52 research outputs found
A New Method for Calculating Arrival Distribution of Ultra-High Energy Cosmic Rays above 10^19 eV with Modifications by the Galactic Magnetic Field
We present a new method for calculating arrival distribution of UHECRs
including modifications by the galactic magnetic field. We perform numerical
simulations of UHE anti-protons, which are injected isotropically at the earth,
in the Galaxy and record the directions of velocities at the earth and outside
the Galaxy for all of the trajectories. We then select some of them so that the
resultant mapping of the velocity directions outside the Galaxy of the selected
trajectories corresponds to a given source location scenario, applying
Liouville's theorem. We also consider energy loss processes of UHE protons in
the intergalactic space. Applying this method to our source location scenario
which is adopted in our recent study and can explain the AGASA observation
above 4 \times 10^{19} eV, we calculate the arrival distribution of UHECRs
including lower energy (E>10^19 eV) ones. We find that our source model can
reproduce the large-scale isotropy and the small-scale anisotropy on UHECR
arrival distribution above 10^19 eV observed by the AGASA. We also demonstrate
the UHECR arrival distribution above 10^19 eV with the event number expected by
future experiments in the next few years. The interesting feature of the
resultant arrival distribution is the arrangement of the clustered events in
the order of their energies, reflecting the directions of the galactic magnetic
field. This is also pointed out by Alvarez-Muniz et al.(2002). This feature
will allow us to obtain some kind of information about the composition of
UHECRs and the magnetic field with increasing amount of data.Comment: 10 pages, 8 figures, to appear in the Astrophysical Journa
Quantization of scalar perturbations in brane-world inflation
We consider a quantization of scalar perturbations about a de Sitter brane in
a 5-dimensional anti-de Sitter (AdS) bulk spacetime. We first derive the second
order action for a master variable for 5-dimensional gravitational
perturbations. For a vacuum brane, there is a continuum of normalizable
Kaluza-Klein (KK) modes with . There is also a light radion mode with
which satisfies the junction conditions for two branes, but is
non-normalizable for a single brane model. We perform the quantization of these
bulk perturbations and calculate the effective energy density of the projected
Weyl tensor on the barne. If there is a test scalar field perturbation on the
brane, the mode together with the zero-mode and an infinite ladder
of discrete tachyonic modes become normalizable in a single brane model. This
infinite ladder of discrete modes as well as the continuum of KK modes with
introduce corrections to the scalar field perturbations at first-order
in a slow-roll expansion. We derive the second order action for the
Mukhanov-Sasaki variable coupled to the bulk perturbations which is needed to
perform the quantization and determine the amplitude of scalar perturbations
generated during inflation on the brane.Comment: 14 page
Cosmic Magnetic Fields and Their Influence on Ultra-High Energy Cosmic Ray Propagation
We discuss the influence of large scale cosmic magnetic fields on the
propagation of hadronic cosmic rays above 10^19 eV based on large scale
structure simulations. Our simulations suggest that rather substantial
deflection up to several tens of degrees at 10^20 eV are possible for nucleon
primaries. Further, spectra and composition of cosmic rays from individual
sources can depend on magnetic fields surrounding these sources in
intrinsically unpredictable ways. This is true even if deflection from such
individual sources is small. We conclude that the influence of large scale
cosmic magnetic fields on ultra-high energy cosmic ray propagation is currently
hard to quantify. We discuss possible reasons for discrepant results of
simulations by Dolag et al. which predict deflections of at most a few degrees
for nucleons. We finally point out that even in these latter simulations a
possible heavy component would in general suffer substantial deflection.Comment: 10 latex pages, 9 ps figues, for the proceedings of the Cosmic Ray
International Seminar (CRIS), May 31 - June 4 200
Revision of the Selection Function of the Optical Redshift Survey using the Sloan Digital Sky Survey Early Data Release: Toward an Accurate Estimate of Source Number Density of Ultra-High Energy Cosmic Rays
If Ultra-High Energy Cosmic Rays (UHECRs) are originated from nearby
galaxies, modeling of the distribution of nearby galaxies is important to an
accurate estimate the source number density of UHECRs. We investigate
uncertainty of the selection function of the Optical Redshift Survey (ORS),
which we used to construct a source model of UHECRs. The investigation is based
on a comparison of numbe counts of ORS galaxies with those of the spectroscopic
sample of the Sloan Digital Sky Survey (SDSS) Early Data Release (EDR). We
carefully count galaxies in the same absolute magnitude bin from the two
samples. We find a slight systematic overestimate of the ORS counts outside
5000 km s by about a factor of 2. We revise the selection function of
the ORS assuming that the SDSS counts are correct. Our revision is based on the
absorption given in the ORS catalog as well as that computed from Schlegel et
al. (1998), which is systematically larger than the former by
mag in the region of low absorption. It is found that introduction of Schlegel
et al.'s absorption changes one of the parameters of the ORS selection function
by more than 10%. The revision should be taken into account in the future
analysis of the source number density of UHECRs based on the ORS. Using the
revised selection function, we determine the global structure of the Local
Supercluster (LSC) with a source model of UHECRs, that is, a number-density
model consisting of a uniform spherical halo and an exponential disk. We find
that the revision is insignificant in terms of the structure of the LSC.
However, the revised selection function will be useful to other studies such as
peculiar velocity and correlation function.Comment: 22 pages, 13 figures. accepted for publication in PAS
Ultra-high energy cosmic rays from a finite number of point sources
We have calculated the probability that the clustering of arrival directions
of ultra-high energy cosmic rays (UHECRs) is consistent with a finite number of
uniformly distributed proton sources. The case of a continuous source
distribution is reached only for an unrealisticly high source density, . Even for densities as large as , less than
half of the observed cluster are on average by chance. For the best-fit value
derived from the AGASA data, the probability
that at least one observed cluster is from a true point source is larger than
99.97%, while on average almost all observed clusters are true. The best-fit
value found is comparable to the density of AGNs and consistent with the recent
HiRes stereo data. In this scenario, the Pierre Auger Observatory will not only
establish the clustering of UHECRs but also determine the density of UHECR
sources within a factor of a few after one year of data taking.Comment: 12 pages, 4 figures; v2 matches version to appea
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 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 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
( 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 Mpc assuming weak
extragalactic magnetic field ( 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.Comment: 8 pages, 7 figure
Arrival Distribution of Ultra-High Energy Cosmic Rays: Prospects for the Future
We predict the arrival distribution of UHECRs above eV
with the event number expected by future experiments in the next few years. We
perform event simulations with the source model which is adopted in our recent
study and can explain the current AGASA observation. At first, we calculate the
harmonic amplitude and the two point correlation function for the simulated
event sets. We find that significant anisotropy on large angle scale will be
observed when cosmic rays above eV are detected
by future experiments. The statistics of the two point correlation function
will also increase. The angle scale at which the events have strong correlation
with each other corresponds to deflection angle of UHECR in propagating in the
EGMF, which in turn can be determined by the future observations. We further
investigate the relation between the number of events clustered at a direction
and the distance of their sources. Despite the limited amount of data, we find
that the C2 triplet events observed by the AGASA may originate from the source
within 100 Mpc. Merger galaxy Arp 299 (NGC 3690 + IC 694) is the best candidate
for their source. If data accumulate, the UHECR sources within Mpc
can be identified from observed event clusterings significantly. This will
provide some kinds of information about poorly known parameters which influence
the propagation of UHECRs, such as extragalactic and galactic magnetic field,
chemical composition of observed cosmic rays. Also, we will reveal their origin
with our method to identify the sources of UHECR. Finally, we predict the
arrival distribution of UHECRs above eV, which is expected to be
observed if the current HiRes spectrum is correct, and discuss their
statistical features and implications.Comment: 11 pages, 9 figures. accepted version for publication in Ap
Dynamical Stability of Six-dimensional Warped Flux Compactification
We show the dynamical stability of a six-dimensional braneworld solution with
warped flux compactification recently found by the authors. We consider linear
perturbations around this background spacetime, assuming the axisymmetry in the
extra dimensions. The perturbations are expanded by scalar-, vector- and
tensor-type harmonics of the four-dimensional Minkoswki spacetime and we
analyze each type separately. It is found that there is no unstable mode in
each sector and that there are zero modes only in the tensor sector,
corresponding to the four-dimensional gravitons. We also obtain the first few
Kaluza-Klein modes in each sector.Comment: 46 pages, 8 figures. Version to appear in JCA
CRT: A numerical tool for propagating ultra-high energy cosmic rays through Galactic magnetic field models
Deflection of ultra high energy cosmic rays (UHECRs) by the Galactic magnetic
field (GMF) may be sufficiently strong to hinder identification of the UHECR
source distribution. A common method for determining the effect of GMF models
on source identification efforts is backtracking cosmic rays. We present the
public numerical tool CRT for propagating charged particles through Galactic
magnetic field models by numerically integrating the relativistic equation of
motion. It is capable of both forward- and back-tracking particles with varying
compositions through pre-defined and custom user-created magnetic fields. These
particles are injected from various types of sources specified and distributed
according to the user. Here, we present a description of some source and
magnetic field model implementations, as well as validation of the integration
routines.Comment: 12 pages, 9 figure
Cross-Correlation between UHECR Arrival Distribution and Large-Scale Structure
We investigate correlation between the arrival directions of
ultra-high-energy cosmic rays (UHECRs) and the large-scale structure (LSS) of
the Universe by using statistical quantities which can find the angular scale
of the correlation. The Infrared Astronomical Satellite Point Source Redshift
Survey (IRAS PSCz) catalog of galaxies is adopted for LSS. We find a positive
correlation of the highest energy events detected by the Pierre Auger
Observatory (PAO) with the IRAS galaxies inside within the angular
scale of . This positive correlation observed in the southern
sky implies that a significant fraction of the highest energy events comes from
nearby extragalactic objects. We also analyze the data of the Akeno Giant Air
Shower Array (AGASA) which observed the northern hemisphere, but the obvious
signals of positive correlation with the galaxy distribution are not found.
Since the exposure of the AGASA is smaller than the PAO, the cross-correlation
in the northern sky should be tested using a larger number of events detected
in the future. We also discuss the correlation using the all-sky combined data
sets of both the PAO and AGASA, and find a significant correlation within . These angular scales can constrain several models of intergalactic
magnetic field. These cross-correlation signals can be well reproduced by a
source model in which the distribution of UHECR sources is related to the IRAS
galaxies.Comment: 21 pages,7 figure
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