A Major Geoeffective CME from NOAA 12371: Initiation, CME–CME Interactions, and Interplanetary Consequences

Joshi, Bhuwan; Ibrahim, M. Syed; Shanmugaraju, A.; Chakrabarty, D.

doi:10.1007/s11207-018-1325-2

Cited by 33 publications

(28 citation statements)

References 60 publications

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“…At the peak time of the flare (around 05:05 UT), we observed the type III burst in the frequency range of 150 MHz to 16 MHz. Type III burst implies the opening of the magnetic filed lines and subsequent ejection of relativistic electron beam (Joshi et al 2018). We can see that a type II radio burst is followed by the type III burst.…”

Section: Radio Observationsmentioning

confidence: 80%

“…These two pre-CMEs erupted consecutively around 01:25 UT and 04:24 UT. Very likely, because of the interaction, the first CME might have lost its energy (Gopalswamy et al 2001c;Yashiro et al 2014;Joshi et al 2018;Morosan et al 2020;Rodríguez Gómez et al 2020;Scolini et al 2020).…”

Section: Discussionmentioning

confidence: 99%

“…Geomagnetic storms are associated with CMEs and their interplanetary counterparts (Zurbuchen & Richardson 2006;Zhao & Dryer 2014;Kilpua et al 2017;Rubtsov et al 2018;Bravo et al 2019;Kharayat et al 2021). To understand the complex process associated with CME origin and its evolution in the interplanetary medium, it is necessary to connect the near-Sun observations, interplanetary radio emissions, and in-situ measurements at 1 AU (see e.g., Joshi et al 2018). In general, ICMEs acceleration and deceleration depends on their speed relative to the solar wind speed (Manoharan 2010;Shanmugaraju & Vršnak 2014;Shanmugaraju et al 2015;Joshi et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…To understand the complex process associated with CME origin and its evolution in the interplanetary medium, it is necessary to connect the near-Sun observations, interplanetary radio emissions, and in-situ measurements at 1 AU (see e.g., Joshi et al 2018). In general, ICMEs acceleration and deceleration depends on their speed relative to the solar wind speed (Manoharan 2010;Shanmugaraju & Vršnak 2014;Shanmugaraju et al 2015;Joshi et al 2018). Slow CMEs are accelerated by the solar wind while the fast CMEs are decelerated by the solar wind.…”

Section: Introductionmentioning

confidence: 99%

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Investigation of two coronal mass ejections from circular ribbon source region: Origin, Sun-Earth propagation and Geo-effectiveness

Ibrahim,

Uddin,

Joshi

et al. 2021

Preprint

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In this article, we compare the properties of two coronal mass ejections (CMEs) that show similar source region characteristics but different evolutionary behavior in the later phases. We discuss the two events in terms of their near-Sun characteristics, interplanetary evolution, and geo-effectiveness. We carefully analyzed the initiation and propagation parameters of these events to establish the precise CME-ICME connection and their near-Earth consequences. The First event was associated with poor geo-magentic storm disturbance index (Dst ≈-20 nT) while the second event is associated with intense geomagnetic storm of DST ≈-119 nT. The configuration of the sunspots in the active regions and their evolution are observed by Helioseismic and Magnetic Imager (HMI). For source region imaging, we rely on data obtained from Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory (SDO) and Hα filtergrams from Solar Tower Telescope at Aryabhatta Research Institute of Observational Sciences (ARIES). For both the CMEs, flux rope eruptions from the source region triggered flares of similar intensities (≈M1). At the solar source region of the eruptions, we observed circular ribbon flare (CRF) for both the cases, suggesting fan-spine magnetic configuration in the active region corona. The multi-channel SDO observations confirm that the eruptive flares and subsequent CMEs were intimately related to the filament eruption. Within the field of views of Large Angle Spectrometric Coronograph (LASCO) field of view (FOV) the two CMEs propagated with linear speeds of 671 and 631 km s −1 , respectively. These CMEs were tracked up to the Earth by Solar Terrestrial and Relational Observatory (STEREO) instruments. We find that the source region evolution of CMEs, guided by the large-scale coronal magnetic field configuration, along with near-Sun propagation characteristics, such as, CME-CME interactions, played important roles in deciding the

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Section: Radio Observationsmentioning

confidence: 80%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Investigation of two coronal mass ejections from circular ribbon source region: Origin, Sun-Earth propagation and Geo-effectiveness

Ibrahim,

Uddin,

Joshi

et al. 2021

Preprint

Self Cite

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show abstract

“…MFRs not only play a crucial role in triggering the eruption but also constitute a key component of CMEs. Near-Earth in-situ measurements often reveal evidence of MFRs at large-scales in the form of interplanetary magnetic clouds signifying the arrival of Earth-directed CMEs (Burlaga et al 1981;Klein & Burlaga 1982;Burlaga et al 1998;Möstl et al 2009;Syed Ibrahim et al 2019), that may subsequently cause geomagnetic disturbances when interacting with Earth's magnetic field (Zhang & Burlaga 1988;Burlaga et al 2001;Zurbuchen & Richardson 2006;Bisoi et al 2016;Joshi et al 2018). Here some basic questions arise: how do MFRs originate in the solar corona and what are the mechanisms responsible for their eruptions?…”

Section: Introductionmentioning

confidence: 99%

HXR emission from an activated flux rope and subsequent evolution of an eruptive long duration solar flare

Sahu,

Joshi,

Mitra

et al. 2020

Preprint

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In this paper, we present a comprehensive study of the evolutionary phases of a major M6.6 long duration event (LDE) with special emphasize on its pre-flare phase. The event occurred in NOAA 12371 on 2015 June 22. A remarkable aspect of the event was an active pre-flare phase lasting for about an hour during which a hot EUV coronal channel was in build-up stage and displayed co-spatial hard X-ray (HXR) emission up to energies of 25 keV. As such, this is the first evidence of HXR coronal channel. The coronal magnetic field configuration based on NLFFF modeling clearly exhibited a magnetic flux rope (MFR) oriented along the polarity inversion line (PIL) and co-spatial with the coronal channel. We observed significant changes in the AR's photospheric magnetic field during an extended period of ≈42 hours in the form of rotation of sunspots, moving magnetic features, and flux cancellation along the PIL. Prior to the flare onset, the MFR underwent a slow rise phase (≈14 km s −1 ) for ≈12 min which we attribute to the faster build-up and activation of the MFR by tethercutting reconnection occurring at multiple locations along the MFR itself. The sudden transition in the kinematic evolution of the MFR from the phase of slow to fast rise (≈109 km s −1 with acceleration ≈110 m s −2 ) precisely divides the pre-flare and impulsive phase of the flare, which points toward the feedback process between the early dynamics of the eruption and the strength of the flare magnetic reconnection.

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Study of the travelling interplanetary shocks, their earth crossings and resulting geomagnetic disturbances

Badruddin

Kumar

Derouich

2019

Astrophys Space Sci

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A Major Geoeffective CME from NOAA 12371: Initiation, CME–CME Interactions, and Interplanetary Consequences

Cited by 33 publications

References 60 publications

Investigation of two coronal mass ejections from circular ribbon source region: Origin, Sun-Earth propagation and Geo-effectiveness

Investigation of two coronal mass ejections from circular ribbon source region: Origin, Sun-Earth propagation and Geo-effectiveness

HXR emission from an activated flux rope and subsequent evolution of an eruptive long duration solar flare

Study of the travelling interplanetary shocks, their earth crossings and resulting geomagnetic disturbances

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