scholarly journals On External Radio Emission from the Earth's Outer Atmosphere

1964 ◽  
Vol 17 (1) ◽  
pp. 63 ◽  
Author(s):  
GRA Ellis
Keyword(s):  
Radio Emission ◽  
Electron Energy ◽  
Geomagnetic Field ◽  
External Radiation ◽  
Frequency Range ◽  
Radiated Power ◽  
Cyclotron Radiation ◽  
Outer Atmosphere

The possibility is considered that cyclotron radiation, generated by fast bunched electrons in the Earth's outer atmosphere, may be observable outside the geomagnetic field. It is shown that the intensity and other properties of such external radiation may be deduced from the known characteristics of v.1.f. hooks. It appears likely that the radiation will occur as short bursts in the frequency range from 200 to 1000 kc/s. The total radiated power may be from 1 to 1000 W, depending on the electron energy.

scholarly journals Electron radiated power in cyclotron radiation emission spectroscopy experiments

2019 ◽  
Vol 99 (5) ◽  
Author(s):  
A. Ashtari Esfahani ◽  
V. Bansal ◽  
S. Böser ◽  
N. Buzinsky ◽  
R. Cervantes ◽  
...  
Keyword(s):  
Emission Spectroscopy ◽  
Radiation Emission ◽  
Radiated Power ◽  
Cyclotron Radiation

scholarly journals Jupiter's Radiation Belts and Upper Atmosphere

1974 ◽  
Vol 65 ◽  
pp. 375-383
Author(s):  
Joseph J. Degioanni ◽  
John R. Dickel
Keyword(s):  
Radio Emission ◽  
Radiation Belts ◽  
Upper Atmosphere ◽  
Mixing Ratio ◽  
Frequency Range ◽  
Emission Data ◽  
High Energies ◽  
Isotropic Distribution ◽  
Relativistic Particles ◽  
Flat Distribution

Models of Jupiter's radiation belts have been constructed to determine the distribution of particles and their energies which will produce the observed decimetric radio emission. Data on the spectrum and the variation of emission with Jovian longitude have been used to show that the relativistic particles have a nearly isotropic distribution with high energies (of order 100 MeV) within 2 Jovian radii and a very flat distribution in the equatorial plane of low energy particles further out in the magnetosphere.Subtraction of the emission predicted by this model from the total radio emission shows that the thermal contribution in the frequency range between 3000 and 10000 MHz is somewhat less than had been previously expected. (The brightness temperature of the planetary disk is 180 K at 3000 MHz, for example.) This suggests that the ammonia mixing ratio in Jupiter's upper atmosphere may be as high as 0.002.

SIMULATION OF RADIO SIGNALS FROM 1-10 TeV AIR SHOWERS USING EGSNRC

2006 ◽  
Vol 21 (supp01) ◽  
pp. 65-69 ◽  
Author(s):  
R. Engel ◽  
N. N. Kalmykov ◽  
A. A. Konstantinov
Keyword(s):  
Monte Carlo ◽  
Radio Emission ◽  
Monte Carlo Simulations ◽  
Frequency Spectrum ◽  
Radial Dependence ◽  
Frequency Range ◽  
Air Showers ◽  
Shower Development ◽  
Radio Signals ◽  
The Individual

Cherenkov and geosynchrotron radiation are considered as two fundamental mechanisms of the radio emission generated by extensive air showers (EAS). The code EGSnrc is used for Monte-Carlo simulations of the individual shower development. Calculations of the radial dependence and frequency spectrum of the emitted radiation are performed for the LOPES experiment frequency range.

The Pitch Angles of Electrons in Jupiter’s Radiation Belt

1976 ◽  
Vol 3 (1) ◽  
pp. 53-55 ◽  
Author(s):  
J. A. Roberts
Keyword(s):  
Radio Emission ◽  
Pitch Angle ◽  
Radiation Belt ◽  
Synchrotron Emission ◽  
Angle Distribution ◽  
Space Probe ◽  
Frequency Range ◽  
Pitch Angle Distribution ◽  
5 Ghz ◽  
Apparent Conflict

The radio emission from Jupiter in the frequency range from ∽ 50 MHz to ∽ 5 GHz is mainly synchrotron emission from electrons in the intense radiation belt which surrounds Jupiter out to several planetary radii. Information about the pitch angles of these electrons can be derived both from the radio observations and from the Pioneer space probe observations. In this communication we discuss the pitch angle distribution inferred from the radio data and the apparent conflict with the Pioneer data.

scholarly journals Zebra pattern in decametric radio emission of Jupiter

2018 ◽  
Vol 610 ◽  
pp. A69 ◽  
Author(s):  
M. Panchenko ◽  
S. Rošker ◽  
H. O. Rucker ◽  
A. Brazhenko ◽  
P. Zarka ◽  
...  
Keyword(s):  
Radio Emission ◽  
Radio Telescope ◽  
Narrow Band ◽  
Central Meridian ◽  
Frequency Interval ◽  
Frequency Range ◽  
Systematic Analysis ◽  
Zebra Pattern ◽  
Left Handed ◽  
New Type

We report the systematic analysis of zebra-like fine spectral structures in decametric frequency range of Jovian radio emission. Observations were performed by the large ground-based radio telescope URAN-2 during three observation campaigns between, Sep., 2012, and May, 2015. In total, 51 zebra pattern (ZP) events were detected. These rare fine radio features are observed in frequency range from 12.5 to 29.7 MHz as quasi-harmonically related bands of enhanced brightness. ZPs are strongly polarized radio emission with a duration from 20 s to 290 s and flux densities ~105−106 Jy (normalized to 1 AU), that is, 1–2 orders lower than for Io-decametric radio emission (DAM). Occurrence of the events does not depend on the position of Io satellite but is strongly controlled by the Jovian central meridian longitude (CML). ZPs are mainly detected in two active sectors of Jovian CMLs: 100∘ to 160∘ for Northern sources (right-handed polarized) and 300∘ and 60∘ (via 360∘) for the Southern sources (left-handed). The frequency interval between neighboring stripes is from 0.26 to 1.5 MHz and in most cases this interval increases with frequency. We discussed the double plasma resonance with electrons or ions as a possible source of the ZPs. The performed analysis of the observations allows us to conclude that the observed ZPs are a new type of narrow band spectral structures in the Jovian DAM.

Site evaluation and RFI spectrum measurements in Portugal at the frequency range 0.408–10GHz for a GEM polarized galactic radio emission experiment

New Astronomy ◽  
2006 ◽  
Vol 11 (8) ◽  
pp. 551-556 ◽  
Author(s):  
Rui Fonseca ◽  
Domingos Barbosa ◽  
Luis Cupido ◽  
Ana Mourão ◽  
Dinis M. dos Santos ◽  
...  
Keyword(s):  
Radio Emission ◽  
Frequency Range ◽  
Spectrum Measurements ◽  
Site Evaluation ◽  
Galactic Radio Emission ◽  
Galactic Radio

A Discussion on the physics of the solar atmosphere - Solar radio observations and interpretations

1976 ◽  
Vol 281 (1304) ◽  
pp. 461-471 ◽  
Keyword(s):  
Radio Emission ◽  
Boundary Conditions ◽  
Solar Atmosphere ◽  
Solar Radio ◽  
Plasma Frequency ◽  
Plasma Turbulence ◽  
Radio Bursts ◽  
Frequency Range ◽  
Radio Observations ◽  
Radio Data

The recent solar radio observations related to flares are reviewed for the frequency range of a few kilohertz to several gigahertz. The analysis of the radio data leads to boundary conditions on the acceleration processes which are responsible for the fast particles which cause the radio emission. The role and cause of plasma turbulence at the plasma-frequency and at much lower frequencies is discussed in relation to the acceleration processes and the radio emission mechanisms for the various radio bursts.

scholarly journals FEATURES OF EXCITATION AND AZIMUTHAL AND MERIDIONAL PROPAGATION OF LONG-PERIOD Pi3 OSCILLATIONS OF THE GEOMAGNETIC FIELD ON DECEMBER 8, 2017

2020 ◽  
Vol 6 (3) ◽  
pp. 56-72
Author(s):  
Aleksey Moiseev ◽  
Sergei Starodubtsev ◽  
Vladimir Mishin
Keyword(s):  
Geomagnetic Field ◽  
Large Scale ◽  
Current System ◽  
Dynamic Pressure ◽  
Small Scale ◽  
Frequency Range ◽  
Latitude Range ◽  
Magnetospheric Convection ◽  
Long Period ◽  
Geomagnetic Observations

We study the Pi3 pulsations (with a period T=15–30 min) that were recorded on December 8, 2017 at ground stations in the midnight sector of the magnetosphere at the latitude range of DP2 current system convective electrojets. We have found that Pi3 are especially pronounced in the pre-midnight sector with amplitude of up to 300 nT and duration of up to 2.5 hrs. The pulsation amplitude rapidly decreased with decreasing latitude from F′=72° to F′=63°. The event was recorded during the steady magnetospheric convection. In the southward Bz component of the interplanetary magnetic field, irregular oscillations were detected in the Pi3 frequency range. They correspond to slow magnetosonic waves occurring without noticeable variations in the dynamic pressure Pd. Ground-based geomagnetic observations have shown azimuthal propagation of pulsations with a 0.6–10.6 km/s velocity east and west of the midnight meridian. An analysis of the dynamics of pulsations along the meridian has revealed their propagation to the equator at a velocity 0.75–7.87 km/s. In the projection onto the magnetosphere, the velocities are close in magnitude to the observed propagation velocities of substorm injected electrons. In the dawn-side magnetosphere during ground-observed Pi3 pulsations, compression mode oscillations were recorded. We conclude that propagation of geomagnetic field oscillations in this event depends on the dynamics of particle injections under the action of a large-scale electric field of magnetospheric convection, which causes the plasma to move to Earth due to reconnection in the magnetotail. Small-scale oscillations in the magnetosphere were secondary, excited by the solar wind oscillations penetrating into the magnetosphere.

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