Coronal Mass Ejections over Solar Cycles 23 and 24

Lamy, Philippe; Floyd, Olivier; Boclet, Brice; Wojak, Julien; Gilardy, Hugo; Barlyaeva, Tatiana

doi:10.1007/s11214-019-0605-y

Cited by 104 publications

(107 citation statements)

References 198 publications

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“…Studies have revealed that CMEs usually undergo three stages of dynamic evolution: a slow rise, a fast acceleration, and a propagation phase (Zhang et al 2001(Zhang et al , 2004. The final speed of a CME varies in a wide range of about 100-3500 kms −1 (e.g., Gopalswamy et al 2009;Lamy et al 2019), while its main acceleration usually takes place within a few to tens of minutes at low coronal heights (e.g., Zhang et al 2001;Vršnak et al 2007;Temmer et al 2008;Bein et al 2011;Veronig et al 2018), where the Lorenz force that accounts for the liftoff of a CME is strong.…”

Section: Introductionmentioning

confidence: 99%

Solar Flare–CME Coupling throughout Two Acceleration Phases of a Fast CME

Gou

Veronig

Liu

et al. 2020

ApJL

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Solar flares and coronal mass ejections (CMEs) are closely coupled through magnetic reconnection. CMEs are usually accelerated impulsively within the low solar corona, synchronized with the impulsive flare energy release. We investigate the dynamic evolution of a fast CME and its associated X2.8 flare occurring on 2013 May 13. The CME experiences two distinct phases of enhanced acceleration, an impulsive one with a peak value of ∼5 kms −2 , followed by an extended phase with accelerations up to 0.7 kms −2. The two-phase CME dynamics is associated with a two-episode flare energy release. While the first episode is consistent with the "standard" eruption of a magnetic flux rope, the second episode of flare energy release is initiated by the reconnection of a large-scale loop in the aftermath of the eruption and produces stronger nonthermal emission up to γ-rays. In addition, this longduration flare reveals clear signs of ongoing magnetic reconnection during the decay phase, evidenced by extended hard X-ray bursts with energies up to 100-300keV and intermittent downflows of reconnected loops for >4hr. The observations reveal that the two-step flare reconnection substantially contributes to the two-phase CME acceleration, and the impulsive CME acceleration precedes the most intense flare energy release. The implications of this non-standard flare/CME observation are discussed.

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Section: Introductionmentioning

confidence: 99%

Solar Flare–CME Coupling throughout Two Acceleration Phases of a Fast CME

Gou

Veronig

Liu

et al. 2020

ApJL

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“…As a result, the slow solar wind, no more spatially limited to just the HCS, becomes the dominant flow state, filling the heliosphere at high latitudes too [9]. During the highest Sun's activity phase, the solar wind is also largely perturbed by CMEs, which occur up to an order of magnitude more frequently at solar maximum than at minimum e.g., [10]. Such transients can reach such high velocities to accelerate Solar Energetic Particles SEPs, [11].…”

Section: Introductionmentioning

confidence: 99%

Persistence of Ion Cyclotron Waves and Stochasticity of Kinetic Alfvén Waves in the Solar Wind

Telloni

2020

Atmosphere

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This paper investigates the nature of the physical processes underlying the origin of the Ion Cyclotron Waves (ICWs) and Kinetic Alfvén Waves (KAWs) in the solar wind, by studying their Waiting Time Distributions (WTDs). The results show that ICWs and KAWs do not share common statistical properties: while KAWs independently occur as stochastic, uncorrelated wave packets governed by Poisson statistics, ICWs are highly correlated, thus departing from the Poisson hypothesis. The results based on the WTD analysis may cast more light on the mechanisms actively at work in the generation of the two wave modes. Specifically, while the stochastic character of KAWs may be reminiscent of the random convection-driven jostling of the flux-tube foot-points that generates the Alfvén waves in the lower solar atmosphere, the correlations among the ICW events can be effectively explained on the basis of the persistent nature of the mechanism underlying the local origin of ICWs, namely the proton cyclotron instability. Alternative explanations for the observed distribution of ICW waiting times, based on a piecewise-constant Poisson process involving time-varying rates, are also reported.

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“…Void zones for silicate nanodust in the small size limit are identified after the passage of a mature CME impact. This finding would impact the nanodust population locally and during certain times, especially at solar maximum conditions when CMEs are frequent (up to 400 per month Lamy et al, 2019). This variability of the nanodust population might be quantified by impact measurements onboard Parker Solar Probe and Solar Orbiter, taking sputtering and also sublimation into account.…”

Section: Discussionmentioning

confidence: 99%

“…Within our solar system, CME rates vary during a solar cycle. The rate can peak up to 400 per month during high solar activity and can be as low as 10 CMEs per month during solar minimum (Lamy et al, 2019). When assuming a mean value of 100 CMEs per month, the duration a 10 µm particle can survive at 0.1 AU is at least 2.5 years.…”

Section: Sputtering Lifetimesmentioning

confidence: 99%

“…The good performance of the MAGMA model encouraged us to use it in the context of dust sublimation near the Sun as well. The vapour pressure for carbon was used from the literature (Leider et al, 1973;Lide, 2003). Figure 8 (blue lines and left y axis) shows the vapour pressure of all three materials in the temperature range between 500 and 3000 K. The exponential growth of the vapour pressure with temperature is a typical behaviour of all materials.…”

Section: Dust Sublimationmentioning

confidence: 99%

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Dust sputtering within the inner heliosphere: a modelling study

2020

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Abstract. The aim of this study is to investigate through modelling how sputtering by impacting solar wind ions influences the lifetime of dust particles in the inner heliosphere near the Sun. We consider three typical dust materials, silicate, Fe0.4Mg0.6O, and carbon, and describe their sputtering yields based on atomic yields given by the Stopping and Range of Ions in Matter (SRIM) package. The influence of the solar wind is characterized by plasma density, solar wind speed, and solar wind composition, and we assume for these parameter values that are typical for fast solar wind, slow solar wind, and coronal mass ejection (CME) conditions to calculate the sputtering lifetimes of dust. To compare the sputtering lifetimes to typical sublimation lifetimes, we use temperature estimates based on Mie calculations and material vapour pressure derived with the MAGMA chemical equilibrium code. We also compare the sputtering lifetimes to the Poynting–Robertson lifetime and to the collision lifetime. We present a set of sputtering rates and lifetimes that can be used for estimating dust destruction in the fast and slow solar wind and during CME conditions. Our results can be applied to solid particles of a few nanometres and larger. The sputtering lifetimes increase linearly with the size of particles. We show that sputtering rates increase during CME conditions, primarily because of the high number densities of heavy ions in the CME plasma. The shortest sputtering lifetimes we find are for silicate, followed by Fe0.4Mg0.6O and carbon. In a comparison between sputtering and sublimation lifetimes we concentrate on the nanodust population. The comparison shows that sublimation is the faster destruction process within 0.1 AU for Fe0.4Mg0.6O, within 0.05 AU for carbon dust, and within 0.07 AU for silicate dust. The destruction by sputtering can play a role in the vicinity of the Sun. We discuss our findings in the context of recent F-corona intensity measurements onboard Parker Solar Probe.

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Coronal Mass Ejections over Solar Cycles 23 and 24

Cited by 104 publications

References 198 publications

Solar Flare–CME Coupling throughout Two Acceleration Phases of a Fast CME

Solar Flare–CME Coupling throughout Two Acceleration Phases of a Fast CME

Persistence of Ion Cyclotron Waves and Stochasticity of Kinetic Alfvén Waves in the Solar Wind

Dust sputtering within the inner heliosphere: a modelling study

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