2,197 research outputs found
A study of Ultra-High-Energy Cosmic Ray propagation in one-dimensional simulations
Cosmic Rays have come to play an important role in understanding the universe,
and astroparticle physics has undergone major developments in the last
few decades. As such, several observatories have been set up with the purpose
of detecting these particles, and simulation frameworks have been developed in
order to further analyze their behavior by creating highly variable environments
and parameters.
This work covers the essential theory required to study propagation of Ultra-
High-Energy Cosmic Rays restricted to linear one-dimensional propagation
only; this includes the primary methods of energy loss during propagation,
mainly through reactions with the photon background like photo-pion production
and photo-disintegration, and additional cosmological effects. The study
was done using the CRPropa 3.0 simulation framework. To determine the best
possible maximum energy for the simulations, initial trials were done by testing
the GZK cutoff for multiple energy values, followed by an analysis of heavier
nuclei propagation.
As a final complete test run, a model of the cosmic ray spectrum for energies
above 1018 eV was made based on two data sets, one made from the average
composition of the whole CR energy spectrum, and the other from The
Pierre-Auger Observatory measurements for the high energy range. The results
showed that initial source composition was the determining factor in the shape
of the CR spectrum. These initial simulations done in this work will set the
ground for future more complex simulations and studies.Los rayos cósmicos juegan un papel importante en nuestro entendimiento del universo, por eso, la física de astropartículas ha sido desarrollada en gran medida en estas últimas décadas. Varios observatorios han sido construidos con el propósito de detectar estas partículas, y a su vez se han desarrollado programas de simulaciones para analizar su comportamiento usando ambientes y variables con una alta variabilidad. Este trabajo cubre la teoría necesaria para estudiar la propagación de rayos cósmicos de ultra-altas energías restringido a una sola dimensión; esto incluye las principales causas de pérdida de energía durante su propagación, principalmente a través de interacciones con el fondo de fotones como la fotoproducción de piones y fotodesintegración, así como otros efectos cosmológicos. Este estudio fue realizado con el programa de simulaciones CRPropa 3.0. Para determinar la mejor energía máxima para las simulaciones, los primeros ensayos comprobaron el límite GZK para múltiples valores de energía, seguido de un análisis de la propagación de núcleos más pesados. A manera de ensayo final, un modelo del espectro de rayos cósmicos para energías mayores a 1018 eV fue hecho basado en dos grupos de datos, uno a partir de la composición general promedio de todo el espectro de energías de los rayos cósmicos, y el otro a partir de mediciones hechas por el observatorio Pierre-Auger para altas energías. Los resultados muestran que la composición inicial de la fuente es el factor determinante en la forma del espectro. Las simulaciones iniciales hechas en este trabajo serán utilizadas como base para futuras y más complejas investigaciones.Trabajo de investigació
Absence of Electron Surfing Acceleration in a Two-Dimensional Simulation
Electron acceleration in high Mach number perpendicular shocks is
investigated through two-dimensional electrostatic particle-in-cell (PIC)
simulation. We simulate the shock foot region by modeling particles that
consist of three components such as incident protons and electrons and
reflected protons in the initial state which satisfies the Buneman instability
condition. In contrast to previous one-dimensional simulations in which strong
surfing acceleration is realized, we find that surfing acceleration does not
occur in two-dimensional simulation. This is because excited electrostatic
potentials have a two-dimensional structure that makes electron trapping
impossible. Thus, the surfing acceleration does not work either in itself or as
an injection mechanism for the diffusive shock acceleration. We briefly discuss
implications of the present results on the electron heating and acceleration by
shocks in supernova remnants.Comment: 12 pages, 4 figures, accepted for publication in ApJ
Galactoseismology: Discovery of Vertical Waves in the Galactic Disk
We present evidence for a Galactic North-South asymmetry in the number
density and bulk velocity of solar neighborhood stars. The number density
profile, which is derived from main-sequence stars in the Sloan Digital Sky
Survey, shows a (North - South)/(North + South) deficit at |z| ~ 400 pc and an
excess at |z| ~ 800 pc. The bulk velocity profile, which is derived from the
Sloan Extension for Galactic Understanding and Exploration, shows a gradual
trend across the Galactic midplane as well as smaller-scale features. We
speculate that the North-South asymmetry, which has the appearance of a
wavelike perturbation, is intrinsic to the disk. We explore the physics of this
phenomenon through an analysis of the linearized Boltzmann and Poisson
equations and through one-dimensional simulations. The perturbation may be
excited by the passage of a satellite galaxy or dark matter subhalo through the
Galactic disk, in which case we are witnessing a recent disk-heating event.Comment: 10 pages, 5 figures, accepted for publication in the Astrophysical
Journal Letter
Approximating strongly correlated spin and fermion wavefunctions with correlator product states
We explore correlator product states for the approximation of correlated
wavefunctions in arbitrary dimensions. We show that they encompass many
interesting states including Laughlin's quantum Hall wavefunction, Huse and
Elser's frustrated spin states, and Kitaev's toric code. We further establish
their relation to common families of variational wavefunctions, such as matrix
and tensor product states and resonating valence bond states. Calculations on
the Heisenberg and spinless Hubbard models show that correlator product states
capture both two-dimensional correlations (independent of system width) as well
as non-trivial fermionic correlations (without sign problems). In
one-dimensional simulations, correlator product states appear competitive with
matrix product states with a comparable number of variational parameters,
suggesting they may eventually provide a route to practically generalise the
density matrix renormalisation group to higher dimensions.Comment: Table 1 expanded, Table 2 updated, optimization method discussed,
discussions expanded in some sections, earlier work on similar wavefunctions
included in text and references, see also (arXiv:0905.3898). 5 pages, 1
figure, 2 tables, submitted to Phys. Rev.
Dynamical formation and interaction of bright solitary waves and solitons in the collapse of Bose-Einstein condensates with attractive interactions
We model the dynamics of formation of multiple, long-lived, bright solitary
waves in the collapse of Bose-Einstein condensates with attractive interactions
as studied in the experiment of Cornish et al. [Phys. Rev. Lett. 96 (2006)
170401]. Using both mean-field and quantum field simulation techniques, we find
that while a number of separated wave packets form as observed in the
experiment, they do not have a repulsive \pi phase difference that has been
previously inferred. We observe that the inclusion of quantum fluctuations
causes soliton dynamics to be predominantly repulsive in one dimensional
simulations independent of their initial relative phase. However, indicative
three-dimensional simulations do not support this conclusion and in fact show
that quantum noise has a negative impact on bright solitary wave lifetimes.
Finally, we show that condensate oscillations, after the collapse, may serve to
deduce three-body recombination rates, and that the remnant atom number may
still exceed the critical number for collapse for as long as three seconds
independent of the relative phases of the bright solitary waves.Comment: 14 pages, 5 figure
Feedback from Central Black Holes in Elliptical Galaxies: Two-dimensional Models Compared to One-dimensional Models
We extend the black hole (BH) feedback models of Ciotti, Ostriker, and Proga
to two dimensions. In this paper, we focus on identifying the differences
between the one-dimensional and two-dimensional hydrodynamical simulations. We
examine a normal, isolated galaxy subject to the cooling flow instability
of gas in the inner regions. Allowance is made for subsequent star formation,
Type Ia and Type II supernovae, radiation pressure, and inflow to the central
BH from mildly rotating galactic gas which is being replenished as a normal
consequence of stellar evolution. The central BH accretes some of the infalling
gas and expels a conical wind with mass, momentum, and energy flux derived from
both observational and theoretical studies. The galaxy is assumed to have low
specific angular momentum in analogy with the existing one-dimensional case in
order to isolate the effect of dimensionality. The code then tracks the
interaction of the outflowing radiation and winds with the galactic gas and
their effects on regulating the accretion. After matching physical modeling to
the extent possible between the one-dimensional and two-dimensional treatments,
we find essentially similar results in terms of BH growth and duty cycle
(fraction of the time above a given fraction of the Eddington luminosity). In
the two-dimensional calculations, the cool shells forming at 0.1--1 kpc from
the center are Rayleigh--Taylor unstable to fragmentation, leading to a
somewhat higher accretion rate, less effective feedback, and a more irregular
pattern of bursting compared to the one-dimensional case.Comment: 15 pages, 10 figures, ApJ 237:26. Updated to match published versio
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