Interplanetary and geomagnetic consequences of 5 January 2005 CMEs associated with eruptive filaments

Sharma, Rahul; Srivastava, Nandita; Chakrabarty, D.; Möstl, Christian; Hu, Qiang

doi:10.1002/jgra.50362

Cited by 23 publications

(13 citation statements)

References 135 publications

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“…Here we have to remind that the solar wind plasma of very high density was originated from an erupting filament [Foullon et al, 2007], which usually contains a significant portion of He. Sharma et al [2013] reported very large He to proton ratio of >20% in the filament plasma observed by ACE/Solar Wind Ion Composition Spectrometer on 7-8 January 2005. It is important to note that those days were not accompanied either by enhanced SEP fluxes or by very fast solar wind and, hence, the Composition Aperture telescope onboard ACE was operating safely.…”

Section: Discussionmentioning

confidence: 94%

“…Sharma et al . [] reported very large He to proton ratio of >20% in the filament plasma observed by ACE/Solar Wind Ion Composition Spectrometer on 7–8 January 2005. It is important to note that those days were not accompanied either by enhanced SEP fluxes or by very fast solar wind and, hence, the Composition Aperture telescope onboard ACE was operating safely.…”

Section: Discussionmentioning

confidence: 99%

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Anomalous dynamics of the extremely compressed magnetosphere during 21 January 2005 magnetic storm

et al. 2014

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The dayside magnetosphere and proton radiation belt were analyzed during unusual magnetic storm on 21 January 2005. We have found that from 1712 to 2400 UT, the subsolar magnetopause was continuously located inside geosynchronous orbit due to strong compression. The compression was extremely strong from 1846 to 2035 UT when the dense plasma of fast erupting filament produced the solar wind dynamic pressure that peaked up to > 100 nPa, and during the first time, the upstream solar wind was observed at geosynchronous orbit for almost 2 h. Under the extreme compression, the outer magnetosphere at L > 5 was pushed inward, and the outer radiation belt particles moved earthward, became adiabatically accelerated, and accumulated in the inner magnetosphere at L < 4 that produced the intensified ring current with an exceptionally long lifetime. The observations were compared with predictions of various empirical and first-principles models. All the models failed to predict the magnetospheric dynamics under the extreme compression when the minimal magnetopause distance was estimated to be~3 RE. The inconsistencies might result from distortions of plasma measurements by extreme heliospheric conditions consisting in very fast solar wind streams and intense fluxes of solar energetic particles. We speculated that anomalous dynamics of the magnetosphere could be well described by the models if the He abundance in the solar wind was assumed to be > 20%, which is well appropriate for erupting filaments and which is in agreement with the upper 27% threshold for the He/H ratio obtained from Cluster measurements.

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Section: Discussionmentioning

confidence: 94%

Section: Discussionmentioning

confidence: 99%

Anomalous dynamics of the extremely compressed magnetosphere during 21 January 2005 magnetic storm

et al. 2014

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“…All the significant filaments identified to date have been different in their charge-state composition and in the distribution of cold filament material within and surrounding the ICME [cf. Burlaga et al, 1998;Skoug et al, 1999;Farrugia et al, 2002;Lepri and Zurbuchen, 2010;Sharma et al, 2013] suggesting that complex processes are responsible for their transport to 1 AU.…”

Section: Introductionmentioning

confidence: 99%

Earth's collision with a solar filament on 21 January 2005: Overview

et al. 2013

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, one of the fastest interplanetary coronal mass ejections (ICME) of solar cycle 23, containing exceptionally dense plasma directly behind the sheath, hit the magnetosphere. We show from charge-state analysis that this material was a piece of the erupting solar filament and further, based on comparisons to the simulation of a fast CME, that the unusual location of the filament material was a consequence of three processes. As the ICME decelerated, the momentum of the dense filament material caused it to push through the flux rope toward the nose. Diverging nonradial flows in front of the filament moved magnetic flux to the sides of the ICME. At the same time, reconnection between the leading edge of the ICME and the sheath magnetic fields worked to peel away the outer layers of the flux rope creating a remnant flux rope and a trailing region of newly opened magnetic field lines. These processes combined to move the filament material into direct contact with the ICME sheath region. Within 1 h after impact and under northward interplanetary magnetic field (IMF) conditions, a cold dense plasma sheet formed within the magnetosphere from the filament material. Dense plasma sheet material continued to move through the magnetosphere for more than 6 h as the filament passed by the Earth. Densities were high enough to produce strong diamagnetic stretching of the magnetotail despite the northward IMF conditions and low levels of magnetic activity. The disruptions from the filament collision are linked to an array of unusual features throughout the magnetosphere, ionosphere, and atmosphere. These results raise questions about whether rare collisions with solar filaments may, under the right conditions, be a factor in producing even more extreme events.

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“…3D rendering of associated plasma structures is done by the use of time dependent reconstruction algorithm (Jackson et al, 2002, and references therein). Sharma et al (2013) reported the event by the study of remote and in-situ observations of two CMEs associated with an active region and quiescent filaments on 5 January 2005. The first CME was associated with an east -west oriented filament and was slow in velocity and acceleration as compared to the second north -south oriented filament.…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

“…At their interface region, these magnetic clouds have embedded filament plasma that shows complex magnetic structures with a distinct magnetic flux rope configuration; these have been modeled by the Grad -Shafranov reconstruction technique. The geomagnetic consequences of these structures have been associated with substorms in recovery phase of a storm and detailed analysis is presented in Sharma et al (2013). In the present paper, we highlight the comparison of shape and extent of two filament plasma remnants in magnetic clouds as revealed by three -dimensional (3D) reconstruction and analysis from the Solar Mass Ejection Imager (SMEI) data.…”

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confidence: 98%

Evolution of the 5 January 2005 CMEs associated with eruptive filaments in inner heliosphere

Sharma¹,

Srivastava

Jackson

et al. 2013

Proc. IAU

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Abstract. On 5 January 2005, SoHO/LASCO observed two CMEs associated with eruptive filaments with different initial velocities and acceleration. The second CME accelerates much faster than the previous and the resulting interaction has been revealed in in-situ spacecraft measurements by the presence of magnetic holes at the border of the two distinct magnetic clouds. At their interface region, these magnetic clouds have embedded filament plasma that shows complex magnetic structures with a distinct magnetic flux rope configuration; these have been modeled by the Grad -Shafranov reconstruction technique. The geomagnetic consequences of these structures have been associated with substorms in recovery phase of a storm and detailed analysis is presented in Sharma et al. (2013). In the present paper, we highlight the comparison of shape and extent of two filament plasma remnants in magnetic clouds as revealed by three -dimensional (3D) reconstruction and analysis from the Solar Mass Ejection Imager (SMEI) data. The results provide an overview of the two eruptive filaments on 5 January 2005 and their interplanetary propagation.

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Interplanetary and geomagnetic consequences of 5 January 2005 CMEs associated with eruptive filaments

Cited by 23 publications

References 135 publications

Anomalous dynamics of the extremely compressed magnetosphere during 21 January 2005 magnetic storm

Anomalous dynamics of the extremely compressed magnetosphere during 21 January 2005 magnetic storm

Earth's collision with a solar filament on 21 January 2005: Overview

Evolution of the 5 January 2005 CMEs associated with eruptive filaments in inner heliosphere

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