scholarly journals Ultrahigh energy cosmic ray probes of large scale structure and magnetic fields

2004 ◽  
Vol 70 (4) ◽  
Author(s):  
Günter Sigl ◽  
Francesco Miniati ◽  
Torsten A. Enßlin
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Cosmic Ray ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Ultrahigh Energy

scholarly journals The Imprint of Large-scale Structure on the Ultrahigh-energy Cosmic-Ray Sky

2021 ◽  
Vol 913 (1) ◽  
pp. L13
Author(s):  
Chen Ding ◽  
Noémie Globus ◽  
Glennys R. Farrar
Keyword(s):  
Large Scale ◽  
Cosmic Ray ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Ultrahigh Energy

scholarly journals Primordial Magnetic Field Effects on the CMB and Large-Scale Structure

2010 ◽  
Vol 2010 ◽  
pp. 1-19 ◽  
Author(s):  
Dai G. Yamazaki ◽  
Kiyotomo Ichiki ◽  
Toshitaka Kajino ◽  
Grant J. Mathews
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Large Scale ◽  
Large Scale Structure ◽  
Big Bang ◽  
Scale Structure ◽  
Magnetic Field Effects ◽  
Power Spectral ◽  
Primordial Magnetic Field ◽  
The Big Bang

Magnetic fields are everywhere in nature, and they play an important role in every astronomical environment which involves the formation of plasma and currents. It is natural therefore to suppose that magnetic fields could be present in the turbulent high-temperature environment of the big bang. Such a primordial magnetic field (PMF) would be expected to manifest itself in the cosmic microwave background (CMB) temperature and polarization anisotropies, and also in the formation of large-scale structure. In this paper, we summarize the theoretical framework which we have developed to calculate the PMF power spectrum to high precision. Using this formulation, we summarize calculations of the effects of a PMF which take accurate quantitative account of the time evolution of the cutoff scale. We review the constructed numerical program, which is without approximation, and an improvement over the approach used in a number of previous works for studying the effect of the PMF on the cosmological perturbations. We demonstrate how the PMF is an important cosmological physical process on small scales. We also summarize the current constraints on the PMF amplitudeBλand the power spectral indexnBwhich have been deduced from the available CMB observational data by using our computational framework.

scholarly journals Cluster Magnetic Fields from Large-Scale Structure and Galaxy Cluster Shocks

2006 ◽  
Vol 642 (1) ◽  
pp. L1-L4 ◽  
Author(s):  
Mikhail V. Medvedev ◽  
Luis O. Silva ◽  
Marc Kamionkowski
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Galaxy Cluster ◽  
Large Scale Structure ◽  
Scale Structure

A Faraday Rotation Search for Magnetic Fields in Large‐scale Structure

2006 ◽  
Vol 637 (1) ◽  
pp. 19-26 ◽  
Author(s):  
Yongzhong Xu ◽  
Philipp P. Kronberg ◽  
Salman Habib ◽  
Quentin W. Dufton
Keyword(s):  
Magnetic Fields ◽  
Faraday Rotation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure

scholarly journals Magnetic fields in our Milky Way Galaxy and nearby galaxies

2012 ◽  
Vol 8 (S294) ◽  
pp. 213-224 ◽  
Author(s):  
JinLin Han
Keyword(s):  
Star Formation ◽  
Magnetic Fields ◽  
Large Scale ◽  
Milky Way ◽  
Spiral Galaxies ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Measure Data ◽  
Submillimeter Wavelength ◽  
Nearby Galaxies

AbstractMagnetic fields in our Galaxy and nearby galaxies have been revealed by starlight polarization, polarized emission from dust grains and clouds at millimeter and submillimeter wavelength, the Zeeman effect of spectral lines or maser lines from clouds or clumps, diffuse radio synchrotron emission from relativistic electrons in interstellar magnetic fields, and the Faraday rotation of background radio sources as well as pulsars for our Milky Way. It is easy to get a global structure for magnetic fields in nearby galaxies, while we have observed many details of magnetic fields in our Milky Way, especially by using pulsar rotation measure data. In general, magnetic fields in spiral galaxies probably have a large-scale structure. The fields follow the spiral arms with or without the field direction reversals. In the halo of spiral galaxies magnetic fields exist and probably also have a large-scale structure as toroidal and poloidal fields, but seem to be slightly weaker than those in the disk. In the central region of some galaxies, poloidal fields have been detected as vertical components. Magnetic field directions in galaxies seem to have been preserved during cloud formation and star formation, from large-scale diffuse interstellar medium to molecular clouds and then to the cloud cores in star formation regions or clumps for the maser spots. Magnetic fields in galaxies are passive to dynamics.

COSMOLOGICAL SHOCK WAVES IN THE LARGE SCALE STRUCTURE OF THE UNIVERSE

2013 ◽  
Vol 23 ◽  
pp. 386-390
Author(s):  
RENYI MA ◽  
DONGSU RYU ◽  
HYESUNG KANG
Keyword(s):  
Shock Waves ◽  
Galaxy Clusters ◽  
Large Scale ◽  
Gamma Ray ◽  
High Redshift ◽  
Cosmic Ray ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Weak Shocks ◽  
The Universe

Based on the cosmological hydrodynamic simulation, we study the properties of shock waves formed during the formation of the large scale structure (LSS) of the universe, and investigate their contribution to the cosmic ray (CR) fraction in the intergalactic medium (IGM). It is found that while strong accretion shocks prevail at high redshift, weak internal shocks become dominant in the intracluster medium (ICM) as galaxy clusters form and virialize at low redshift, z < 1. The accumulated CR proton energy is likely to be less than 10 % of the thermal energy in the ICM, since weak shocks of M ≲ 3 are most abundant. This is consistent with the upper limit constrained by radio and gamma-ray observations of galaxy clusters. In the warm-hot medium (WHIM) inside filaments, CRs and gas could be almost in energy equipartition, since relatively stronger shocks of 5 ≲ M ≲ 10 are dominant there. We suggest that the non-thermal emissions from the CR electrons and protons accelerated by cosmological shock waves could provide a new way to detect the WHIM of the universe.

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