Features and Properties of Coronal Mass Ejection/Flare Current Sheets

Lin, Jin‐Ming; Li, J.; Forbes, T. G.; Ko, Yuan‐Kuen; Raymond, J. C.; Vourlidas, A.

doi:10.1086/515568

Cited by 89 publications

(108 citation statements)

References 27 publications

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“…All times are UT. From Lin et al (2007) is a composite of LASCO C2 (at 17:50 UT), MK4 (17:49 UT), and EIT 195 Å (17:48 UT) images of the event, clearly illustrating the positions of the post-flare/CME loops, cusp point, and extended current sheet, which resembles the typical Kopp-Pneuman configuration for major flares]. Figure 11 indicates that the CS could extend up to 20 R .…”

Section: Upward Reconnection Outflowsmentioning

confidence: 94%

“…From Lin et al (2007) from either low density or high speed of H I atoms, or both. A low density of H I atoms means that the temperature is so high that H I atoms have mostly ionized.…”

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

“…The event studied by Ko et al (2003) occurred on the east limb The corresponding distances of two successive blobs are also indicated. From Lin et al (2007) and produced a fast CME associated with a growing SXR flare loop system (the main part of the flare was behind the limb so it is hard to determine the class of the flare). The advantage of studying this event is that it occurred on the limb and the current sheet above the flare loop system could be observed edge on, so that enough emission measure from the sheet would be collected and reliable diagnostics of plasma properties of the sheet could be performed.…”

Section: Upward Reconnection Outflowsmentioning

confidence: 99%

“…Figure 18 of Ko et al (2003) displays two examples, one showed accelerating motion pattern, and another one showed tendency of slowing down. Selecting 5 blobs with sharp edge that could be easily recognized and following their motions, Lin et al (2007) plotted their heights at different times as shown in Fig. 10, and further deduced the velocity of each blob, which is between 300 and 650 km s −1 .…”

Section: Upward Reconnection Outflowsmentioning

confidence: 99%

“…Different mechanisms could give rise to the same output. For example, Sweet-Parker CS with anomalous resistivity Biskamp 2000;Priest and Forbes 2000), Petschek-type reconnection (Petschek 1964;Biskamp 1986;Forbes and Priest 1987;Yokoyama and Shibata 1994;Kulsrud 2001;Drake et al 2006;Baty et al 2009;Vršnak et al 2009;Zweibel and Yamada 2009;Ko et al 2010;Liu et al 2012), and turbulent reconnection (Strauss 1988;Bhattacharjee and Yuan 1995;Lazarian and Vishniac 1999;Lin et al 2007Lin et al , 2009Lazarian et al , 2014. These different dissipation styles may even work together to yield a much more complex pattern and more efficient diffusion than that dominated only by a single mechanism (e.g., see also Mei et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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We introduce how the catastrophe model for solar eruptions predicted the formation and development of the long current sheet (CS) and how the observations were used to recognize the CS at the place where the CS is presumably located. Then, we discuss the direct measurement of the CS region thickness by studying the brightness distribution of the CS region at different wavelengths. The thickness ranges from 10 4 km to about 10 5 km at heights between 0.27 and 1.16 R from the solar surface. But the traditional theory indicates that the CS is as thin as the proton Larmor radius, which is of order tens of meters in the corona. We look into the huge difference in the thickness between observations and theoretical expectations. The possible impacts that affect measurements and results are studied, and physical causes leading to a thick CS region in which reconnection can still occur at a reasonably fast rate are analyzed. Studies in both theories and observations suggest that the difference between the true value and the apparent value of the CS thickness is not significant as long as the CS could be recognised in observations. We review observations that show complex structures and flows inside the CS region and present recent numerical modelling results on some aspects of these structures. Both observations and numerical experiments indicate that the downward reconnection outflows are usually slower than the upward ones in the same eruptive event. Numerical simulations show that the complex structure inside CS and its temporal behavior as a result of turbulence and the Petschek-type slow-mode shock could probably account for the thick CS and fast reconnection. But whether the CS itself is that thick still remains unknown since, for the time being, we cannot measure the electric current directly in that region. We also review the most recent laboratory experiments of reconnection driven by energetic laser beams, and discuss some important topics for future works.

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Section: Upward Reconnection Outflowsmentioning

confidence: 94%

“…From Lin et al (2007) from either low density or high speed of H I atoms, or both. A low density of H I atoms means that the temperature is so high that H I atoms have mostly ionized.…”

Section: The Reconnection Inflow Near the Current Sheetmentioning

confidence: 99%

Section: Upward Reconnection Outflowsmentioning

confidence: 99%

Section: Upward Reconnection Outflowsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Review on Current Sheets in CME Development: Theories and Observations

et al. 2015

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Operational Space Weather Services in National Space Science Center of Chinese Academy of Sciences

Liu¹,

Gong²

2015

Space Weather

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The Full-disk magnetograph is a main scientific payload onboard the Advanced Space based Solar Observatory (ASO-S/FMG) that through Stokes parameters' observation to measures the vector magnetic field. The accuracy of magnetic-field values is an important aspect of checking the quality of the FMG magnetic-field measurement. According to the design of the FMG, the linear calibration method under the weak-field approximation is the preferred scheme for magnetic-field calibration.However, the spacecraft orbital velocity can affect the position of observed spectral lines, then result in a change of the polarization-signal strength. Thus, the magnetic field is modulated by the orbit velocity of the spacecraft. In this article, through cross calibration between FMG and HMI (Helioseismic and Magnetic Imager onboard the Solar Dynamic Observatory), the effects of spacecraft orbital velocity on the coefficient of magnetic-field calibration are investigated. By comparing the magnetic field of FMG and HMI with spacecraft orbital velocity as an auxiliary reference, the revised linear-calibration coefficients that depend on spacecraft orbital velocity are obtained.Magnetic field of FMG corrected by the revised calibration coefficients removing the effect of spacecraft orbital velocity will be more accurate and suitable for scientific research.

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Astronomy and Astrophysics Library

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Features and Properties of Coronal Mass Ejection/Flare Current Sheets

Cited by 89 publications

References 27 publications

Review on Current Sheets in CME Development: Theories and Observations

Review on Current Sheets in CME Development: Theories and Observations

Operational Space Weather Services in National Space Science Center of Chinese Academy of Sciences

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