Coronal Jets, Magnetic Topologies, and the Production of Interplanetary Electron Streams

Li, C.; Matthews, Sarah; Driel-Gesztelyi, L. van; Sun, Jian; Owen, C. J.

doi:10.1088/0004-637x/735/1/43

Cited by 8 publications

(7 citation statements)

References 27 publications

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“…In present study, the power-law index of WTD of SEEs is 0.99 for short waiting times, that is much harder than the WTD of flares. The reason probably arises from the fact that SEEs are not only flare-related, but many of them appear to be associated with narrow CMEs, coronal jets, or energy releases in high coronal sites (Kahler et al 2001;Klein et al 2001;Pick et al 2006;Li et al 2011;Wang et al 2012). The power-law index of WTD of SEEs is 1.92 for long waiting times, taking into account the possible modulation of CIRs, that is comparable to the WTDs of flares and SPEs.…”

Section: Summary and Discussionmentioning

confidence: 99%

Waiting Time Distribution of Solar Energetic Particle Events Modeled With a Non-Stationary Poisson Process

Zhong

Wang

et al. 2014

ApJ

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We present a study of the waiting time distributions (WTDs) of solar energetic particle (SEP) events observed with the spacecraft W IND and GOES. Both the WTDs of solar electron events (SEEs) and solar proton events (SPEs) display a power-law tail ∼ ∆t −γ . The SEEs display a broken power-law WTD. The powerlaw index is γ 1 = 0.99 for the short waiting times (<70 hours) and γ 2 = 1.92 for large waiting times (>100 hours). The break of the WTD of SEEs is probably due to the modulation of the corotating interaction regions (CIRs). The power-law index γ ∼ 1.82 is derived for the WTD of SPEs that is consistent with the WTD of type II radio bursts, indicating a close relationship between the shock wave and the production of energetic protons. The WTDs of SEP events can be modeled with a non-stationary Poisson process which was proposed to understand the waiting time statistics of solar flares (Wheatland 2000;Aschwanden & McTiernan 2010). We generalize the method and find that, if the SEP event rate λ = 1/∆t varies as the time distribution of event rate f (λ) = Aλ −α exp(−βλ), the timedependent Poisson distribution can produce a power-law tail WTD ∼ ∆t α−3 , where 0 ≤ α < 2.

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Section: Summary and Discussionmentioning

confidence: 99%

Waiting Time Distribution of Solar Energetic Particle Events Modeled With a Non-Stationary Poisson Process

Zhong

Wang

et al. 2014

ApJ

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“…In radio observations, type III bursts are produced by electrons streaming along open field lines extending to interplanetary space. Many studies have indicated that type III radio bursts and SEP events are spatially and temporally associated with solar jets [69,[257][258][259][260][261][262]. Wang et al [263] investigated 25 3 He-rich events and found that their sources lie close to coronal holes and are characterized by jet-like ejections along Earth-directed open field lines.…”

Section: (E) Particle Accelerationmentioning

confidence: 99%

Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

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The solar atmosphere is full of complicated transients manifesting the reconfiguration of the solar magnetic field and plasma. Solar jets represent collimated, beam-like plasma ejections; they are ubiquitous in the solar atmosphere and important for our understanding of solar activities at different scales, the magnetic reconnection process, particle acceleration, coronal heating, solar wind acceleration, as well as other related phenomena. Recent high-spatio-temporal-resolution, wide-temperature coverage and spectroscopic and stereoscopic observations taken by ground-based and space-borne solar telescopes have revealed many valuable new clues to restrict the development of theoretical models. This review aims at providing the reader with the main observational characteristics of solar jets, physical interpretations and models, as well as unsolved outstanding questions in future studies.

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“…By applying the same model, a statistical link between the coronal magnetic topologies and dynamics of in-situ electrons was recently established (Li et al 2010). For individual SEP event, a more practical and accurate method to construct coronal magnetic fields is absolutely necessary (Li et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Electron and Proton Acceleration During the First Ground Level Enhancement Event of Solar Cycle 24

Firoz

Sun

et al. 2013

ApJ

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High-energy particles were recorded by the near-Earth spacecraft and groundbased neutron monitors (NMs) on 2012 May 17. This event was the first Ground Level Enhancement (GLE) of the solar cycle 24. In present study, we try to identify the acceleration source(s) of solar energetic particles (SEPs) by combining in-situ particle measurements from W IND/3DP, GOES 13, and solar cosmic rays (SCRs) registered by several NMs, as well as the remote-sensing solar observations from SDO/AIA, SOHO/LASCO, and RHESSI. We derive the interplanetary magnetic field (IMF) path length (1.25 ± 0.05 AU) and solar particle release (SPR) time (01:29 ± 00:01 UT) of the first arriving electrons by using their velocity dispersion and taking into account the contamination effects. It is found that the electron impulsive injection phase, indicated by the dramatic change of spectral index, is consistent with the flare non-thermal emission and type III radio bursts. Based on the potential field source surface (PFSS) concept, a modeling of the open-field lines rooted in the active region (AR) has been performed to provide escaping channels for flare-accelerated electrons. Meanwhile, relativistic protons are found to be released ∼10 min later than the electrons, assuming their scatter-free travel along the same IMF path length. Combining multi-wavelength imaging data on the prominence eruption and coronal mass ejection (CME), we obtain some evidence of that GLE protons, with estimated kinetic energy of ∼1.12 GeV, are probably accelerated by the CME-driven shock when it travels to ∼3.07 solar radii. The time-of-maximum (TOM) spectrum of protons is typical for the shock wave acceleration.

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Coronal Jets, Magnetic Topologies, and the Production of Interplanetary Electron Streams

Cited by 8 publications

References 27 publications

Waiting Time Distribution of Solar Energetic Particle Events Modeled With a Non-Stationary Poisson Process

Waiting Time Distribution of Solar Energetic Particle Events Modeled With a Non-Stationary Poisson Process

Observation and modelling of solar jets

Electron and Proton Acceleration During the First Ground Level Enhancement Event of Solar Cycle 24

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