44Ti/56Ni in Cas A and Axisymmetric Collapse-Driven Supernova Explosion

The large abundance ratio of $^{44}Ti/^{56}Ni$ in Cas A is puzzling. In fact, the ratio seems to be larger than the theoretical constraint derived by Woosley & Hoffman (1991). However, this constraint is obtained on the assumption that the explosion is spherically symmetric, whereas Cas A is famous for the asymmetric form of the remnant. Recently, Nagataki et al. (1997) calculated the explosive nucleosynthesis of axisymmetrically deformed collapse-driven supernova. They reported that the ratio of $^{44}Ti/^{56}Ni$ was enhanced by the stronger alpha-rich freezeout in the polar region. In this paper, we apply these results to Cas A and examine whether this effect can explain the large amount of $^{44}Ti$ and the large ratio of $^{44}Ti/^{56}Ni$. We demonstrate that the conventional spherically symmetric explosion model can not explain the $^{44}$Ti mass produced in Cas A if its lifetime is shorter than $\sim$ 80 years and the intervening space is transparent to the gamma-ray line from the decay of $^{44}$Ti. On the other hand, we show the axisymmetric explosion models can solve the problem. We expect the same effect from a three dimensionally asymmetric explosion, since the stronger alpha-rich freezeout will also occur in that case in the region where the larger energy is deposited.

astro-ph↗

arXiv1998

Dispersion of Inferred SNe Ia/SNe II Ratios for Current Models of Supernova Nucleosynthesis

We have estimated the dispersion of the inferred relative frequencies of Type-Ia and Type- II supernovae ($N_{Ia}/ N_{II}$) in our Galaxy by fitting the numerical results of supernova nucleosynthesis to the solar-system abundances. The ratio $N_{Ia}/ N_{II}$ is estimated to be 0.056--0.14, which is consistent with the observation, if the model of Woosley and Weaver (1995, WW95) is adopted for Type-II supernovae (SNe II). On the other hand, the upper limit of $N_{Ia}/ N_{II}$ becomes too large for the model of Hashimoto (1995, Ha95). However, Ha95 can fit the solar values better than WW95 as far as the abundant nuclei are concerned. These results mean that Ha95 can reproduce the main nuclei of the solar-system well and that WW95 can reproduce the solar values over a wide mass-number range. We also note that $N_{Ia}/ N_{II}$ tends to become smaller if the delayed detonation model is adopted for Type-Ia supernovae (SNe Ia). The dispersion of $N_{Ia}/ N_{II}$ obtained in the present investigation is larger than that concluded by Tsujimoto et al. (1995), which will have an influence on the estimate of the average life time of SNe Ia's progenitors and/or the star-formation rate history in our galaxy.

astro-ph↗

arXiv1997

Future Detection of Supernova Neutrino Burst and Explosion Mechanism

Future detection of a supernova neutrino burst by large underground detectors would give important information for the explosion mechanism of collapse-driven supernovae. We studied the statistical analysis for the future detection of a nearby supernova by using a numerical supernova model and realistic Monte-Carlo simulations of detection by the Super-Kamiokande detector. We mainly discuss the detectability of the signatures of the delayed explosion mechanism in the time evolution of the $\anue$ luminosity and spectrum. For a supernova at 10 kpc away from the Earth, we find that not only the signature is clearly discernible, but also the deviation of energy spectrum from the Fermi-Dirac (FD) distribution can be observed. The deviation from the FD distribution would, if observed, provide a test for the standard picture of neutrino emission from collapse-driven supernovae. For the $D$ = 50 kpc case, the signature of the delayed explosion is still observable, but statistical fluctuation is too large to detect the deviation from the FD distribution. We also propose a method for statistical reconstruction of the time evolution of $\anue$ luminosity and spectrum from data, by which we can get a smoother time evolution and smaller statistical errors than a simple, time-binning analysis. This method is useful especially when the available number of events is relatively small, e.g., a supernova in the LMC or SMC. Neutronization burst of $ν_e$'s produces about 5 scattering events when $D$ = 10 kpc and this signal is difficult to distinguish from $\anue p$ events.

astro-ph↗

arXiv1997

Evolution of the Luminosity Density in the Universe: Implications for the Nonzero Cosmological Constant

We show that evolution of the luminosity density of galaxies in the universe provides a powerful test for the geometry of the universe. Using reasonable galaxy evolution models of population synthesis which reproduce the colors of local galaxies of various morphological types, we have calculated the luminosity density of galaxies as a function of redshift $z$. Comparison of the result with recent measurements by the Canada-France Redshift Survey in three wavebands of 2800Å, 4400Å, and 1 micron at z<1 indicates that the Λ-dominated flat universe with λ_0 \sim 0.8 is favored, and the lower limit on λ_0 yields 0.37 (99% C.L.) or 0.53 (95% C.L.) if Ω_0+λ_0=1. The Einstein-de Sitter universe with (Ω_0, λ_0)=(1, 0) and the low-density open universe with (0.2, 0) are however ruled out with 99.86% C.L. and 98.6% C.L., respectively. The confidence levels quoted apply unless the standard assumptions on galaxy evolution are drastically violated. We have also calculated a global star formation rate in the universe to be compared with the observed rate beyond z \sim 2. We find from this comparison that spiral galaxies are formed from material accretion over an extended period of a few Gyrs, while elliptical galaxies are formed from initial star burst at z >~ 5 supplying enough amount of metals and ionizing photons in the intergalactic medium.

astro-ph↗

arXiv1996

Radiation from a class of string theoretic black holes

The emission of a scalar with low energy $ω$, from a $D (4\le D\le 8 )$ dimensional black hole with n charges is studied in both string and semiclassical calculations. In the lowest order in $ω$, the weak coupling string and semiclassical calculations agree provided that the Bekenstein--Hawking formula is valid and the effective central charge $c_{eff}=6$ for any D. When the next order in $ω$ is considered however, there is no agreement between the two schemes unless D=5, n=3 or D=4, n=4.

hep-th↗

arXiv1996

D-strings and F-strings from string loops

Since the background fields of the string low energy action are supposed to be the long range manifestation of a condensate of strings, the addition of world sheet actions to the low energy effective action needs some string theoretic explanation. In this paper we suggest that this may be understood, as being due to string loop effects. We first present arguments using an equation due to Tseytlin and then more rigorously in the particular case of type IIB theory by invoking the Fischler-Susskind effect. The argument provides further justification for ${\rm SL}(2,Z)$ duality between D-strings and F(fundamental)-strings. In an appendix we comment on recent attempts to relate the type IIA membrane to the 11-dimensional membrane.

hep-th↗