scholarly journals Analytical Model Nonequilibrium Inhomogeneous Plasma of the Heliosphere

2021 ◽  
Author(s):  
Philipp Vysikaylo
Keyword(s):  
Solar Wind ◽  
Electric Fields ◽  
Inhomogeneous Plasma ◽  
Solar Wind Plasma ◽  
High Energy ◽  
Gas Discharge ◽  
The Sun ◽  
Energetic Electrons ◽  
Positively Charged

We prove that a nonequilibrium inhomogeneous giant gas discharge is realized in the heliosphere with huge values of the parameter <i>E</i>/<i>N</i>, which determines the temperature of electrons. This quasi-stationary discharge determines the main parameters of the weak solar wind (SW) in the heliosphere. In connection with the development of space technologies and the human spacewalk, the problem of the nature of the SW is acute. The study of the interference of gravitational and electrical potentials at the Earth's surface began with the work of Hilbert 1600. Such polarization effects – the interference of Coulomb and gravitational forces – have not been studied well enough even in the heliosphere. Our article is devoted to this problem. Pannekoek-Rosseland-Eddington model do not take into account the important role of highly energetic running (away from the Sun) electrons and, accordingly, the duality of electron fluxes. According to an alternative model formulated by we, highly energetic (escaping from the Sun) electrons leave the Sun and the heliosphere, and weakly energetic ones, unable to leave the Coulomb potential well (hole) – the positively charged Sun and the heliosphere, return to the Sun. The weak difference between the opposite currents of highly energetic (escaping from the Sun) electrons and weakly energetic (returning to the Sun) electrons is compensated by the current of positive ions and protons from the Sun – SW. These dynamic processes maintain a quasi-constant effective dynamic charge of the Sun and the entire heliosphere. At the same time, quasi-neutrality in the Sun and heliosphere is well performed up to 10<sup>-36</sup>. According to experiments and analytical calculations based on our model: 1) the plasma in the corona is nonequilibrium; 2) the maximum electron temperature is T<sub>e</sub> ~ 1-2 million degrees; 3) T<sub>e</sub> grows from 1000 km away from the Sun and 4) the role of highly energetic electrons escaping from the plasma leads to a significant increase in the effective: solar charge and electric fields in the heliosphere in relation to the Pannekoek-Rosseland-Eddington model. This is due to the absence of a compensation layer that screens the effective charge of the Sun. It is not formed at all due to the escape of highly energetic electrons (as in a conventional gas discharge) in the entire heliosphere with high temperatures exceeding the temperature of the Sun's surface. Thus, the process of escape of highly energetic electrons forms the internal EMF of the entire heliosphere. Interference of gravitational and Coulomb potentials in the entire heliosphere is considered, it is being manifested in generation of two opposite flows of particles: 1) that are neutral or with a small charge (to the Sun), and 2) in the form of high-energy electrons (escaping from the positively charged Sun) and a solar wind (from the Sun). Calculated values of the registered ion parameters in the solar wind were compared with experimental observations. Reasons for generating the ring current in inhomogeneous heliosphere and inapplicability of the Debye theory in describing processes in the solar wind (plasma with current) are considered.

scholarly journals Analytical Model Nonequilibrium Inhomogeneous Plasma of the Heliosphere

2021 ◽  
Author(s):  
Philipp Vysikaylo
Keyword(s):  
Solar Wind ◽  
Electric Fields ◽  
Inhomogeneous Plasma ◽  
Solar Wind Plasma ◽  
High Energy ◽  
Gas Discharge ◽  
The Sun ◽  
Energetic Electrons ◽  
Positively Charged

We prove that a nonequilibrium inhomogeneous giant gas discharge is realized in the heliosphere with huge values of the parameter <i>E</i>/<i>N</i>, which determines the temperature of electrons. This quasi-stationary discharge determines the main parameters of the weak solar wind (SW) in the heliosphere. In connection with the development of space technologies and the human spacewalk, the problem of the nature of the SW is acute. The study of the interference of gravitational and electrical potentials at the Earth's surface began with the work of Hilbert 1600. Such polarization effects – the interference of Coulomb and gravitational forces – have not been studied well enough even in the heliosphere. Our article is devoted to this problem. Pannekoek-Rosseland-Eddington model do not take into account the important role of highly energetic running (away from the Sun) electrons and, accordingly, the duality of electron fluxes. According to an alternative model formulated by we, highly energetic (escaping from the Sun) electrons leave the Sun and the heliosphere, and weakly energetic ones, unable to leave the Coulomb potential well (hole) – the positively charged Sun and the heliosphere, return to the Sun. The weak difference between the opposite currents of highly energetic (escaping from the Sun) electrons and weakly energetic (returning to the Sun) electrons is compensated by the current of positive ions and protons from the Sun – SW. These dynamic processes maintain a quasi-constant effective dynamic charge of the Sun and the entire heliosphere. At the same time, quasi-neutrality in the Sun and heliosphere is well performed up to 10<sup>-36</sup>. According to experiments and analytical calculations based on our model: 1) the plasma in the corona is nonequilibrium; 2) the maximum electron temperature is T<sub>e</sub> ~ 1-2 million degrees; 3) T<sub>e</sub> grows from 1000 km away from the Sun and 4) the role of highly energetic electrons escaping from the plasma leads to a significant increase in the effective: solar charge and electric fields in the heliosphere in relation to the Pannekoek-Rosseland-Eddington model. This is due to the absence of a compensation layer that screens the effective charge of the Sun. It is not formed at all due to the escape of highly energetic electrons (as in a conventional gas discharge) in the entire heliosphere with high temperatures exceeding the temperature of the Sun's surface. Thus, the process of escape of highly energetic electrons forms the internal EMF of the entire heliosphere. Interference of gravitational and Coulomb potentials in the entire heliosphere is considered, it is being manifested in generation of two opposite flows of particles: 1) that are neutral or with a small charge (to the Sun), and 2) in the form of high-energy electrons (escaping from the positively charged Sun) and a solar wind (from the Sun). Calculated values of the registered ion parameters in the solar wind were compared with experimental observations. Reasons for generating the ring current in inhomogeneous heliosphere and inapplicability of the Debye theory in describing processes in the solar wind (plasma with current) are considered.

scholarly journals A review of the SCOSTEP’s 5-year scientific program VarSITI—Variability of the Sun and Its Terrestrial Impact

2021 ◽  
Vol 8 (1) ◽  
Author(s):  
Kazuo Shiokawa ◽  
Katya Georgieva
Keyword(s):  
Solar Wind ◽  
Interplanetary Space ◽  
Solar Wind Plasma ◽  
The Sun ◽  
Scientific Program ◽  
Solar Cycles ◽  
Grand Minimum ◽  
The Earth ◽  
Earth Connection ◽  
Near Future

AbstractThe Sun is a variable active-dynamo star, emitting radiation in all wavelengths and solar-wind plasma to the interplanetary space. The Earth is immersed in this radiation and solar wind, showing various responses in geospace and atmosphere. This Sun–Earth connection variates in time scales from milli-seconds to millennia and beyond. The solar activity, which has a ~11-year periodicity, is gradually declining in recent three solar cycles, suggesting a possibility of a grand minimum in near future. VarSITI—variability of the Sun and its terrestrial impact—was the 5-year program of the scientific committee on solar-terrestrial physics (SCOSTEP) in 2014–2018, focusing on this variability of the Sun and its consequences on the Earth. This paper reviews some background of SCOSTEP and its past programs, achievements of the 5-year VarSITI program, and remaining outstanding questions after VarSITI.

scholarly journals The unexpected role of evolving longitudinal electric fields in generating energetic electrons in relativistically transparent plasmas

2018 ◽  
Vol 20 (9) ◽  
pp. 093024 ◽  
Author(s):  
L Willingale ◽  
A V Arefiev ◽  
G J Williams ◽  
H Chen ◽  
F Dollar ◽  
...  
Keyword(s):  
Electric Fields ◽  
Energetic Electrons

scholarly journals The role of aerodynamic drag in dynamics of coronal mass ejections

2008 ◽  
Vol 4 (S257) ◽  
pp. 271-277
Author(s):  
Bojan Vršnak ◽  
Dijana Vrbanec ◽  
Jaša Čalogović ◽  
Tomislav Žic
Keyword(s):  
Solar Wind ◽  
Wind Speed ◽  
Coronal Mass Ejections ◽  
Weather Forecasting ◽  
Aerodynamic Drag ◽  
Interplanetary Space ◽  
Solar Wind Speed ◽  
Standard Form ◽  
The Sun

AbstractDynamics of coronal mass ejections (CMEs) is strongly affected by the interaction of the erupting structure with the ambient magnetoplasma: eruptions that are faster than solar wind transfer the momentum and energy to the wind and generally decelerate, whereas slower ones gain the momentum and accelerate. Such a behavior can be expressed in terms of “aerodynamic” drag. We employ a large sample of CMEs to analyze the relationship between kinematics of CMEs and drag-related parameters, such as ambient solar wind speed and the CME mass. Employing coronagraphic observations it is demonstrated that massive CMEs are less affected by the aerodynamic drag than light ones. On the other hand, in situ measurements are used to inspect the role of the solar wind speed and it is shown that the Sun-Earth transit time is more closely related to the wind speed than to take-off speed of CMEs. These findings are interpreted by analyzing solutions of a simple equation of motion based on the standard form for the drag acceleration. The results show that most of the acceleration/deceleration of CMEs on their way through the interplanetary space takes place close to the Sun, where the ambient plasma density is still high. Implications for the space weather forecasting of CME arrival-times are discussed.

A Survey of Interplanetary Small Flux Ropes at Mercury

2020 ◽  
Author(s):  
Réka Winslow ◽  
Amy Murphy ◽  
Nathan Schwadron ◽  
Noé Lugaz ◽  
Wenyuan Yu ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Current Sheet ◽  
Heliocentric Distance ◽  
Free Field ◽  
Flux Rope ◽  
Solar Wind Plasma ◽  
The Sun ◽  
Superposed Epoch Analysis ◽  
Flux Ropes

&lt;p&gt;Small flux ropes (SFRs) are interplanetary magnetic flux ropes with durations from a few minutes to a few hours. We have built a comprehensive catalog of SFRs at Mercury using magnetometer data from the orbital phase of the MESSENGER mission (2011-2015). In the absence of solar wind plasma measurements, we developed strict identification criteria for SFRs in the magnetometer observations, including conducting force-free field fits for each flux rope. We identified a total of 48 events that met our strict criteria, with events ranging in duration from 2.5 minutes to 4 hours. Using superposed epoch analysis, we obtained the generic SFR magnetic field profile at Mercury. Due to the large variation in Mercury's heliocentric distance (0.31-0.47 AU), we split the data into two distance bins. We found that the average SFR profile is more symmetric &quot;farther from the Sun&quot;, in line with the idea that SFRs form closer to the Sun and undergo a relaxation process in the solar wind. Based on this result, as well as the SFR durations and the magnetic field strength fall-off with heliocentric distance, we infer that the SFRs observed at Mercury are expanding as they propagate with the solar wind. We also determined that the SFR occurrence frequency is nearly four times as high at Mercury as for similarly detected events at 1 AU. Most interestingly, we found two SFR populations in our dataset, one likely generated in a quasi-periodic formation process near the heliospheric current sheet, and the other formed away from the current sheet in isolated events.&lt;/p&gt;

Gravitational and Coulomb Potentials Interference in Heliosphere

2020 ◽  
pp. 93-121
Author(s):  
P.I. Vysikaylo ◽  
N.S. Ryabukha
Keyword(s):  
Solar Wind ◽  
Solar Wind Plasma ◽  
The Sun ◽  
Number Density ◽  
Heavy Particles ◽  
Debye Theory ◽  
Experimental Values ◽  
First Time ◽  
Small Charge ◽  
Coulomb Potentials

Interference of gravitational and Coulomb potentials in the entire heliosphere is considered, it is being manifested in generation of two opposite flows of charged particles: 1) that are neutral or with a small charge to the Sun, and 2) in the form of a solar wind from the Sun. According to the Einstein --- Smoluchowski relation Te(R) = eDe / µe ~ (E/N)0.75 based on the N experimental values (heavy particles number density --- the ne electron concentration), the Te electron temperature in the entire heliosphere was for the first time analytically calculated depending on the charge of the Sun and distance to it R. Calculated values of the registered ion parameters in the solar wind were compared with experimental observations. Reasons for generating the ring current in inhomogeneous heliosphere and inapplicability of the Debye theory in describing processes in the solar wind (plasma with current) are considered

scholarly journals Long-lasting injection of solar energetic electrons into the heliosphere

2018 ◽  
Vol 613 ◽  
pp. A21 ◽  
Author(s):  
N. Dresing ◽  
R. Gómez-Herrero ◽  
B. Heber ◽  
A. Klassen ◽  
M. Temmer ◽  
...  
Keyword(s):  
Energetic Electron ◽  
Solar Energetic Particle ◽  
High Energy ◽  
Interaction Region ◽  
Energetic Electrons ◽  
Coronal Activity ◽  
High Energy Particles ◽  
Electron Event

Context. The main sources of solar energetic particle (SEP) events are solar flares and shocks driven by coronal mass ejections (CMEs). While it is generally accepted that energetic protons can be accelerated by shocks, whether or not these shocks can also efficiently accelerate solar energetic electrons is still debated. In this study we present observations of the extremely widespread SEP event of 26 Dec 2013 To the knowledge of the authors, this is the widest longitudinal SEP distribution ever observed together with unusually long-lasting energetic electron anisotropies at all observer positions. Further striking features of the event are long-lasting SEP intensity increases, two distinct SEP components with the second component mainly consisting of high-energy particles, a complex associated coronal activity including a pronounced signature of a shock in radio type-II observations, and the interaction of two CMEs early in the event. Aims. The observations require a prolonged injection scenario not only for protons but also for electrons. We therefore analyze the data comprehensively to characterize the possible role of the shock for the electron event. Methods. Remote-sensing observations of the complex solar activity are combined with in situ measurements of the particle event. We also apply a graduated cylindrical shell (GCS) model to the coronagraph observations of the two associated CMEs to analyze their interaction. Results. We find that the shock alone is likely not responsible for this extremely wide SEP event. Therefore we propose a scenario of trapped energetic particles inside the CME–CME interaction region which undergo further acceleration due to the shock propagating through this region, stochastic acceleration, or ongoing reconnection processes inside the interaction region. The origin of the second component of the SEP event is likely caused by a sudden opening of the particle trap.

scholarly journals The RPW Low Frequency Receiver (LFR) on Solar Orbiter: in-situ LF electric and magnetic field measurements of the solar wind expansion

2020 ◽  
Author(s):  
Thomas Chust ◽  
Olivier Le Contel ◽  
Matthieu Berthomier ◽  
Alessandro Retinò ◽  
Fouad Sahraoui ◽  
...  
Keyword(s):  
Solar Wind ◽  
Low Frequency ◽  
Field Measurements ◽  
Solar Wind Plasma ◽  
Wind Condition ◽  
The Sun ◽  
Nasa Mission ◽  
Magnetic Field Measurements ◽  
Electric And Magnetic Field

&lt;p&gt;Solar Orbiter (SO) is an ESA/NASA mission for exploring the Sun-Heliosphere connection which has been launched in February 2020. The Low Frequency Receiver (LFR) is one of the main subsystems of the Radio and Plasma Wave (RPW) experiment on SO. It is designed for characterizing the low frequency (~0.1Hz&amp;#8211;10kHz) electromagnetic fields &amp; waves which develop, propagate, interact, and dissipate in the solar wind plasma. In correlation with particle observations it will help to understand the heating and acceleration processes at work during its expansion. We will present the first LFR data gathered during the Near Earth Commissioning Phase, and will compare them with MMS data recorded in similar solar wind condition.&lt;/p&gt;

scholarly journals Radio Astronomical Scintillation in the Solar Wind Plasma: Imaging Interplanetary Disturbances

2002 ◽  
Vol 199 ◽  
pp. 426-429 ◽  
Author(s):  
P.K. Manoharan ◽  
M. Pick ◽  
Lasco Consortium
Keyword(s):  
Solar Wind ◽  
Refractive Index ◽  
Random Medium ◽  
Solar Wind Plasma ◽  
Radio Sources ◽  
The Sun ◽  
Radio Waves ◽  
Paper Briefly ◽  
Plasma Imaging ◽  
Salient Features

When radio waves propagate through a irregular medium, scattering by the random refractive index inhomogeneities can lead to a wide variety of phenomena, which include intensity scintillation. The observed scattering can be interpreted to gain information about the random medium and such inversion studies are valuable when the accessibility of the medium becomes difficult. This paper briefly describes the intensity scintillation of celestial radio sources caused by the turbulence in the solar wind and summarizes the salient features of the method employed in mapping the structure of disturbances leaving the Sun out to ∼1 AU.

scholarly journals The Sun as a Stellar Laboratory: Unsolved Problems

2004 ◽  
Vol 219 ◽  
pp. 1-10
Author(s):  
John C. Brown
Keyword(s):  
Particle Acceleration ◽  
Solar Physics ◽  
High Energy ◽  
Atmospheric Plasma ◽  
Energy Budgets ◽  
The Sun ◽  
Stellar Flare ◽  
Neupert Effect ◽  
Kinetic Effects

A brief overview is given of some of the current outstanding problems in solar physics with greatest emphasis on high energy phenomena in the atmosphere. The importance of plasma kinetic effects, as well as MHD, in understanding the complex finely structured and dynamic solar atmospheric plasma is stressed. Key results from the RHESSI Mission on energetic flare particle acceleration, propagation, and flare energy budgets are presented as are recent findings concerning the solar and stellar flare Neupert effect and the possible role of energetic particles in micro-events in the ‘non-flaring’ sun. Finally, evidence showing that magnetic fields are also important in hot star phenomena is mentioned.

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