Earth-affecting solar transients: a review of progresses in solar cycle 24

Zhang, J.; Temmer, Manuela; Gopalswamy, Ν.; Malandraki, O.; Nitta, N.; Patsourakos, S.; Shen, Fang; Vršnak, Bojan; Wang, Yuming; Webb, D. F.; Desai, M. I.; Dissauer, Karin; Dresing, Nina; Dumbović, Mateja; Feng, Xueshang; Heinemann, Stephan G.; Laurenza, M.; Lugaz, Noé; Zhuang, Bin

doi:10.1186/s40645-021-00426-7

Cited by 69 publications

(40 citation statements)

References 911 publications

(1,079 reference statements)

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“…The magnetic structure of coronal mass ejections (CMEs) is primarily known from direct in situ measurements of their magnetic field in the heliosphere and through reconstruction and fitting of magnetic field measurements, both in the photosphere and heliosphere (e.g., see the recent review by Zhang et al 2021). Multispacecraft measurements of CMEs, while rare, have been central in revealing that CMEs are global structures (Burlaga et al 1982) that can often be understood as near-force-free flux ropes (Burlaga 1988).…”

Section: Introductionmentioning

confidence: 99%

A Coronal Mass Ejection and Magnetic Ejecta Observed In Situ by STEREO-A and Wind at 55° Angular Separation

Lugaz

Salman

Zhuang

et al. 2022

ApJ

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We present an analysis of in situ and remote-sensing measurements of a coronal mass ejection (CME) that erupted on 2021 February 20 and impacted both the Solar TErrestrial RElations Observatory (STEREO)-A and the Wind spacecraft, which were separated longitudinally by 55°. Measurements on 2021 February 24 at both spacecraft are consistent with the passage of a magnetic ejecta (ME), making this one of the widest reported multispacecraft ME detections. The CME is associated with a low-inclined and wide filament eruption from the Sun’s southern hemisphere, which propagates between STEREO-A and Wind around E34. At STEREO-A, the measurements indicate the passage of a moderately fast (∼425 km s−1) shock-driving ME, occurring 2–3 days after the end of a high speed stream (HSS). At Wind, the measurements show a faster (∼490 km s−1) and much shorter ME, not preceded by a shock nor a sheath, and occurring inside the back portion of the HSS. The ME orientation measured at both spacecraft is consistent with a passage close to the legs of a curved flux rope. The short duration of the ME observed at Wind and the difference in the suprathermal electron pitch-angle data between the two spacecraft are the only results that do not satisfy common expectations. We discuss the consequence of these measurements on our understanding of the CME shape and extent and the lack of clear signatures of the interaction between the CME and the HSS.

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Section: Introductionmentioning

confidence: 99%

A Coronal Mass Ejection and Magnetic Ejecta Observed In Situ by STEREO-A and Wind at 55° Angular Separation

Lugaz

Salman

Zhuang

et al. 2022

ApJ

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“…The altered properties of CMEs resulted space weather that is milder than what is expected from the reduced activity alone. The same applies to space weather caused by CIRs [4,29,30]. Instead of looking at the intense geomagnetic storms, if one starts with the magnetic clouds (MCs) and examines their space weather impact, the reduction in geoeffectiveness (as measured by Dst) is again clear [23,30].…”

Section: Impact Of Weak Solar Activity In Cycle 24 On Space Weathermentioning

confidence: 99%

Solar activity and space weather

Gopalswamy

Mäkelä

Yashiro

et al. 2022

J. Phys.: Conf. Ser.

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After providing an overview of solar activity as measured by the sunspot number (SSN) and space weather events during solar cycles (SCs) 21-24, we focus on the weak solar activity in SC 24. The weak solar activity reduces the number of energetic eruptions from the Sun and hence the number of space weather events. The speeds of coronal mass ejections (CMEs), interplanetary (IP) shocks, and the background solar wind all declined in SC 24. One of the main heliospheric consequences of weak solar activity is the reduced total (magnetic + gas) pressure, magnetic field strength, and Alfvén speed. There are three groups of phenomena that decline to different degrees in SC 24 relative to the corresponding ones in SC 23: (i) those that decline more than SSN does, (ii) those that decline like SSN, and (iii) those that decline less than SSN does. The decrease in the number of severe space weather events such as high-energy solar energetic particle (SEP) events and intense geomagnetic storms is deeper than the decline in SSN. The reduction in the number of severe space weather events can be explained by the backreaction of the weak heliosphere on CMEs. CMEs expand anomalously and hence their magnetic content is diluted resulting in weaker geomagnetic storms. The reduction in the number of intense geomagnetic storms caused by corotating interaction regions is also drastic. The diminished heliospheric magnetic field in SC 24 reduces the efficiency of particle acceleration, resulting in fewer high-energy SEP events. The numbers of IP type II radio bursts, IP socks, and high-intensity energetic storm particle events closely follow the number of fast and wide CMEs (and approximately SSN) because all these phenomena are closely related to CME-driven shocks. The number of halo CMEs in SC 24 declines less than SSN does, mainly due to the weak heliospheric state. Phenomena such as IP CMEs and magnetic clouds related to frontside halos also do not decline significantly. The mild space weather is likely to continue in SC 25, whose strength has been predicted to be not too different from that of SC 24.

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“…The magnetic structure of coronal mass ejections (CMEs) is primarily known from direct in situ measurements of their magnetic field in the heliosphere and through reconstruction and fitting of magnetic field measurements, both in the photosphere and heliosphere (e.g., see recent review by Zhang et al 2021). Multi-spacecraft measurements of CMEs, while rare, have been central in revealing that CMEs are global structures (Burlaga et al 1982) that can often be understood as near-force-free flux ropes (Burlaga 1988).…”

Section: Introductionmentioning

confidence: 99%

A Coronal Mass Ejection and Magnetic Ejecta Observed In Situ by STEREO-A and Wind at 55$^\circ$ Angular Separation

Lugaz,

Salman,

Farrugia

et al. 2022

Preprint

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We present an analysis of in situ and remote-sensing measurements of a coronal mass ejection (CME) that erupted on 2021 February 20 and impacted both the Solar TErrestrial RElations Observatory (STEREO)-A and the Wind spacecraft, which were separated longitudinally by 55 • . Measurements on 2021 February 24 at both spacecraft are consistent with the passage of a magnetic ejecta (ME), making this one of the widest reported multi-spacecraft ME detections. The CME is associated with a low-inclined and wide filament eruption from the Sun's southern hemisphere, which propagates between STEREO-A and Wind around E34. At STEREO-A, the measurements indicate the passage of a moderately fast (∼ 425 km s −1 ) shock-driving ME, occurring 2-3 days after the end of a high speed stream (HSS). At Wind, the measurements show a faster (∼ 490 km s −1 ) and much shorter ME, not preceded by a shock nor a sheath, and occurring inside the back portion of the HSS. The ME orientation measured at both spacecraft is consistent with a passage close to the legs of a curved flux rope. The short duration of the ME observed at Wind and the difference in the suprathermal electron pitch-angle data between the two spacecraft are the only results that do not satisfy common expectations. We discuss the consequence of these measurements on our understanding of the CME shape and extent and the lack of clear signatures of the interaction between the CME and the HSS.

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Earth-affecting solar transients: a review of progresses in solar cycle 24

Cited by 69 publications

References 911 publications

A Coronal Mass Ejection and Magnetic Ejecta Observed In Situ by STEREO-A and Wind at 55° Angular Separation

A Coronal Mass Ejection and Magnetic Ejecta Observed In Situ by STEREO-A and Wind at 55° Angular Separation

Solar activity and space weather

A Coronal Mass Ejection and Magnetic Ejecta Observed In Situ by STEREO-A and Wind at 55$^\circ$ Angular Separation

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