CORONAS‐F/SPIRIT EUV observations of October–November 2003 solar eruptive events in combination with SOHO/EIT data

Grechnev, V. V.; Chertok, I. M.; Slemzin, V. A.; Kuzin, S. V.; Ignat'ev, A. P.; Pertsov, A. A.; Zhitnik, I. A.; Delaboudinière, J. P.; Auchère, F.

doi:10.1029/2004ja010931

Cited by 36 publications

(24 citation statements)

References 35 publications

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“…It is interpreted as a density depletion associated with the CME initiation (Hudson & Webb 1997;Zarro et al 1999, and others). The procedure of image pre-processing and of selection of the dimming regions we used here was described in detail elsewhere (Chertok et al 2004;Slemzin et al 2005Slemzin et al , 2006. A detailed analysis of dimmings and their relationship with CMEs have been carried out in many papers (e.g.…”

Section: Euv Dimmingsmentioning

confidence: 99%

Analysis and interpretation of a fast limb CME with eruptive prominence, C-flare, and EUV dimming

Koutchmy¹,

Slemzin²,

Filippov³

et al. 2008

A&A

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Aims. Coronal mass ejections or CMEs are large dynamical solar-corona events. The mass balance and kinematics of a fast limb CME, including its prominence progenitor and the associated flare, will be compared with computed magnetic structures to look for their origin and effect. Methods. Multi-wavelength ground-based and spaceborne observations are used to study a fast W-limb CME event of December 2, 2003, taking into account both on and off disk observations. Its erupting prominence is measured at high cadence with the Pic du Midi full Hα line-flux imaging coronagraph. EUV images from SOHO/EIT and CORONAS-F/SPIRIT space instruments are processed including difference imaging. SOHO/LASCO images are used to study the mass excess and motions. Computed coronal structures from extrapolated surface magnetic fields are compared to observations. Results. A fast bright expanding coronal loop is identified in the region recorded slightly later by GOES as a C7.2 flare, followed by a brightening and an acceleration phase of the erupting material with both cool and hot components. The total coronal radiative flux dropped by ∼7% in the 19.5 nm channel and by 4% in the 17.5 nm channel, revealing a large dimming effect at and above the limb over a 2 h interval. The typical 3-part structure observed 1 h later by the Lasco C2 and C3 coronagraphs shows a core shaped similarly to the eruptive filament/prominence. The total measured mass of the escaping CME (∼1.5 × 10 16 g from C2 LASCO observations) definitely exceeds the estimated mass of the escaping cool prominence material although assumptions made to analyze the Hα erupting prominence, as well as the corresponding EUV darkening of the filament observed several days before, made this evaluation uncertain by a factor of 2. This mass budget suggests that the event is not confined to the eruption region alone. From the current free extrapolation we discuss the shape of the magnetic neutral surface and a possible scenario leading to an instability, including the small scale dynamics inside and around the filament.

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Section: Euv Dimmingsmentioning

confidence: 99%

Analysis and interpretation of a fast limb CME with eruptive prominence, C-flare, and EUV dimming

Koutchmy¹,

Slemzin²,

Filippov³

et al. 2008

A&A

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“…Afterwards, the ejecta does not resemble itself as it at the onset of the eruption was. An example is the 18.11.2003 event mentioned above [2,3], in which an eruptive filament encountered an invisible obstacle and visually transformed into two wide diverging jets carrying material of the filament to remote sites on the solar surface.…”

Section: Discussionmentioning

confidence: 99%

Solar flare-related eruptions followed by long-lasting occultation of the emission in the He II 304 Å line and in microwaves

et al. 2011

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Plasma with a temperature close to the chromospheric one is ejected in solar eruptions. Such plasma can occult some part of emission of compact sources in active regions as well as quiet solar areas. Absorption phenomena can be observed in the microwave range as the so-called "negative bursts" and also in the He II 304Å line. The paper considers three eruptive events associated with rather powerful flares. Parameters of absorbing material of an eruption are estimated from multi-frequency records of a "negative burst" in one event. "Destruction" of an eruptive filament and its dispersion like a cloud over a huge area observed as a giant depression of the 304Å line emission has been revealed in a few events. One such event out of three ones known to us is considered in this paper. Another event is a possibility. PACS numbers: 96.60.qf IntroductionProminences (filaments) in many solar events erupt and draw away from the Sun as parts of Coronal Mass Ejections (CMEs). Partial plasma flows from an eruptive prominence along its legs down to the solar surface are often observed. "Failed" eruptions are also known, when an eruptive prominence or filament after lift-off rapidly decelerates and falls at nearly the same position 1 where it was located before the eruption [1]. Observations of the 18.11.2003 eruptive event with the CORONAS-F/SPIRIT telescope in the He II 304Å line revealed one more scenario. An eruptive filament disintegrated to form a Y-like cloud, flew above the solar surface a distance of more than the solar radius and, probably, landed far from the eruption site [2,3]. A similar anomalous eruption was observed in the 13.07.2004 event [4]. Detailed observations of this event revealed an eruption from an active region of a compact filament and its subsequent dispersion over a huge area comparable with a quarter of the visible solar disk. These events were accompanied with impulsive flares.Eruptive events associated with flares produce various phenomena of different temporal and spatial scales. These phenomena are observed in diverse spectral domains (see [5]). These are flare arcades whose emission is registered from X-rays up to radio waves. Other phenomena are dimmings, i.e., depressions of soft X-ray and extreme ultraviolet (EUV) emissions that reach significant sizes and exist from a few hours up to two days. The major cause of quasi-stationary dimmings is plasma density decrease due to expansion of eruptive structures. Shock waves excited by impulsive eruptions from active regions are manifest in Moreton waves and some "EUV waves" (or "EIT waves"). Propagation of shock waves is traced from slowly drifting type II bursts at metric and decimetric waves. Most likely, shock waves form leading edges of fast CMEs, especially decelerating ones [6].Erupted plasmas with nearly chromospheric temperatures can occult some part of the solar emission and absorb its detectable fraction. Absorption phenomena are observed in various emission ranges. Erupted plasmas show up in the Hα line mainly as surges, which ...

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“…Chandra et al (2010) have convincingly confirmed this conjecture. This mismatch, along with the conclusion of Grechnev et al (2005) that the eruptive filament had not left the Sun, seems to be sufficient to warn against a simple scenario in which the MC is considered as a stretched magnetic rope initially associated with the pre-eruption filament in AR 10501. However, this circumstance was not fully acknowledged.…”

Section: Why the 18 -20 November 2003 Event Hindered Understanding?mentioning

confidence: 99%

“…A series of big eruptive flares in a complex of large super-active regions 10484, 10486, and 10488 occurred late in October 2003 (see, e.g., Veselovsky et al, 2004;Gopalswamy et al, 2005aGopalswamy et al, , 2005bGrechnev et al, 2005). These 'Halloween 2003 events' produced geomagnetic superstorms with Dst = −353 and −383 nT 1 on 29 -31 October.…”

Section: Introductionmentioning

confidence: 99%

A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. IV. Unusual Magnetic Cloud and Overall Scenario

et al. 2014

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The geomagnetic superstorm of 20 November 2003 with Dst = −422 nT, one of the most intense in history, is not well understood. The superstorm was caused by a moderate solar eruptive event on 18 November, comprehensively studied in our preceding Papers I -III. The analysis has shown a number of unusual and extremely complex features, which presumably led to the formation of an isolated right-handed magnetic-field configuration. Here we analyze the interplanetary disturbance responsible for the 20 November superstorm, compare some of its properties with the extreme 28 -29 October event, and reveal a compact size of the magnetic cloud (MC) and its disconnection from the Sun. Most likely, the MC had a spheromak configuration and expanded in a narrow angle of ≤ 14• . A very strong magnetic field in the MC up to 56 nT was due to the unusually weak expansion of the disconnected spheromak in an enhanced-density environment constituted by the tails of the preceding ICMEs. Additional circumstances favoring the superstorm were (i) the exact impact of the spheromak on the Earth's magnetosphere and (ii) the almost exact southward orientation of the magnetic field, corresponding to the original orientation in its probable source region near the solar disk center.

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CORONAS‐F/SPIRIT EUV observations of October–November 2003 solar eruptive events in combination with SOHO/EIT data

Cited by 36 publications

References 35 publications

Analysis and interpretation of a fast limb CME with eruptive prominence, C-flare, and EUV dimming

Analysis and interpretation of a fast limb CME with eruptive prominence, C-flare, and EUV dimming

Solar flare-related eruptions followed by long-lasting occultation of the emission in the He II 304 Å line and in microwaves

A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. IV. Unusual Magnetic Cloud and Overall Scenario

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