scholarly journals Ensemble fluctuations of the cosmic ray energy spectrum and the intergalactic magnetic field

2015 ◽  
Vol 91 (12) ◽  
Author(s):  
A. D. Supanitsky ◽  
G. Medina-Tanco
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Ray ◽  
Intergalactic Magnetic Field

scholarly journals Cosmic ray acceleration by shocks: spectral steepening due to turbulent magnetic field amplification

2019 ◽  
Vol 488 (2) ◽  
pp. 2466-2472 ◽  
Author(s):  
A R Bell ◽  
J H Matthews ◽  
K M Blundell
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Ray ◽  
Field Amplification ◽  
Cosmic Ray Acceleration

Abstract We show that the energy required to turbulently amplify magnetic field during cosmic ray (CR) acceleration by shocks extracts energy from the CR and steepens the CR energy spectrum.

scholarly journals Further measurements of the cosmic-ray energy spectrum

1937 ◽  
Vol 159 (896) ◽  
pp. 1-18 ◽  
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Glass Plate ◽  
Cosmic Ray ◽  
Expansion Ratio ◽  
Initial Slope ◽  
Oxygen Mixture ◽  
Water Mixture ◽  
Small Distortion ◽  
Normal Lens

The work already described (Blackett and Brode 1936) of determining the energy spectrum of cosmic-ray particles, by measuring the curvature of their tracks with a counter-controlled cloud chamber in a strong magnetic field, has been continued. A new set of 641 tracks in a magnetic field of 12,000-14,000 gauss have been measured, making with the 188 already reported a total of 829 tracks. An expansion ratio of about 1·08 was used, with an argon-oxygen mixture for the gas and with an ethyl alcohol and water mixture for the liquid. In order to avoid the inconveniently large distortions of the lenses previously used, Messrs Taylor, Taylor and Hobson supplied a new pair of 35 mm. f /2 ciné lenses, which were especially adjusted to have a very small distortion, when used with a 1·2 cm. glass plate as the roof of the chamber: fig. 1 shows the distortion curves, that is, the image curvature c as a function of the displacement x , both for the normal and for these special lenses. The initial slope of the curve for the new lens is about one-fifth of that for the normal lens, while the deviation from linearity is only reduced in much less degree. This confirms the statement (Blackett and Brode 1936, p. 578) of Mr A. Warmisham of Taylor, Taylor and Hobson, Ltd., that the coefficient a 1 of the linear term, which gives the initial slope of the curve c = f ( x ), is easily under the designer’s control, whereas the coefficient a 2 of the cubic term, which governs the departure from linearity, is roughly a constant for a given type of lens. The use of these lenses has greatly facilitated the work.

scholarly journals Ultrahigh energy cosmic ray deflection by the intergalactic magnetic field

2021 ◽  
Vol 104 (8) ◽  
Author(s):  
Andrés Arámburo-García ◽  
Kyrylo Bondarenko ◽  
Alexey Boyarsky ◽  
Dylan Nelson ◽  
Annalisa Pillepich ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Cosmic Ray ◽  
Ultrahigh Energy ◽  
Intergalactic Magnetic Field

Gradient of galactic cosmic rays normal to the solar equatorial plane

1968 ◽  
Vol 46 (10) ◽  
pp. S981-S984 ◽  
Author(s):  
D. Patel ◽  
V. Sababhai ◽  
G. Subramanian
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Rays ◽  
Interplanetary Magnetic Field ◽  
Equatorial Plane ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Cosmic Ray Intensity ◽  
Positive Exponent ◽  
Ray Density

Predictions concerning the anisotropy of galactic cosmic rays due to a gradient of cosmic-ray density perpendicular to the solar equatorial plane have been verified experimentally as follows. (1) The energy spectrum of the variation of the semidiurnal component has a positive exponent. (2) The diurnal and the semidiurnal components are oriented with respect to the interplanetary magnetic field. (3) A deficiency of cosmic-ray intensity, Tmin, is observed along the direction of the interplanetary magnetic field on days when the energy spectrum of the diurnal variation has an exponent different from zero.

scholarly journals Can the Local Bubble explain the radio background?

2021 ◽  
Vol 502 (2) ◽  
pp. 2807-2814
Author(s):  
Martin G H Krause ◽  
Martin J Hardcastle
Keyword(s):  
Magnetic Field ◽  
Energy Density ◽  
Radio Emission ◽  
Magnetic Energy ◽  
Cosmic Ray ◽  
Observational Constraints ◽  
Local Bubble ◽  
Magnetic Energy Density ◽  
Magnetic Field Model ◽  
Radio Background

ABSTRACT The ARCADE 2 balloon bolometer along with a number of other instruments have detected what appears to be a radio synchrotron background at frequencies below about 3 GHz. Neither extragalactic radio sources nor diffuse Galactic emission can currently account for this finding. We use the locally measured cosmic ray electron population, demodulated for effects of the Solar wind, and other observational constraints combined with a turbulent magnetic field model to predict the radio synchrotron emission for the Local Bubble. We find that the spectral index of the modelled radio emission is roughly consistent with the radio background. Our model can approximately reproduce the observed antenna temperatures for a mean magnetic field strength B between 3 and 5 nT. We argue that this would not violate observational constraints from pulsar measurements. However, the curvature in the predicted spectrum would mean that other, so far unknown sources would have to contribute below 100 MHz. Also, the magnetic energy density would then dominate over thermal and cosmic ray electron energy density, likely causing an inverse magnetic cascade with large variations of the radio emission in different sky directions as well as high polarization. We argue that this disagrees with several observations and thus that the magnetic field is probably much lower, quite possibly limited by equipartition with the energy density in relativistic or thermal particles (B = 0.2−0.6 nT). In the latter case, we predict a contribution of the Local Bubble to the unexplained radio background at most at the per cent level.

scholarly journals Measurements of the time-dependent cosmic-ray Sun shadow with seven years of IceCube data: Comparison with the Solar cycle and magnetic field models

2021 ◽  
Vol 103 (4) ◽  
Author(s):  
M. G. Aartsen ◽  
R. Abbasi ◽  
M. Ackermann ◽  
J. Adams ◽  
J. A. Aguilar ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Cosmic Ray ◽  
Time Dependent ◽  
Data Comparison

scholarly journals The measurement of the energy of cosmic rays - II—The curvature measurements and the energy spectrum

1936 ◽  
Vol 154 (883) ◽  
pp. 573-587 ◽  
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Rays ◽  
Magnetic Fields ◽  
Strong Magnetic Fields ◽  
The Earth ◽  
Primary Particles ◽  
Curvature Measurements

Both the penetrating power of the cosmic rays through material ab­sorbers and their ability to reach the earth in spite of its magnetic field, make it certain that the energy of many of the primary particles must reach at least 10 11 e-volts. However, the energy measurements by Kunze, and by Anderson, using cloud chambers in strong magnetic fields, have extended only to about 5 x 10 9 e-volts. Particles of greater energy were reported, but the curvature of their tracks was too small to be measured with certainty. We have extended these energy measurements to somewhat higher energies, using a large electro-magnet specially built for the purpose and described in Part I. As used in these experiments, the magnet allowed the photography of tracks 17 cm long in a field of about 14,000 gauss. The magnet weighed about 11,000 kilos and used a power of 25 kilowatts.

ON A RESULT CONCERNING THE BEHAVIOR OF A RELATIVISTIC QUANTUM SYSTEM IN THE COSMIC STRING SPACETIME

2009 ◽  
Vol 24 (08n09) ◽  
pp. 1549-1556 ◽  
Author(s):  
V. B. BEZERRA ◽  
GEUSA DE A. MARQUES
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Dirac Equation ◽  
Quantum System ◽  
Relativistic Electron ◽  
Coulomb Potential ◽  
Cosmic String ◽  
Relativistic Quantum

We consider the problem of a relativistic electron in the presence of a Coulomb potential and a magnetic field in the background spacetime corresponding to a cosmic string. We find the solution of the corresponding Dirac equation and determine the energy spectrum of the particle.

scholarly journals Measurement of the Cosmic Ray Helium Energy Spectrum from 70 GeV to 80 TeV with the DAMPE Space Mission

2021 ◽  
Vol 126 (20) ◽  
Author(s):  
F. Alemanno ◽  
Q. An ◽  
P. Azzarello ◽  
F. C. T. Barbato ◽  
P. Bernardini ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
Space Mission

scholarly journals The Origin and Dynamical Effects of the Magnetic Fields and Cosmic Rays in the Disk of the Galaxy

1970 ◽  
Vol 39 ◽  
pp. 168-183
Author(s):  
E. N. Parker
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Magnetic Fields ◽  
Dynamical Behavior ◽  
Cosmic Ray ◽  
Interested Reader ◽  
Written Text ◽  
The Galaxy ◽  
Basic Ideas ◽  
The Magnetic Field

The topic of this presentation is the origin and dynamical behavior of the magnetic field and cosmic-ray gas in the disk of the Galaxy. In the space available I can do no more than mention the ideas that have been developed, with but little explanation and discussion. To make up for this inadequacy I have tried to give a complete list of references in the written text, so that the interested reader can pursue the points in depth (in particular see the review articles Parker, 1968a, 1969a, 1970). My purpose here is twofold, to outline for you the calculations and ideas that have developed thus far, and to indicate the uncertainties that remain. The basic ideas are sound, I think, but, when we come to the details, there are so many theoretical alternatives that need yet to be explored and so much that is not yet made clear by observations.

Sign in / Sign up

Export Citation Format

Share Document