The Angular Dispersion of the Cosmic Radiation in the Upper Atmosphere Resulting from Deflections of Low Energy Particles in the Earth's Magnetic Field

1939 ◽  
Vol 56 (3) ◽  
pp. 226-231 ◽  
Author(s):  
T. H. Johnson
Keyword(s):  
Magnetic Field ◽  
Cosmic Radiation ◽  
Low Energy ◽  
Upper Atmosphere ◽  
Angular Dispersion ◽  
Earth’S Magnetic Field ◽  
Earth's Magnetic Field

scholarly journals Drivers of Upper Atmosphere Climate Change

Eos ◽  
2020 ◽  
Vol 101 ◽  
Author(s):  
Sarah Stanley
Keyword(s):  
Climate Change ◽  
Magnetic Field ◽  
Carbon Dioxide ◽  
Upper Atmosphere ◽  
Earth’S Magnetic Field ◽  
Temperature Trends ◽  
Earth's Magnetic Field ◽  
New Research

New research confirms the influence of carbon dioxide on long-term temperature trends in the upper atmosphere, but changes in Earth’s magnetic field also play a key role.

LOW ENERGY γ-RAY DETECTION (E ≤ 30 GEV): EFFECT OF EARTH'S MAGNETIC FIELD AND A NOVEL TRIGGER TECHNIQUE

2005 ◽  
Vol 20 (29) ◽  
pp. 7006-7008 ◽  
Author(s):  
◽  
R. DE LOS REYES ◽  
E. OÑA-WILHELMI ◽  
J. L. CONTRERAS ◽  
O. C. DE JAGER ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Low Energy ◽  
Extensive Air Showers ◽  
Large Collection ◽  
Earth’S Magnetic Field ◽  
Air Showers ◽  
Cherenkov Telescope ◽  
Earth's Magnetic Field ◽  
Γ Ray

Here we discuss two related aspects of the detection of low energy gammas by IACT's (Imaging Atmospheric Cherenkov Telescope): the effect of the Earth's magnetic field and a possible novel trigger technique. The Earth's magnetic field affects the development of extensive air showers (EAS), spreading the collected photons and, therefore, decreasing the sensitivity of the Cherenkov telescope. The new effects that appear in low energy showers can be partially offset modifying the trigger criteria. The result is a large collection area (> 1000 m2) below 10 GeV for a typical 17 m class telescope, increasing its sensitivity at these energies.

scholarly journals II. The lunar diurnal magnetic variation at Greenwich and other observatories

1926 ◽  
Vol 225 (626-635) ◽  
pp. 49-91 ◽  
Keyword(s):  
Magnetic Field ◽  
Electrical Conductivity ◽  
Diurnal Variation ◽  
Solid Earth ◽  
Upper Atmosphere ◽  
Earth’S Magnetic Field ◽  
Terrestrial Magnetism ◽  
Magnetic Variation ◽  
Earth's Magnetic Field ◽  
The Subject

§ 1. The present research forms part of a wider investigation of terrestrial magnetism, the main object of which is the study of certain electrical phenomena that are associated with solar emissions absorbed in the upper atmosphere, and with the systematic motions of the upper atmosphere. The subject also bears on the electrical conductivity of the solid earth and oceans. The results are briefly discussed from this standpoint in Part IV. The immediate subject of the paper is the lunar diurnal variation of the earth’s magnetic field, and particularly that of the declination at Greenwich, although the results of extensive reductions for other elements, at Batavia, Zikawei, and Pavlovsk, are also included.

scholarly journals The electrical conductivity of an ionized gas in a magnetic field, with applications to the solar atmosphere and the ionosphere

1945 ◽  
Vol 183 (995) ◽  
pp. 453-479 ◽  
Keyword(s):  
Magnetic Field ◽  
Transverse Magnetic ◽  
Upper Atmosphere ◽  
Exact Methods ◽  
Earth’S Magnetic Field ◽  
Dynamo Theory ◽  
Ionized Gas ◽  
Earth’S Atmosphere ◽  
Earth's Magnetic Field ◽  
Earth's Atmosphere

The methods of Chapman and Enskog are used to discuss conduction of electricity and diffusion currents in an ionized gas with several constituents, in a transverse magnetic field. The free-path formula for the conductivity is compared with that derived by the exact methods. The two formulae are identical in form if a correction is applied to the usual freepath method; this correction robs the method of much of its simplicity. The uncorrected freepath method, however, gives correct results for the electron contribution to the conductivity in all practical cases; and for the ion contribution if a large number of neutral molecules are present— e.g. in the earth’s upper atmosphere, about 5 x 105 times the number of ions (of both signs). Numerical values are given for the conductivity in the sun’s outer layers and in the earth’s upper atmosphere. Mechanical forces due to currents induced in moving material are shown to be very important in the sun, and in the F-layer of the earth’s atmosphere. The solar results are used to discuss the motion of solar prominences and eruptions. In the earth’s atmosphere, the observed collision frequencies of electrons are shown to imply upper limits for ion-densities in the E and F layers. The integral conductivities of the E and F layers are estimated, and it is shown that, on the dynamo theory of the lunar variation of the earth’s magnetic field, tidal oscillations in these layers must be between 100 and 1000 times as great as those at the ground. Diamagnetism and drift currents are shown to make negligible contributions to the lunar and solar variations of the earth’s magnetic field. In an Appendix, the applicability of Boltzmann’s equation to strongly ionized gases is discussed.

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