| The surface temperature of the sun is as high as6000K. This temperature couldcause ionization of almost all its surface substances. Ionized particle flow can bereleased outward to form solar wind as a result of radiation effects of fixed stars. This isone reason the entire interplanetary space is filled with solar wind, which hassignificant effects on earth. The solar wind could be considered as a bond between theearth and the solar space. Through this bond, solar energy, electromagnetic radiation,and corona effects from the sun are received by the earth. Thus, various studies on solarwind are considered significant to research on modern physical space. Most of thephysical phenomena associated with the sun and earth are closely related to solar wind.Given its physical significance, research on solar wind also has remarkable applicationvalue.In the research process for this thesis, observation features of solar wind wereanalyzed. Analyzed data were collected from satellites such as Helios, Ulysses,Advanced Composition Explorer (ACE), and wind. These were all primarily adopted,wherein the orbit of Helios was mainly from0.3AU to1AU, and the orbit of Ulysseswas mainly from1AU to5AU. The orbit of Ulysses is the distant orbit from the solarpole. Thus, field observation data for the solar wind adopted in this thesis wereextensive and feasible for comprehensive research. The observation satellites provideda variety of data, which involved number density, velocity, and temperature of particles,and even the velocity distribution function of certain categories of particles. All of thedata were acceptable with respect to research, which featured the solar wind and itsmotion characteristics by means of decomposing various micro-kinetic features of thecorona and various types of particles. These features of the solar wind includefractional anisotropies and velocity distribution function. Understanding anddifferentiating the kind of mechanism is necessary with regard to the most criticalfunction of the corona heating and acceleration of the solar wind.Based on the analyses of the observed features of the solar wind, research analyses were also conducted on corona heating and acceleration model of the solar wind.Comparative studies were performed between theoretical speculations and authenticobservation data of the solar wind velocity. Starting from the formation of corona wasnecessary when conducting research on the solar wind. The research typically startsfrom the bottom part of the corona where large quantities of observation results areavailable concerning the quality, velocity, energy, and magnetic field of the solar wind.These results make the observation basis accessible when explaining the physicalmechanisms of both corona heating and acceleration process of high-velocity solarwind. Likewise, a number of constraining conditions were generated during theestablishment of a theoretical model. Thus, to determine the constraining conditions forthis thesis, conditions that have been recognized by most researchers were used asreferences in the numerical simulation process. Considering that the solar wind couldbe formed while the corona plasma expands outward within a relatively short distance,based on previous research, most scholars considered the acceleration of solar wind andthat of the corona as identical issues to be investigated.Furthermore, based on the theoretical analyses of solar wind, studies on its plasmawere conducted. Comprehensive analyses and numerical simulations concerningmotion mechanism as well as motion structures of solar wind were conducted.According to the current available observation data, the interplanetary space was filledwith plasma in motion. This plasma was mostly formed from the radiation of fixed stars.Based on studies on the status of the plasma, the most critical part that should beunderstood is that the plasma contains a sufficient amount of charged particles. Also,since the surface of the sun is filled with electromagnetic fields, its motions would beaffected. Therefore, when research is conducted on its kinetic motion mechanism, theelectromagnetic force imposed on it should also be analyzed. Visible differences indynamic force have been observed between the plasma and the other substances ingaseous, liquid, and solid states. The plasma has its own unique law of motion becauseit is composed of electrons and ions. The substance of the three other states were mostlycomposed of neutral molecules or atoms, which also explains why plasma is consideredas the fourth state of matter and why separate analyses of its unique stress phenomenaare necessary in conducting studies of its law of motion.Finally, surface activities and disturbances of the sun have been studied so thatexisting research results could be verified. Since most scientific researchers argue forthe existence of Alfven wave transmitted outwardly from the sun within the interstellar medium, when establishing a model for this thesis, we assume that the Alfven waveexists within the transition area of the solar wind. The primary physical parameterssuch as density, velocity, temperature, and coordinates of the solar wind plasma areconsidered. Because of the existence of such physical parameters, numerous non-linearmutual functions among them were also generated, causing energy transmission amongthem and conversion of such energy into proton thermal energy. Based on theseparameters, numerical simulations were conducted for the model, and preliminarycalculations and discussions were conducted through calculation methods with finiteelements. This study has the following accomplishments:1. Observation data were collected and results from the satellites such as Helios,Ulysses, ACE, and WIND were adopted, and based on them, data analyses wereperformed on sunspot and corona activities by means of theoretical analyses, dataanalyses, and numerical simulations.2. Based on the theoretical study on corona heating and solar wind acceleration, atheoretical study on the model of solar wind acceleration was conducted. Also,simulation and analyses of radial velocity and tangential speed via theoreticalspeculation were also conducted.3. The motion mechanism of solar wind plasma was studied extensively. Analyseswere conducted in terms of hydromagnetic equations and similar parameters basedon the numerical simulation of the plasma rotation. A discontinuous motionmechanism was also employed.4. Studies and analyses were conducted on the existing mechanisms of solar windacceleration and heating, based on which kind of mechanism between non-linearacceleration and heating of solar wind was proposed. Numerical simulation wasperformed concerning this mechanism, and the corresponding merits and defects ofsuch mechanism were summarized.5. The establishment of a non-linear heat accelerates the solar wind model. Themain use of the solar wind plasma density, velocity, temperature and other physicalcoordinates to model. Established a correlation equations and the equations as amixed type equations. Research and analysis shows that solar wind plasma showschanges in the energy transfer process model can be better. |
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