Small-amplitude Langmuir pulse excited by a planar grid electrode in a flowing plasma

2015 ◽  
Vol 81 (5) ◽  
Author(s):  
John J. Podesta
Keyword(s):  
Solar Wind ◽  
Flow Velocity ◽  
Small Amplitude ◽  
Collisionless Plasma ◽  
Distribution Functions ◽  
Bulk Flow ◽  
Wire Mesh ◽  
High Time Resolution ◽  
Grid Electrode ◽  
Planar Grid

The generation and propagation of a small-amplitude Langmuir pulse excited by a planar grid electrode in a spatially uniform collisionless plasma with a constant flow velocity is studied by solving the linearized Vlasov–Poisson equations. The electrode is transparent to the flow of particles, like a screen or a wire mesh. The particles are assumed to have a Kappa velocity distribution, a reasonable approximation for electron distribution functions in the solar wind. Exact, closed-form solutions are obtained for ${\it\kappa}=1$, the Lorentzian distribution, and for ${\it\kappa}=2$. The explicit form of the solution in the case ${\it\kappa}=2$ has not, to our knowledge, appeared in the literature before. The properties of the solutions are investigated and a practical technique for measuring the bulk flow velocity in plasma experiments is proposed that may be useful for high-accuracy, high-time-resolution measurements of the bulk flow velocity in the solar wind.

Joint Estimation of Bulk Flow Velocity and Angle Using a Lateral Line Probe

2016 ◽  
Vol 65 (3) ◽  
pp. 601-613 ◽  
Author(s):  
Nataliya Strokina ◽  
Joni-Kristian Kamarainen ◽  
Jeffrey A. Tuhtan ◽  
Juan Francisco Fuentes-Perez ◽  
Maarja Kruusmaa
Keyword(s):  
Flow Velocity ◽  
Lateral Line ◽  
Joint Estimation ◽  
Bulk Flow

Intercomponent Momentum Transport and Electrical Conductivity of Collisionless Plasma

1973 ◽  
Vol 51 (24) ◽  
pp. 2604-2611 ◽  
Author(s):  
H. E. Wilhelm
Keyword(s):  
Electrical Conductivity ◽  
Electric Field ◽  
Collisionless Plasma ◽  
Electrical Current ◽  
Distribution Functions ◽  
Momentum Transport ◽  
Ion Drift ◽  
Moment Approximation ◽  
Electrons And Ions ◽  
Two Component

Based on the Lenard–Balescu equation, the interaction integral for the intercomponent momentum transfer in a two-component, collisionless plasma is evaluated in closed form. The distribution functions of the electrons and ions are represented in the form of nonisothermal, displaced Max wellians corresponding to the 5-moment approximation. As an application, the transport of electrical current in an electric field is discussed for infrasonic up to sonic electron–ion drift velocities.

Design of Interplanetary Observation Terminal based on All Programmable System-on-Chip

2021 ◽  
Author(s):  
Haonan Jin ◽  
Lesheng He ◽  
Liang Dong ◽  
Yongliang Tan ◽  
Qingyang Kong
Keyword(s):  
Solar Wind ◽  
Human Life ◽  
Average Power ◽  
Experimental Tests ◽  
System On Chip ◽  
High Time Resolution ◽  
Processing Scheme ◽  
Gigabit Ethernet ◽  
System Memory ◽  
On Chip

The drastic changes in the solar wind will cause serious harm to human life. Monitoring interplanetary scintillation (IPS) can predict solar wind activity, thereby effectively reducing the harm caused by space weather. Aiming at the problem of the lack of the ability to observe IPS phenomenon of the 40-meter radio telescope at the Yunnan Astronomical Observatory of China in the frequency band around 300MHz, an IPS real-time acquisition and processing scheme based on all programmable system-on-chip(APSoC) was proposed. The system calculates the average power of 10ms IPS signal in PL-side and transmits it to the system memory through AXI4 bus. PS-side reads the data, takes logarithms, packages it, and finally transmits it to the LabVIEW host computer through gigabit Ethernet UDP mode for display and storage. Experimental tests show that the system functions correctly, and the PL-side power consumption is only 1.955 W, with a high time resolution of 10ms, and no data is lost in 24 hours of continuous observation, with good stability. The system has certain application value in IPS observation.

Early Observations from the Solar Orbiter SWA/Electron Analyser System

2021 ◽  
Author(s):  
Christopher Owen ◽  
Keyword(s):  
Solar Wind ◽  
Field Vector ◽  
Field Of View ◽  
High Time Resolution ◽  
Angle Distribution ◽  
Pitch Angle Distribution ◽  
Burst Mode ◽  
Steering Mechanism ◽  
Operational Issues ◽  
Electrostatic Analyser

<p>Solar Orbiter carries a total of 10 instrument suites making up the payload for the mission.  One of these, the Solar Wind Analyser (SWA) instrument, is comprised of 3 sensor units which are together served by a central DPU unit.  Of particular focus in this presentation are the early measurements from one of these sensors, the Electron Analyser System (EAS).  EAS is a dual-head, top-hat electrostatic analyser system that is capable of making 3D measurements of solar wind electrons at energies below ~5 keV from a vantage point at the end of a 4-metre boom extending into the shadow of the spacecraft.  The sensor was accommodated in this location to both maximise the unobstructed field of view and to minimise the effect of spacecraft related disturbances on the low-energy (less than a few tens of eV) electrons expected the core population of the solar wind.</p><p>To date the SWA instrument sensors have operated sporadically during the mission cruise phase, which began in June 2020.  This is due to a number of operational issues faced by the SWA team, which mean we have not been able to take data in a continuous manner.  However, the data that has been taken shows the clear promise of the SWA measurements, in general, once these issues can be overcome.  For example, EAS is using a novel sample steering mechanism in burst mode which, with reference to a magnetic field vector shared onboard by the MAG instrument, allows the capture of the electron pitch angle distribution at unusually high time resolution.  We discuss these observations here, and illustrate the potential science returns from the burst mode.  We also present results from the new EAS observations in the vicinity of reconnecting current sheets in the solar wind, to more generally illustrate the capability of the sensor. </p>

Boundary Layer Flashback in Premixed Hydrogen–Air Flames With Acoustic Excitation

2017 ◽  
Vol 140 (5) ◽  
Author(s):  
Vera Hoferichter ◽  
Thomas Sattelmayer
Keyword(s):  
Boundary Layer ◽  
Flow Velocity ◽  
Gas Turbine ◽  
Gas Turbines ◽  
Excitation Amplitude ◽  
Bulk Flow ◽  
Acoustic Excitation ◽  
Worst Case ◽  
Thermoacoustic Instabilities ◽  
Flame Flashback

Lean premixed combustion is prevailing in gas turbines to minimize nitrogen oxide emissions. However, this technology bears the risk of flame flashback and thermoacoustic instabilities. Thermoacoustic instabilities induce velocity oscillations at the burner exit which, in turn, can trigger flame flashback. This article presents an experimental study at ambient conditions on the effect of longitudinal acoustic excitation on flashback in the boundary layer of a channel burner. The acoustic excitation simulates the effect of thermoacoustic instabilities. Flashback limits are determined for different excitation frequencies characterizing intermediate frequency dynamics in typical gas turbine combustors (100–350 Hz). The excitation amplitude is varied from 0% to 36% of the burner bulk flow velocity. For increasing excitation amplitude, the risk of flame flashback increases. This effect is strongest at low frequencies. For increasing excitation frequency, the influence of the velocity oscillations decreases as the flame has less time to follow the changes in bulk flow velocity. Two different flashback regimes can be distinguished based on excitation amplitude. For low excitation amplitudes, flashback conditions are reached if the minimum flow velocity in the excitation cycle falls below the flashback limit of unexcited unconfined flames. For higher excitation amplitudes, where the flame starts to periodically enter the burner duct, flashback is initiated if the maximum flow velocity in the excitation cycle is lower than the flashback limit of confined flames. Consequently, flashback limits of confined flames should also be considered in the design of gas turbine burners as a worst case scenario.

Tsallis Distribution Functions in the Solar Wind: Magnetic Field and Velocity Observations

2007 ◽  
Author(s):  
Leonard F. Burlaga ◽  
Adolfo F. Viñas ◽  
Sumiyoshi Abe ◽  
Hans Herrmann ◽  
Piero Quarati ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Distribution Functions ◽  
Solar Wind Magnetic Field ◽  
Tsallis Distribution

scholarly journals Ion-driven Instabilities in the Inner Heliosphere. I. Statistical Trends

2021 ◽  
Vol 923 (1) ◽  
pp. 116
Author(s):  
Mihailo M. Martinović ◽  
Kristopher G. Klein ◽  
Tereza Ďurovcová ◽  
Benjamin L. Alterman
Keyword(s):  
Solar Wind ◽  
Particle Interaction ◽  
Radial Distance ◽  
Solar Wind Plasma ◽  
Distribution Functions ◽  
Nyquist Criterion ◽  
Velocity Distribution Functions ◽  
Instability Growth ◽  
Statistical Trends ◽  
The Impact

Abstract Instabilities described by linear theory characterize an important form of wave–particle interaction in the solar wind. We diagnose unstable behavior of solar wind plasma between 0.3 and 1 au via the Nyquist criterion, applying it to fits of ∼1.5M proton and α particle Velocity Distribution Functions (VDFs) observed by Helios I and II. The variation of the fraction of unstable intervals with radial distance from the Sun is linear, signaling a gradual decline in the activity of unstable modes. When calculated as functions of the solar wind velocity and Coulomb number, we obtain more extreme, exponential trends in the regions where collisions appear to have a notable influence on the VDF. Instability growth rates demonstrate similar behavior, and significantly decrease with Coulomb number. We find that for a nonnegligible fraction of observations, the proton beam or secondary component might not be detected, due to instrument resolution limitations, and demonstrate that the impact of this issue does not affect the main conclusions of this work.

Analysis of Alfvénic flows with Solar Orbiter: particle and magnetic observations down to kinetic scales.

2021 ◽  
Author(s):  
Philippe Louarn ◽  
Andrei fedorov ◽  
alexis Rouillard ◽  
Benoit Lavraud ◽  
Vincent Génot ◽  
...  
Keyword(s):  
Solar Wind ◽  
Fine Structure ◽  
Time Resolution ◽  
Time Scale ◽  
Residual Energy ◽  
Distribution Functions ◽  
Strongly Correlated ◽  
Temperature Anisotropy ◽  
Velocity Fluctuations ◽  
Turbulence Parameters

<p>The magnetic and velocity fluctuations of the solar wind may be strongly correlated. This characterizes the  ‘Alfvenic’ flows. Using the observations of the Proton Alfa sensor (PAS/SWA) and the magnetometer (MAG) onboard Solar Orbiter, we analyze a period of 100 hours of such alfvenic flows, at different scales. Several parameters of the turbulence are computed (V-B correlation, various spectral indexes, cross-helicity, residual energy). We explore how these parameters may vary with time and characterize different turbulent states of the flow. More specifically, using the unprecedented time resolution of PAS during burst mode, especially its capability to measure 3D distribution functions at time scale below the proton gyroperiod, we study the connection of the turbulence to the dissipation domain and analyze the fine structure of the distribution functions and their evolutions at sub-second scales. The goal is to investigate whether some characteristics of the distributions, as their more or less pronounced temperature anisotropy, may be related to the turbulence parameters and the degree of V-B correlation.</p>

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