Solar Sources of Interplanetary Coronal Mass Ejections During the Solar Cycle 23/24 Minimum

Kilpua, Emilia; Mierla, M.; Zhukov, A. N.; Rodriguez, L.; Vourlidas, A.; Wood, Brian E.

doi:10.1007/s11207-014-0552-4

Cited by 56 publications

(67 citation statements)

References 57 publications

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“…However, all Earth-directed coronal events and their low coronal sources detected in STEREO/SECCHI EUVI could be associated subsequently, in the worst cases, to almost imperceptible activity on the best SDO/AIA images of the AR cluster at CM (see remarks on stealth CMEs in Howard and Harrison, 2013). Kilpua et al (2014) remarked that of the 16 CMEs related with their set of 20 ICMEs, 10 were stealth CMEs, i.e. they had no obvious EUV on-disk activity.…”

Section: Discussionmentioning

confidence: 98%

“…This result exceeds the 32 % frontside CMEs that cannot be recognized by SOHO found by Wang et al (2011) and the findings by Schwenn et al (2005), who could not associate an observable halo CME with nearly 20 % geoeffective interplanetary CMEs (ICMEs). On the other hand, after the analysis of 20 ICMEs detected in 2009 in the near-Earth solar wind by Kilpua et al (2014), only six events could be observed in SOHO/LASCO images, out of which only one was wider than 120 • . After considering STEREO data, they were able to find the coronal counterparts of 16 ICMEs.…”

Section: Discussionmentioning

confidence: 99%

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Coronal Mass Ejections from the Same Active Region Cluster: Two Different Perspectives

et al. 2015

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The cluster formed by active regions (ARs) NOAA 11121 and 11123, approximately located on the solar central meridian on 11 November 2010, is of great scientific interest. This complex was the site of violent flux emergence and the source of a series of Earth-directed events on the same day. The onset of the events was nearly simultaneously observed by the Atmospheric Imaging Assembly (AIA) telescope onboard the Solar Dynamics Observatory (SDO) and the Extreme-Ultraviolet Imagers (EUVI) on the Sun-Earth Connection Coronal and Heliospheric Investigation (SECCHI) suite of telescopes onboard the Solar-Terrestrial Relations Observatory (STEREO) twin spacecraft. The progression of these events in the low corona was tracked by the Large Angle Spectroscopic Coronagraphs (LASCO) onboard the Solar and Heliospheric Observatory (SOHO) and the SECCHI/COR coronagraphs on STEREO. SDO and SOHO imagers provided data from the Earth's perspective, whilst the STEREO twin instruments procured images from the orthogonal directions. This spatial configuration of spacecraft allowed optimum simultaneous observations of the AR cluster and the coronal mass ejections that originated in it. Quadrature coronal observations provided by STEREO revealed many more ejective events than were detected from Earth. Furthermore, joint observations by SDO/AIA and STEREO/SECCHI EUVI of the source region indicate that all events classified by GOES as X-ray flares had an ejective B H. Cremades H. Cremades et al. coronal counterpart in quadrature observations. These results directly affect current space weather forecasting because alarms might be missed when there is a lack of solar observations in a view direction perpendicular to the Sun-Earth line.

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Section: Discussionmentioning

confidence: 98%

Section: Discussionmentioning

confidence: 99%

Coronal Mass Ejections from the Same Active Region Cluster: Two Different Perspectives

et al. 2015

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“…Solar storms, their connections to magnetic sources in the Sun's atmosphere, and the resultant coronal mass ejections (CMEs) and interplanetary coronal mass ejections (ICMEs) observed at 1 AU have also been studied extensively but independently of their ionospheric impacts [e.g., Möstl et al ., ; Lugaz et al ., ; Davies et al ., ; Kilpua et al ., ; Li et al ., ; Möstl et al ., ; Patsourakos et al ., ]. These studies similarly categorize a solar storm's geoeffectiveness according to indices such as Kp , ap , and Dst .…”

Section: Introductionmentioning

confidence: 99%

Comparative ionospheric impacts and solar origins of nine strong geomagnetic storms in 2010–2015

et al. 2016

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For nine of the strongest geomagnetic storms in solar cycle 24 we characterize, quantify, and compare the impacts on ionospheric total electron content (TEC) and the U.S. Wide Area Augmentation System (WAAS) with the heliospheric morphology and kinematics of the responsible coronal mass ejections (CMEs) and their solar source regions. Regional TEC responses to the events are similar in many respects, especially in the initial positive phase. For the subsequent negative phase, Dst is a better indicator than ap of the magnitude of the TEC decrease. The five events that arrive between 13:00 UT and 21:00 UT (local daytime in the U.S.) produce large WAAS degradations, and the four events that arrive outside this time of day produce lesser or no WAAS degradation. Our sample of geoeffective events includes CMEs with only modestly fast speeds, ones that only provided glancing impacts on Earth by their shock sheaths and ones not associated with any significant flare. While all of the CMEs traveled faster than the solar wind, they nevertheless have a wide range of velocities and produced a range of Bz values; neither speed nor Bz correlates significantly with ionospheric impact. Comparison with the locations of surface activity leads to estimates of deflection for the CMEs, with the average deflection being 19°. At least a few events may have missed Earth entirely in the absence of coronal deflection.

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“…However, even in that case, the flux rope may still erupt due to a loss of equilibrium or an ideal MHD instability and no flare, brightening, or post-eruptive arcade need necessarily be observed as signatures of the eruption. This phenomenon is generally referred to as a stealth CME (Robbrecht et al 2009b;D'Huys et al 2014;Kilpua et al 2014). …”

Section: Models For Cme Initiationmentioning

confidence: 99%

Solar signatures and eruption mechanism of the August 14, 2010 coronal mass ejection (CME)

D’Huys

Seaton

Groof

et al. 2017

J. Space Weather Space Clim.

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On August 14, 2010 a wide-angled coronal mass ejection (CME) was observed. This solar eruption originated from a destabilized filament that connected two active regions and the unwinding of this filament gave the eruption an untwisting motion that drew the attention of many observers. In addition to the erupting filament and the associated CME, several other low-coronal signatures that typically indicate the occurrence of a solar eruption were associated with this event. However, contrary to what was expected, the fast CME (v > 900 km s À1 ) was accompanied by only a weak C4.4 flare. We investigate the various eruption signatures that were observed for this event and focus on the kinematic evolution of the filament in order to determine its eruption mechanism. Had this solar eruption occurred just a few days earlier, it could have been a significant event for space weather. The risk of underestimating the strength of this eruption based solely on the C4.4 flare illustrates the need to include all eruption signatures in event analyses in order to obtain a complete picture of a solar eruption and assess its possible space weather impact.

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Solar Sources of Interplanetary Coronal Mass Ejections During the Solar Cycle 23/24 Minimum

Cited by 56 publications

References 57 publications

Coronal Mass Ejections from the Same Active Region Cluster: Two Different Perspectives

Coronal Mass Ejections from the Same Active Region Cluster: Two Different Perspectives

Comparative ionospheric impacts and solar origins of nine strong geomagnetic storms in 2010–2015

Solar signatures and eruption mechanism of the August 14, 2010 coronal mass ejection (CME)

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