• Title/Summary/Keyword: Sun%3A corona

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NON-HYDROSTATIC SUPPORT OF PLASMA IN THE SOLAR CHROMOSPHERE AND CORONA

  • Chae, Jong-Chul
    • Journal of The Korean Astronomical Society
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    • v.43 no.3
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    • pp.55-64
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    • 2010
  • We investigate how plasma structures in the solar chromosphere and corona can extend to altitudes much above hydrostatic scale heights from the solar surface even under the force of gravity. Using a simple modified form of equation of motion in the vertical direction, we argue that there are two extreme ways of non-hydrostatic support: dynamical support and magnetic support. If the vertical acceleration is downward and its magnitude is a significant fraction of gravitational acceleration, non-hydrostatic support is dynamical in nature. Otherwise non-hydrostatic support is static, and magnetic support by horizontal magnetic fields is the only other possibility. We describe what kind of observations are needed in the clarification of the nature of non-hydrostatic support. Observations available so far seem to indicate that spicules in the quiet regions and dynamic fibrils in active regions are dynamically supported whereas the general chromosphere as well as prorninences is magnetically supported. Moreover, it appears that magnetic support is required for plasma in some coronal loops as well. We suspect that the identification of a coronal loop with a simple magnetic flux tube might be wrong in this regard.

A New Type of Nonthermal Plasma Reactor

  • Geum, Sang-Taek;Moon, Jae-Duk;Jun, Sun-Gon
    • The Korean Journal of Ceramics
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    • v.5 no.3
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    • pp.245-249
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    • 1999
  • A new type of nonthermal plasma reactor utilizing ferroelectric pellets is proposed to generate nonthermal plasma efficiently, which is used for simultaneous control of various pollutant gases. Electric charges stored on ferroelctric pellets by corona discharge between a corona tip and a mesh electrode provide partial electrical discharges among ferroelectric pellets. These partial electrical discharges can enhance partial discharges around the surface of ferroelectric pellets. This method utilizes wide reacting area of ferroelectric pellets and partial discharge. Positive and negative dc voltage are applied to the corona tip to generate partial discharges, and corona currents are estimated to investigate charge storage on ferroelectric pellets as function of time and charge relaxation time constants of ferroelectric pellects. As a result, charge relaxationtime, dielectric constants of ferroelectric pellets, polarity of applied voltage and applied time influence partial discharges among ferroelectric pellect.

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NUMERICAL CALCULATION OF TWO FLUID SOLAR WIND MODEL

  • KIM S.-J.;KIM K.-S.;MOON Y.-J.;CRO K.-S.;PARK Y. D.
    • Journal of The Korean Astronomical Society
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    • v.37 no.1
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    • pp.55-59
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    • 2004
  • We have developed a two fluid solar wind model from the Sun to 1 AU. Its basic equations are mass, momentum and energy conservations. In these equations, we include a wave mechanism of heating the corona and accelerating the wind. The two fluid model takes into account the power spectrum of Alfvenic wave fluctuation. Model computations have been made to fit observational constraints such as electron($T_e$) and proton($T_p$) temperatures and solar wind speed(V) at 1 AU. As a result, we obtained physical quantities of solar wind as follows: $T_e$ is $7.4{\times}10^5$ K and density(n) is $1.7 {\times}10^7\;cm^{-3}$ in the corona. At 1 AU $T_e$ is $2.1 {\times} 10^5$ K and n is $0.3 cm^{-3}$, and V is $511 km\;s^{-1}$. Our model well explains the heating of protons in the corona and the acceleration of the solar wind.

Improvement of Corona Temperature and Velocity Determination Method Using a Coronagraph Filter System

  • Cho, Kyuhyoun;Chae, Jongchul;Lim, Eun-Kyung
    • The Bulletin of The Korean Astronomical Society
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    • v.42 no.2
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    • pp.85.3-86
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    • 2017
  • We have developed a methodology to determine the coronal electron temperature and solar wind speed using a four filter coronagraph system. The method developed so far have been applied to total eclipse observation and have yielded plausible results. The current methodology starts from the assumption that 1) coronal free electrons are isothermal and 2) coronal free electrons have spherically symmetric distrubution. However, the actual solar corona differs significantly from the two assumptions above. The coronal electron density is not spherically symmetric due to streamers, plumes, and coronal loops, and the electron temperature is also expected to increase rapidly with distance from the sun. We will discuss how to determine the temperature and wind speed of the corona in the case of corona with thermal structures and non-spherical symmetric electron density.

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Creating Mosaic Image of the Korean Peninsula from CORONA Imagery (CORONA 영상을 이용한 한반도 지역 모자이크 영상 제작)

  • Song, Yeong-Sun
    • Journal of Korean Society for Geospatial Information Science
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    • v.13 no.4 s.34
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    • pp.67-73
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    • 2005
  • The urbanization of Korea has been rapidly progressed since 1960, but satellite imagery have provided the information only after 1975. Recently released CORONA imagery is one of the few source of satellite image which can provide 1960's topographic information of the Korean Peninsular. It can be applied to change detection in various fields such as urban, forest, and environmental planning. In this research mosaic image of past Korean Peninsular using CORONA imagery in the 1960s were generated. A polynomial equation and a modified collinearity equation were applied for geo-referencing and a comparative analysis was conducted. In this research the 2nd polynomial equations were used for geo-referencing of CORONA imagery. After carrying out geo-referencing, mosaic image was generated using Erdas Imagine. It is assumed that this result image is very useful for various fields such as generation of thematic maps, urban planning, and change detection.

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Development of UV Corona Camera for the Detecting of Discharge on Power Facility using UV Transmittance Improvement Filter (UV 투과율 향상 필터 기술을 이용한 전력설비 방전 검출용 자외선 코로나 카메라 개발)

  • Kim, Young-Seok;Choi, Myeong-Il;Kim, Chong-Min;Bang, Sun-Bae;Shong, Kil-Mok
    • The Transactions of The Korean Institute of Electrical Engineers
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    • v.61 no.11
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    • pp.1656-1661
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    • 2012
  • UV inspection technology is being used for predictive maintenance of power facility together with IR-thermography and ultrasonic devices. In this paper, the UV corona camera design, fabrication, and perform a simple test to be take advantage of the diagnostic equipment. The UV corona camera developed a $6.4^{\circ}{\times}4.8^{\circ}$ of the field of view as a conventional camera to diagnose a wide range of slightly enlarged, and power equipment to measure the distance between the camera and the distance meter has been attached. The transmission between 250 to 280nm was 11% ($12.5%{\times}88%{\times}98%$) by combing the transmission on absorption film, window and other filter(UG 5, nickel sulphate and so on). In a distance of 5m with the UV corona camera it is possible to detect partial discharge with a PD level of 2.5pC and a RIV level of $3.6dB{\mu}V$.

THE SOLAR-B MISSION

  • ICHIMOTO KIYOSHI;TEAM THE SOLAR-B
    • Journal of The Korean Astronomical Society
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    • v.38 no.2
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    • pp.307-310
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    • 2005
  • The Solar-B is the third Japanese spacecraft dedicated for solar physics to be launched in summer of 2006. The spacecraft carries a coordinated set of optical, EUV and X-ray instruments that will allow a systematic study of the interaction between the Sun's magnetic field and its high temperature, ionized atmosphere. The Solar Optical Telescope (SOT) consists of a 50cm aperture diffraction limited Gregorian telescope and a focal plane package, and provides quantitative measurements of full vector magnetic fields at the photosphere with spatial resolution of 0.2-0.3 arcsec in a condition free from terrestrial atmospheric seeing. The X-ray telescope (XRT) images the high temperature (0.5 to 10 MK) corona with improved spatial resolution of approximately 1 arcsec. The Extreme Ultraviolet Imaging Spectrometer (EIS) aims to determine velocity fields and other plasma parameters in the corona and the transition region. The Solar-B telescopes, as a whole, will enable us to explore the origins of the outer solar atmosphere, the corona, and the coupling between the fine magnetic structure at the photosphere and the dynamic processes occurring in the corona. The mission instruments (SOT/EIS/XRT) are joint effort of Japan (JAXA/NAO), the United States (NASA), and the United Kingdom (PPARC). An overview of the spacecraft and its mission instruments are presented.

Motor Function Recovery in Stroke Patients with Corona Radiata Infarct: 4 Case Studies

  • Kim, Chung-Sun;Kwon, Jung-Won
    • The Journal of Korean Physical Therapy
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    • v.22 no.3
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    • pp.31-35
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    • 2010
  • Purpose: The aim of this study was to use fMRI and clinical prognosis criteria to evaluate therapeutic interventions in stroke patients with corona radiata infarct and acquire fundamental information about recovery mechanisms. Methods: Four subjects (2 men, 2 women) who had strokes with corona radiata infarct were recruited. For all subjects, motor functions such as motricity index (MI), modified brunnstrom classification (MBC), functional ambulatory category (FAC), and bathel index (BI) were evaluated. Evaluations were done at least 4 times over a period of approximately 6~7 months from stroke onset. We compared the final evaluation with the first. Results: All patients with corona radiata infarct showed improvement in motor outcomes with the passing of time. The strength of all patients improved from zero or trace levels to normal or good levels in the MI (Motricity Index) test. Other motor outcomes including the modified brunnstrom classification (MBC), the functional ambulatory category (FAC), and the bathel index (BI) also improved with the passing of time. Conclusion: Stroke patients with corona radiata infarcts change for the better over time. Therefore, one can introduce clinical interventions by the aspect of progress in functional motor recovery.

CME propagation and proton acceleration in solar corona

  • Kim, Roksoon;Kwon, Ryunyoung;Lee, Jaeok;Lario, David
    • The Bulletin of The Korean Astronomical Society
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    • v.43 no.1
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    • pp.53.3-54
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    • 2018
  • Solar Proton Events (SPEs) are the energetic phenomena related particle acceleration occurred in solar corona. Conventionally, they have been classified into two groups as the impulsive and gradual cases caused by reconnection in the flaring site and by shock generated by CME, respectively. In the previous studies, we classified these into four groups by analyzing the proton acceleration patterns in multi-energy channel observation. This showed that acceleration due to the magnetic reconnection may occur in the corona region relatively higher than the flaring site. In this study, we analyzes 54 SPEs observed in the energy band over 25 MeV from 2009 to 2013, where STEREO observations as well as SOHO can be utilized. From the multi-positional observation, we determine the exact time at which the Sun-Earth magnetic field line meets the CME shock structure by considering 3-dimensional structure of CME. Also, we determine the path length by considering the solar wind velocity for each event, so that the SPE onset time near the sun is obtained more accurately. Based on this study, we can get a more understanding of the correlation between CME progression and proton acceleration in the solar coronal region.

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COMPARISON OF LOS DOPPLER VELOCITIES AND NON-THERMAL LINE WIDTHS IN THE OFF-LIMB SOLAR CORONA MEASURED SIMULTANEOUSLY BY COMP AND HINODE/EIS

  • Lee, Jae-Ok;Lee, Kyoung-Sun;Seough, Jungjoon;Cho, Kyung-Suk
    • Journal of The Korean Astronomical Society
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    • v.54 no.2
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    • pp.49-60
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    • 2021
  • Observations of line of sight (LOS) Doppler velocity and non-thermal line width in the off-limb solar corona are often used for investigating the Alfvén wave signatures in the corona. In this study, we compare LOS Doppler velocities and non-thermal line widths obtained simultaneously from two different instruments, Coronal Multichannel Polarimeter (CoMP) and Hinode/EUV Imaging Spectrometer (EIS), on various off-limb coronal regions: flaring and quiescent active regions, equatorial quiet region, and polar prominence and plume regions observed in 2012-2014. CoMP provides the polarization at the Fe xiii 10747 Å coronal forbidden lines which allows their spectral line intensity, LOS Doppler velocity, and line width to be measured with a low spectral resolution of 1.2 Å in 2-D off limb corona between 1.05 and 1.40 RSun, while Hinode/EIS gives us the EUV spectral information with a high spectral resolution (0.025 Å) in a limited field of view raster scan. In order to compare them, we make pseudo raster scan CoMP maps using information of each EIS scan slit time and position. We compare the CoMP and EIS spectroscopic maps by visual inspection, and examine their pixel to pixel correlations and percentages of pixel numbers satisfying the condition that the differences between CoMP and EIS spectroscopic quantities are within the EIS measurement accuracy: ±3 km s-1 for LOS Doppler velocity and ±9 km s-1 for non-thermal width. The main results are summarized as follows. By comparing CoMP and EIS Doppler velocity distributions, we find that they are consistent with each other overall in the active regions and equatorial quiet region (0.25 ≤ CC ≤ 0.7), while they are partially similar to each other in the overlying loops of prominences and near the bottom of the polar plume (0.02 ≤ CC ≤ 0.18). CoMP Doppler velocities are consistent with the EIS ones within the EIS measurement accuracy in most regions (≥ 87% of pixels) except for the polar region (45% of pixels). We find that CoMP and EIS non-thermal width distributions are similar overall in the active regions (0.06 ≤ CC ≤ 0.61), while they seem to be different in the others (-0.1 ≤ CC ≤ 0.00). CoMP non-thermal widths are similar to EIS ones within the EIS measurement accuracy in a quiescent active region (79% of pixels), while they do not match in the other regions (≤ 61% of pixels); the CoMP observations tend to underestimate the widths by about 20% to 40% compared to the EIS ones. Our results demonstrate that CoMP observations can provide reliable 2-D LOS Doppler velocity distributions on active regions and might provide their non-thermal width distributions.