CME propagation through the heliosphere: Status and future of observations and model development

Temmer, Manuela; Scolini, Camilla; Richardson, I. G.; Heinemann, Stephan G.; Paouris, Evangelos; Vourlidas, A.; Bisi, M. M.; Al-Haddad, Nada; Amerstorfer, Tanja; Barnard, Luke; Burešová, Dalia; Hofmeister, Stefan J.; Iwai, Kazumasa; Jackson, B. V.; Jarolim, Robert; Jian, L. K.; Linker, J. A.; Lugaz, Noé; Manoharan, P. K.; Mays, M. L.; Mishra, Wageesh; Owens, M. J.; Palmerio, Erika; Perri, Barbara; Pomoell, Jens; Pinto, Rui; Samara, Evangelia; Singh, Talwinder; Verbeke, C.; Veronig, Astrid; Zhuang, Bin

doi:10.1016/j.asr.2023.07.003

Cited by 13 publications

(6 citation statements)

References 519 publications

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“…In other words, the parameter space of the simulation has a large number of poorly constrained degrees of freedom, thus making generalisation of the method for space weather forecasting applications particularly challenging. Extensive efforts dedicated to quantitative comparisons and performance benchmarking for each of these pieces of the modelling chain (e.g., Reiss et al, 2023a,b;Temmer et al, 2023;Whitman et al, 2023) will be increasingly important for model refinement and development and advancing our space weather prediction capabilities.…”

Section: Discussionmentioning

confidence: 99%

Improved modelling of SEP event onset within the WSA–Enlil–SEPMOD framework

Palmerio,

Luhmann,

Mays

et al. 2024

J. Space Weather Space Clim.

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Multi-spacecraft observations of solar energetic particle (SEP) events enable not only a for deeper understanding and development of particle acceleration and transport theories, but also provide important constraints for model validation efforts. However, because of computational limitations, a given physics-based SEP model is usually best-suited to capture a particular phase of an SEP event, rather than its whole development from onset through decay. For example, magnetohydrodynamic (MHD) models of the heliosphere often incorporate solar transients only at the outer boundary of their so-called coronal domain—usually set at a heliocentric distance of 20–30 R☉. This means that particle acceleration at CME-driven shocks is also computed from this boundary onwards, leading to simulated SEP event onsets that can be many hours later than observed, since shock waves can form much lower in the solar corona. In this work, we aim to improve the modelled onset of SEP events by inserting a "fixed source" of particle injection at the outer boundary of the coronal domain of the coupled WSA–Enlil 3D MHD model of the heliosphere. The SEP model that we employ for this effort is SEPMOD, a physics-based test-particle code based on a field line tracer and adiabatic invariant conservation. We apply our initial tests and results of SEPMOD's fixed-source option to the 2021 October 9 SEP event, which was detected at five well-separated locations in the inner heliosphere—Parker Solar Probe, STEREO-A, Solar Orbiter, BepiColombo, and near-Earth spacecraft.

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Section: Discussionmentioning

confidence: 99%

Improved modelling of SEP event onset within the WSA–Enlil–SEPMOD framework

Palmerio,

Luhmann,

Mays

et al. 2024

J. Space Weather Space Clim.

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“…These effects may be enhanced due to an interaction with other magnetic structures propagating in the heliosphere, primarily due to the compression of the existing B z magnetic field component (e.g., Farrugia et al 2006;Dumbović et al 2015;Lugaz et al 2017). The examination of interaction events involving CMEs (e.g., see Kilpua et al 2019;Scolini et al 2020) and their resulting geoeffectiveness has been recognized as one of the objectives outlined by the heliospheric clusters within the International Space Weather Action Teams (ISWAT), which serves as a roadmap for future research (Temmer et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Classification of Enhanced Geoeffectiveness Resulting from High-speed Solar Wind Streams Compressing Slower Interplanetary Coronal Mass Ejections

Heinemann,

Sishtla,

Good

et al. 2024

ApJL

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High-speed solar wind streams (HSSs) interact with the preceding ambient solar wind to form stream interaction regions (SIRs), which are a primary source of recurrent geomagnetic storms. However, HSSs may also encounter and subsequently interact with interplanetary coronal mass ejections (ICMEs). In particular, the impact of the interaction between slower ICMEs and faster HSSs represents an unexplored area that requires further in-depth investigation. This specific interaction can give rise to unexpected geomagnetic storm signatures, diverging from the conventional expectations of individual SIR events sharing similar HSS properties. Our study presents a comprehensive analysis of solar wind data spanning from 1996 to 2020, capturing 23 instances where such encounters led to geomagnetic storms (SymH < −30 nT). We determined that interaction events between preceding slower ICMEs and faster HSSs possess the potential to induce substantial storm activity, statistically nearly doubling the geoeffective impact in comparison to SIR storm events. The increase in the amplitude of the SymH index appears to result from heightened dynamic pressure, often coupled with the concurrent amplification of the CMEs rearward ∣B∣ and/or B z components.

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“…Impulsive CMEs have been on highlight due to their geoeffectiveness characteristic in causing geomagnetic storms as they mark high magnitudes in all properties. Gradual CMEs are less intense, yet they take a long time to reach the Earth which also can enhance their geoeffectiveness through long interaction with solar wind [17]. Apart from the presence of Moreton waves, impulsive CMEs are commonly linked to the solar radio bursts type II with harmonic structure and herringbone (HB) at angular widths greater than 60° and velocity greater than 500 km/s [18].…”

Section: Introductionmentioning

confidence: 99%

On propagation of gradual and impulsive Coronal Mass Ejections (CMEs)

Mohamad Ansor,

Hamidi,

Shariff

2024

J. Phys.: Conf. Ser.

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Coronal Mass Ejection (CME) is a significant solar activity that releases magnetic field and plasma out of the corona and they are known as the main driver of space weather. In general, CMEs are characterized as gradual and impulsive based on their kinematic properties that include velocity and acceleration. This paper is aimed to analyze the differences in behaviour of gradual and impulsive CME based on recent events (dates) in solar cycle 25 and to justify their characterizations that have been demonstrated a while ago. Data analysis is conducted by studying the height-time, height-velocity and height-acceleration profiles for each event, based on SOHO LASCO Catalogue. Results show that impulsive CME travels a lot faster than gradual CME, with average velocity of 1239 km/s and 503.6 km/s respectively. It is believed that M6.7 flare accompanying the impulsive CME has been the main reason to high velocity due to its ability to contribute more heat energy and enhances the energy conversion during magnetic reconnection. Deceleration is observed in impulsive CME that is caused by the loss of momentum as interacting with the background solar wind and small-scale acceleration is manifested by gradual CME all through the propagation.

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CME propagation through the heliosphere: Status and future of observations and model development

Cited by 13 publications

References 519 publications

Improved modelling of SEP event onset within the WSA–Enlil–SEPMOD framework

Improved modelling of SEP event onset within the WSA–Enlil–SEPMOD framework

Classification of Enhanced Geoeffectiveness Resulting from High-speed Solar Wind Streams Compressing Slower Interplanetary Coronal Mass Ejections

On propagation of gradual and impulsive Coronal Mass Ejections (CMEs)

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