Control of plasma waves associated with the space shuttle by the angle between the orbiter's Velocity vector and the magnetic field

1991 ◽  
Vol 96 (A5) ◽  
pp. 7591 ◽  
Author(s):  
Iver H. Cairns ◽  
Donald A. Gurnett
Keyword(s):  
Magnetic Field ◽  
Velocity Vector ◽  
Space Shuttle ◽  
Plasma Waves ◽  
The Magnetic Field

scholarly journals Plasma Emission Processes in a Magnetoactive Plasma

1972 ◽  
Vol 25 (4) ◽  
pp. 387 ◽  
Author(s):  
DB Melrose ◽  
WN Sy
Keyword(s):  
Magnetic Field ◽  
Second Harmonic ◽  
Magnetoactive Plasma ◽  
Plasma Waves ◽  
Weak Field ◽  
Type I ◽  
Plasma Emission ◽  
Weak Field Limit ◽  
Electron Cyclotron Waves ◽  
The Magnetic Field

Plasma emission (i.e. emission at about the plasma frequency and twice this frequency) is treated taking into account the effects of the magnetic field on the electron plasma waves, on the conversion processes, and on the escaping radiation. The expected degrees of polarization of the fundamental and second harmonic are calculated in the weak field limit. The results are used to estimate the magnetic field strength B at the 80 MHz level from the observed polarization of type III bursts; the result B < 0�04 G is smaller than previous estimates. The possible importance of electron-cyclotron waves in an application to type I bursts is noted.

scholarly journals Polar and Cluster observations of a dayside inverted-V during conjunction

2007 ◽  
Vol 25 (2) ◽  
pp. 543-555 ◽  
Author(s):  
J. D. Menietti ◽  
R. A. Frahm ◽  
A. Korth ◽  
F. S. Mozer ◽  
Y. Khotyaintsev
Keyword(s):  
Magnetic Field ◽  
Boundary Layer ◽  
Electric Field ◽  
Electric Fields ◽  
Magnetic Field Line ◽  
Large Amplitude ◽  
Field Data ◽  
Plasma Waves ◽  
Magnetic Field Data ◽  
The Magnetic Field

Abstract. We investigate particle and fields data during a conjunction of the Polar and Cluster spacecraft. This conjunction occurs near the dayside cusp boundary layer when a dayside inverted-V was observed in the particle data of both satellites. Electron, ion, electric field, and magnetic field data from each satellite confirm that the dayside inverted-V (DSIV) structure is present at the location of both satellites and the electric fields persist from the altitude of the Polar (lower) spacecraft to the altitude of the Cluster spacecraft. We observe accelerated, precipitating electrons and upward ions along the magnetic field. In addition, large amplitude electric fields perpendicular to the ambient magnetic field seen by Polar and by Cluster suggest significant parallel electric fields associated with these events. For similar DSIV events observed by the Polar spacecraft, plasma waves (identified as possible Alfvén waves) have been observed to propagate in both directions along the magnetic field line. Future conjunctions will be necessary to confirm that DSIVs are associated with reconnection sites.

scholarly journals On the Nature of Radio Eclipsing

2000 ◽  
Vol 177 ◽  
pp. 533-534
Author(s):  
Ya. N. Istomin
Keyword(s):  
Magnetic Field ◽  
Electromagnetic Wave ◽  
Electric Current ◽  
Plasma Waves ◽  
Bow Shock ◽  
Companion Star ◽  
Atmosphere Density ◽  
Pulsar Wind ◽  
Transverse Electromagnetic ◽  
The Magnetic Field

AbstractIt is shown that the phenomena of radio eclipsing can be explained by the linear mechanism of transformation of the transverse electromagnetic wave, propagating in the pulsar wind, into the plasma waves in the region of interaction of wind with a companion star atmosphere. The coefficient of the passingηdepends on the wave frequencyωby the exponential mannerη= exp{–const ·ω−1}. The estimated scale for the pulsar wind and star’s atmosphere density gradients are of the order of 100 meters. Such gradient can be obtained in the bow shock forming when the pulsar wind enters into the companion star atmosphere. Annihilation of the part of the wind’s positrons with the star’s electrons produces the electric current. This current generates the magnetic field from which the pulsar wind’s particles are reflected. The magnitude of the magnetic field in this shock of about several Gauss.

scholarly journals Source location of chorus emissions observed by Cluster

2003 ◽  
Vol 21 (2) ◽  
pp. 473-480 ◽  
Author(s):  
M. Parrot ◽  
O. Santolík ◽  
N. Cornilleau-Wehrlin ◽  
M. Maksimovic ◽  
C. C. Harvey
Keyword(s):  
Magnetic Field ◽  
Electromagnetic Waves ◽  
Plasma Waves ◽  
Magnetic Activity ◽  
Spectral Matrix ◽  
Chorus Waves ◽  
Storms And Substorms ◽  
Wave Normal ◽  
The Magnetic Field ◽  
Different Levels

Abstract. One of the objectives of the Cluster mission is to study sources of various electromagnetic waves using the four satellites. This paper describes the methods we have applied to data recorded from the STAFF spectrum analyser. This instrument provides the cross spectral matrix of three magnetic and two electric field components. This spectral matrix is analysed to determine, for each satellite, the direction of the wave normal relative to the Earth’s magnetic field as a function of frequency and of time. Due to the Cluster orbit, chorus emissions are often observed close to perigee, and the data analysis determines the direction of these waves. Three events observed during different levels of magnetic activity are reported. It is shown that the component of the Poynting vector parallel to the magnetic field changes its sense when the satellites cross the magnetic equator, which indicates that the chorus waves propagate away from the equator. Detailed analysis indicates that the source is located in close vicinity of the plane of the geomagnetic equator. Key words. Magnetospheric physics (plasma waves and instabilities; storms and substorms); Space plasma physics (waves and instabilities)

Damping of Large-Amplitude Plasma Waves Propagating Perpendicular to the Magnetic Field

1983 ◽  
Vol 50 (19) ◽  
pp. 1455-1458 ◽  
Author(s):  
J. M. Dawson ◽  
V. K. Decyk ◽  
Robert W. Huff ◽  
I. Jechart ◽  
T. Katsouleas ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Large Amplitude ◽  
Plasma Waves ◽  
The Magnetic Field

scholarly journals First observations of the Search Coil Magnetometer on Solar Orbiter / RPW: results and performances

2020 ◽  
Author(s):  
Matthieu Kretschmar ◽  
Volodya Krasnoselskikh ◽  
Jean-Yves Brochot ◽  
Guillaume Jannet ◽  
Thierry Dudok de Wit ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Plasma Waves ◽  
Search Coil ◽  
The Magnetic Field

&lt;p&gt;The Search Coil Magnetometer (SCM) onboard Solar Orbiter is part of the Radio and Plasma Waves (RPW) experiment and measures the variations of the magnetic field between 10 Hz and 50 kHz on three axes and between 1 kHz and 1MHz in one axis. The SCM is located on the boom of the spacecraft and its signal is processed by the LFR, TDS, and HFR analyzers of the RPW experiment. These measurements are essential for the characterization of waves and turbulence in the solar wind. We will describe the first observations made by the instrument with an emphasis on its performances.&lt;span&gt;&amp;#160;&lt;/span&gt;&lt;/p&gt;

An examination of radio-auroral aspect sensitivity

1985 ◽  
Vol 63 (7) ◽  
pp. 1005-1012 ◽  
Author(s):  
D. R. Moorcroft
Keyword(s):  
Magnetic Field ◽  
Plasma Waves ◽  
Magnetic Field Direction ◽  
Anomalous Resistivity ◽  
Earth’S Magnetic Field ◽  
Earth's Magnetic Field ◽  
E Region ◽  
Radar Wave ◽  
The Magnetic Field ◽  
Aspect Sensitivity

An attempt has been made to account for the experimental observations of scattering at angles away from perpendicularity to the earth's magnetic field (aspect sensitivity). First, it was necessary to develop a scattering model appropriate for the plasma waves generally assumed to be responsible for the scattering, consisting of an assembly of irregularities, each one a wave with a Gaussoidal envelope. Then, effects were included for off-perpendicular propagation of plasma waves, the perturbation of the magnetic field direction owing to the presence of auroral currents, and refraction of the radar wave in the E region. Even when possible effects from anomalous resistivity are included, many of the experimental observations require scattering models consisting of irregularities that are elongated along the direction of the earth's magnetic field by only a few plasma wavelengths (in some cases no more than one or two wavelengths). This is physically unreasonable and suggests that our understanding of auroral E-region irregularities and (or) the scattering processes responsible for auroral echoes is still incomplete.

scholarly journals A Theory of Type I Solar Radio Bursts

1974 ◽  
Vol 57 ◽  
pp. 293-294 ◽  
Author(s):  
W. N.-C. Sy
Keyword(s):  
Magnetic Field ◽  
Electric Field ◽  
Electromagnetic Radiation ◽  
Plasma Waves ◽  
Electron Plasma ◽  
Source Size ◽  
Plasma Radiation ◽  
Type I ◽  
Non Linear ◽  
The Magnetic Field

(Proc. Astron. Soc. Australia). A theory is developed to account for the observed properties of type I storm bursts in terms of plasma radiation – that is, electromagnetic radiation at the electron plasma frequency resulting from the non-linear scattering of electron plasma waves on plasma ions. Now the average brightness temperature of a type I source is greater than 109 K, or even higher if, because of coronal scattering, the apparent source size is larger than the true source size. For brightness temperatures as high as 109 K the non-linear scattering must be of the induced kind in which electromagnetic radiation below the frequency of the electron plasma waves is amplified. For such radiation to be strongly circularly polarized in the o-mode, as observed in type I bursts, requires that the amplification be more effective in the o-mode than in the x-mode (Figure 1). This is found to be so for plasma waves excited by electrons travelling parallel to the magnetic field. The electric field of the plasma waves is then also parallel to the magnetic field. The non-linear scattering is more efficient for that magnetoionic mode which has the greater component of electric field in the same direction. This mode is the o-mode.

Sign in / Sign up

Export Citation Format

Share Document