A beam/plasma interaction in the high-altitude auroral ionosphere

Ambient thermal electrons are found to be heated to temperatures as high as 10⁵ K by the passage of a field-aligned beam of suprathermal electrons through the ionosphere at altitudes over 660 km. These secondary electrons will increase the proportion of 630 nm emission, caused by the primary electron precipitation, and change the secondary electron spectrum observed at lower altitudes from that expected on the basis of atmospheric collisions alone.     

Auroral arc classification scheme based on the observed arc-associated electric field pattern

Radar and rocket electric field observations of auroral arcs have earlier been used to identify essentially four different arc types, namely anticorrelation and correlation arcs (with, respectively, decreased and increased arc-associated field) and asymmetric and reversal arcs. In this paper, rocket double probe and supplementary observations from the literature, obtained under various geophysical conditions, are used to organize the different arc types on a physical rather than morphological basis. This classification is based on the relative influence on the electric field pattern from the two current continuity mechanisms, polarization electric fields and Birkeland currents. In this context the tangential electric field plays an essential role and it is thus important that it can be obtained with both high accuracy and resolution. In situ observations by sounding rockets are shown to be better suited for this specific task than monostatic radar observations. Depending on the dominating mechanism, estimated quantitatively for a number of arc-crossings, the different arc types have been grouped into the following main categories: Polarization arcs, Birkeland current arcs and Combination arcs. Finally the high altitude potential distributions corresponding to some of the different arc types are presented.     

Initial interpretation of Titan plasma interaction as observed by the Cassini plasma spectrometer: Comparisons with Voyager 1

The Cassini plasma spectrometer (CAPS) instrument made measurements of Titan's plasma environment when the Cassini Orbiter flew through the moon's plasma wake October 26, 2004 (flyby TA). Initial CAPS ion and electron measurements from this encounter will be compared with measurements made by the Voyager 1 plasma science instrument (PLS). The comparisons will be used to evaluate previous interpretations and predictions of the Titan plasma environment that have been made using PLS measurements. The plasma wake trajectories of flyby TA and Voyager 1 are similar because they occurred when Titan was near Saturn's local noon. These similarities make possible direct, meaningful comparisons between the various plasma wake measurements. They lead to the following: (A) The light and heavy ions, H⁺and N⁺/O⁺, were observed by PLS in Saturn's magnetosphere in the vicinity of Titan while the higher mass resolution of CAPS yielded H⁺ and H₂⁺as the light constituents and O⁺/CH₄⁺ as the heavy ions. (B) Finite gyroradius effects were apparent in PLS and CAPS measurements of ambient O⁺ ions as a result of their absorption by Titan's extended atmosphere. (C) The principal pickup ions inferred from both PLS and CAPS measurements are H⁺, H₂⁺, N⁺, CH₄⁺ and N₂⁺. (D) The inference that heavy pickup ions, observed by PLS, were in narrow beam distributions was empirically established by the CAPS measurements. (E) Slowing down of the ambient plasma due to pickup ion mass loading was observed by both instruments on the anti-Saturn side of Titan. (F) Strong mass loading just outside the ionotail by a heavy ion such as N₂⁺ is apparent in PLS and CAPS measurements. (G) Except for the expected differences due to the differing trajectories, the magnitudes and structures of the electron densities and temperatures observed by both instruments are similar. The high-energy electron bite-out observed by PLS in the magnetotail is consistent with that observed by CAPS.     

Auroral E-region: Ion composition and nitric oxide

Data from eight auroral ion composition measurements, seven of which have been reported in the literature, are analyzed and compared in terms of a single model format. We find, contrary to conclusions published previously for two of the experiments, that there is no discrepancy concerning O⁺ ions. In general, the mean CIRA 1972 neutral model is found to be quite suitable as a representative of the major gas composition required for auroral E-region calculations which agree with the data. Nitric oxide profiles inferred from analysis of the data range from about normal non-auroral E-region nitrix oxide distributions with peak concentrations near 10⁸ cm^?3 to profiles with peak populations near 10⁹ cm^?3. Although the higher concentrations are generally correlated with intense aurora, we acknowledge that the length and strength of auroral activity prior to the individual rocket flights can have an even greater bearing, at times, on the NO “snapshot” profile deduced from the auroral ion composition data.     

High temperature plasma inβ Lyrae,observed fromCopernicus

High-resolution ultraviolet spectrophotometry of the complex close binary systemβ Lyrae was performed with the Princeton Telescope Spectrometer onCopernicus. Observations were made at phases 0.0, 0.25, 0.5, and 0.75 with the resolution of 0.2 Å (far-ultraviolet) and 0.4 Å (mid-ultraviolet). The far-ultraviolet spectrum is completely dominated by emission lines indicating existence of high temperature plasma in this binary. The spectrum ofthis object is unlike any other object observed fromCopernicus. It is believed that this high temperature plasma results from dynamic mass transfer taking place in this binary. The current results are compared with the OAO-2 Wisconsin Experiment Package observations and other observational results. The possibility that the secondary component is a collapsed object is also discussed; theCopernicus observations are consistent with the hypothesis that the spectroscopically invisible secondary component is a black hole.     

Equatorial ionospheric plasma density bubbles observed by ESRO-4

It is shown that the ESRO-4 satellite, in a polar orbit, was able to observe equatorial plasma bubbles using the fixed-bias total ion current probe. Experimental conditions were suitable for observations during a period at the vernal equinox 1973, when 21 plasma density depletion events were identified, extending across the equator. Statistical analysis suggests that the bubble cross-sections, transformed on to the zero-dip surface, were elongated, with an axial ratio of the order of 7:1, and were tilted upwards by about 10° to the east. The observations were made selectively near the F-layer peak; no movement of bubbles was measured.     

Nonlinear interaction of plasma waves in a cold magnetized plasma

The general coupling equation for the wave-wave scattering in a cold magnetized plasma is derived. Specifically, the transformation of electrostatic waves is studied in connection with solar type-III radiation. The relevant numerical analysis is also presented.     

Low-frequency plasma turbulence during solar wind-comet interaction

The pick up cometary ion distributions are shown to excite Alfvénic mode instabilities, slow ion-acoustic mode instability and a lower hybrid instability during solar wind-comet interaction. The growth rates of all these instabilities become larger as the comet is approached. The lower hybrid instability is shown to account for the low-frequency 0–300 Hz electrostatic turbulence observed near comet Halley. The Alfvén modes can grow to large amplitudes and become modulationally unstable, in the presence of low-frequency density fluctuations, going over to envelope Alfvén solitons. A model consisting of a gas of Alfvén solitons is suggested to explain the hydromagnetic turbulence observed near comet Halley and comet Giacobini-Zinner.     

Variable,optically thick,hot plasma observed in interacting binaries

We report recent International Ultraviolet Explorer (IUE) observations of two interacting binaries, R Arae and HD 207739. The ultraviolet spectra indicate the presence of optically-thick, variable hot plasma in those binary systems. These two binaries may belong to a class of binaries that are currently undergoing a rarely observed and probably short-lived phase in their evolution. Their properties are compared with those of two other interacting binaries, U Cephei and Lyrae.Paper presented at the Lembang-Bamberg IAU Colloquium No. 80 on Double Stars: Physical Properties and Generic Relations, held at Bandung, Indonesia, 3–7 June, 1983.     

Laboratory studies for beam plasma discharge experiments with rockets

Laboratory results of beam plasma discharge (BPD) (dimensions several metres) in a homogeneous atmosphere and a jet of neutral gas are presented. The beam was obtained by an electron gun of the same type as used in rocket experiments.The BPD parameters glow intensity, electromagnetic field and its spectrum, electron density as well as the flux of scattered electrons were measured. In addition, photographs of the BPD were taken. The threshold of BPD ignition was determined as a function of gas pressure and beam parameters. The initial stage of BPD formation as well as various types of oscillatory processes in the discharge were studied. A possible process of BPD initiation is presented.     

Instability of a thin field-aligned electron beam in a plasma

The formulation of Elliott (1975) is recapitulated somewhat more elegantly for a monenergetic beam of “Top Hat” profile. The mode corresponding most closely to the parallel-polarized mode in a uniform beam is explored for phase velocities less than the beam velocity and frequencies between the hybrid frequencies. The mere existence of solutions indicates the possibility of instability in some real case. Solutions are found for all frequencies except for a range above the gyrofrequency, beyond which a ducted solution exists up to the plasma frequency. In the other range radiative solutions exist.The nature of the results provides a guide for several applications, but more realistic models must be specific to the application.     

The interaction of cosmic rays and magnetized plasma

A large flux of cosmic rays streaming through a magnetized plasma creates cavities of low plasma density and low magnetic field. The magnetic field focuses the cosmic ray trajectories into the cavities with the possible formation of filaments or beams of high-energy cosmic rays.     

Supersonic plasma jet interaction with gases and plasmas

The interaction of supersonic plasma jets with dense gases and plasmas has been studied experimentally and theoretically. Collimated plasma jets were generated from the laser pulse interaction with solid targets. The jet propagates with the velocity exceeding 400 km/s and transports the energy of a few kJ/cm². The interaction of such a jet with an Ar and He gases at various pressures has been studied by using optical and X-ray diagnostics. Qualitative estimates and numerical simulations with a radiative hydrodynamic code explain a sequence of physical processes during the interaction. Experimental and numerical results show that, by changing ambient material, the working surface structure changes from an adiabatic outflow to a radiative cooling jet. The applications of this phenomenon to astrophysical conditions and the inertial confinement fusion are discussed.     

Erupting Magnetic Structures observed with SOHO/LASCO

We report observations, from March 1999 to December 1999, of slow-moving, low-mass (10¹⁴ g) erupting structures. The 20 events seen in this period appear with a double or multiple loop structure. Their speeds range from approximately 10 to 60 km s^–1. There are no significant associated flares or radio signatures. Although the speed distribution of these events overlaps that of coronal mass ejections (CMEs), we propose that they are morphologically different structures and are not merely a continuation of the lower range of the CME speed distribution. The aim of this paper is to characterize these events and to emphasize the insight into general CME research that such simple phenomena could give.     

Recurrent coronal jets observed by SDO/AIA

In this paper,we carried out multiwavelength observations of three recurring jets on 2014 November 7.The jets originated from the same region at the edge of AR ...     

Nonsteady interaction of plasma with bodies moving in space

Nonsteady interactions between spacecraft and plasma are investigated in detail. The system of equations describing these interactions is obtained. It is shown that an electromagnetic soliton is excited via the modulational instabilities, which result from the radiation of antenna systems on the body which are the source of waves. In the meantime the density in far wake diminishes, and its disturbance becomes also a soliton if the pump wave is sufficiently intense.     

Gyrosynchrotron instability in a plasma with a beam of moderately relativistic electrons

The possibility of gyrosynchrotron instability development in a plasma with moderately relativistic electrons is revealed. The absorption and emission coefficients are numerically calculated for a Gaussian distribution function of these electrons. It shows the presence of emission bands where the absorption coefficientµ is negative, and their dependence on the halfwidth,v, of the Gaussian as well as on the observation angle is established. In conclusion, results obtained are applied for the interpretation of microwave bursts registered during solar flares.     

The propagation of a dense quasi-neutral ion beam across a magnetized plasma

Propagation of a quasi-neutral narrow ion beam across a magnetised cold plasma is investigated in slab geometry. This problem is of interest in connection with artificial beam injection experiments and with naturally appearing plasma injections into magnetic fields as astrophysical jets. Several different cases are discussed briefly where the beam is assumed either slow or fast. For fast beams it is shown that they propagate due to generation of a polarisation electric field even in the case of presence of a background plasma. Slow beams can depolarise by currents flowing into the beam along the field lines and providing the required electrons for charge neutralisation. Some implications of the model are discussed in the context of recent active beam injection experiments into space plasma.     

Alfvén wave plasma turbulence during solar wind-comet interaction

The large differences in drift velocities between the solar wind protons and the picked-up ions of cometary origin cause the Alfvén waves (among others) to become unstable and generate turbulence. A self-consistent treatment of such instabilities has to take into account that these cometary ions affect the solar wind plasma in a decisive way. With the help of a previously developed formalism one finds the correct Alfvén instability criterion, which is here nondispersive, in contrast to recent calculations where the cometary ions are treated as a low-density, high-speed, and non-neutral beam through an otherwise undisturbed solar wind. The true bulk speed of the combined solar wind plus cometary ion plasma clearly shows the mass-loading and deceleration of the solar wind near the cometary nucleus, indicating a bow shock. The instability criterion is also used to determine the region upstream where the Alfvén waves can be unstable, based upon recent observations near comet Halley.