Stream structure and coronal sources of the solar wind during the May 12th, 1997 CME

Arge, C. N.; Luhmann, J. G.; Odstrčil, D.; Schrijver, Carolus J.; Li, Y.

doi:10.1016/j.jastp.2004.03.018

Cited by 306 publications

(352 citation statements)

References 31 publications

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“…The symmetric halo CME was associated with the best-known symmetric EIT double dimming, an EIT wave with a circular wave front and a C1.3 X-ray flare. The counter-part ICME containing a magnetic cloud was observed in-situ on 15 May at the L1 point by the Wind satellite (Webb et al, 2000;Arge et al, 2004). The 12 May halo CME has been a focused event for many coordinated research efforts.…”

Section: Introductionmentioning

confidence: 99%

Sequential Coronal Mass Ejections from AR8038 in May 1997

Lynch

Welsch

et al. 2010

Sol Phys

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Three homologous coronal mass ejections (CMEs) occurred on 5, 12 and 16 May 1997 from the single magnetic polarity inversion line (PIL) of AR8038. The three events together provide STEREO-like quadrature views of the 12 May 1997 CME and EIT double dimming. The recurrent CMEs with the nearly identical post-CME potential state and the 'sigmoid to arcade to sigmoid' transformations indicate a repeatable store -release -restore process of the free energy. How was the free magnetic energy re-introduced to the potential state corona after each release in this decaying active region? Making use of the known time Electronic supplementary material The online version of this article (doi:10.1007/s11207-010-9547-y) contains supplementary material, which is available to authorized users. interval bounded by the adjacent homologous CMEs, we made the following measures. The unsigned magnetic flux of AR8038, AR , decreased by approximately 18% during 66 h, while the unsigned flux, PIL , in a Gaussian-weighted PIL-region containing the flare site increased by about 50% during 36 hrs prior to the C1.3 flare on 12 May 1997. The significant increase of PIL demonstrates the magnetic gradient increase and the build-up of free energy in the PIL-region during the time leading to the eruption. Fourier local correlation tracking (FLCT) flow speed in AR8038 ranges from 0 to 292.8 m s −1 with a mean value of 63.2 m s −1 . The flow field contains a persistent converging flow towards the flaring PIL and an effective shear flow distributed in the AR. Minor angular motions were found. An integrated proxy Poynting flux S h estimates the energy input to the corona to be on the order of 1.15 × 10 32 erg during the 66 hrs before the C1.3 flare. It suggests that sufficient energy for a flare/CME can be introduced to the corona on the order of several days by the flows deduced from photospheric magnetic field motions in this small decaying active region.

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Section: Introductionmentioning

confidence: 99%

Sequential Coronal Mass Ejections from AR8038 in May 1997

Lynch

Welsch

et al. 2010

Sol Phys

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“…Observationally, the solar wind speeds as measured insitu are found to correlate with the expansion rate of the flux tube in the corona [54] and the angular distance from the flux tube footpoints to nearby coronal holes [55]. This provides support to the wave-driven scenario of the solar wind origin.…”

Section: Acceleration Of the Slow Solar Wind Associated With Coronal mentioning

confidence: 59%

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Chen

2013

Chin. Sci. Bull.

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In this article I present a review of recent studies on coronal dynamics, including research progresses on the physics of coronal streamers that are the largest structure in the corona, physics of coronal mass ejections (CMEs) that may cause a global disturbance to the corona, as well as physics of CME-streamer interactions. The following topics will be discussed in depth: (1) acceleration of the slow wind flowing around the streamer considering the effect of magnetic flux tube curvature; (2) physical mechanism accounting for persistent releases of streamer blobs and diagnostic results on the temporal variability of the slow wind speed with such events; (3) force balance analysis and energy release mechanism of CMEs with a flux rope magnetohydrodynamic model; (4) statistical studies on magnetic islands along the coronal-ray structure behind a CME and the first observation of magnetic island coalescence with associated electron acceleration; and (5) white light and radio manifestations of CME-streamer interactions. These studies shed new light on the physics of coronal streamers, the acceleration of the slow wind, the physics of solar eruptions, the physics of magnetic reconnection and associated electron acceleration, the large-scale coronal wave phenomenon, as well as the physics accounting for CME shock-induced type II radio bursts. solar wind, coronal streamer, coronal mass ejection, solar radio burst, magnetic reconnection Citation:Chen Y. A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions.

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“…Based on the photospheric magnetograph from the Mount Wilson Observatory (MWO, Ulrich et al, 2002), the Wang -Sheeley -Arge (WSA) coronal model (Arge et al, 2004, and references therein) can derive the coronal field and solar wind speed at 21.5 solar radii (R s ). Figure 1 illustrates such a case for CR 2055 longitude 60°-CR 2056 longitude 60°.…”

Section: Sta and Stb: 7 -8 May 2007mentioning

confidence: 99%

“…The areas shaded light (or dark) gray are closed field lines with B r > 0 (or B r < 0) in the photosphere. The color scale indicates the solar wind speed at 21.5 R s (related to the expansion factor, see Arge et al, 2004, and references therein) associated with the flux tubes. In all three panels, the + symbol marks the daily position of the sub-Earth point on the Sun.…”

Section: Sta and Stb: 7 -8 May 2007mentioning

confidence: 99%

“…This perihelion pass provides a good opportunity to study the radial evolution of an SIR from 1 to 1.4 AU, which will be addressed later in this article by investigating the August event. We use the 4-min resolution plasma data from the Solar Wind Observations Over the Poles of the Sun (SWOOPS) instrument (Bame et al, 1992) and magnetic field data from the magnetometer (Balogh et al, 1992) onboard the Ulysses spacecraft. To identify shocks, 1-sec resolution magnetic field data are also used.…”

Section: Introductionmentioning

confidence: 99%

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Multi-Spacecraft Observations: Stream Interactions and Associated Structures

et al. 2009

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The stream interaction region (SIR), formed when a fast stream overtakes a preceding slow stream, is the predominant large-scale solar wind structure at this early phase of the STEREO mission. Using multi-spacecraft observations from STEREO A and B, ACE, Wind, and Ulysses in 2007, we analyze three stream interaction events in depth in May, August, and November of 2007, respectively, when the spacecraft had quite different spatial separations. We attempt to determine the causes of the differences in the SIR properties, whether they are spatial or temporal variations, and also to examine the steepening or widening of the SIR during its radial evolution. The presence and characteristics of associated shocks, the relation to the heliospheric current sheet, and other structures are also studied.

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Stream structure and coronal sources of the solar wind during the May 12th, 1997 CME

Cited by 306 publications

References 31 publications

Sequential Coronal Mass Ejections from AR8038 in May 1997

Sequential Coronal Mass Ejections from AR8038 in May 1997

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Multi-Spacecraft Observations: Stream Interactions and Associated Structures

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