Solar Interacting Protons Versus Interplanetary Protons in the Core Plus Halo Model of Diffusive Shock Acceleration and Stochastic Re-Acceleration

Kocharov, L. G.; Laitinen, Timo; Vainio, R.; Afanasiev, Alexandr; Мурсула, К.; Ryan, J. M.

doi:10.1088/0004-637x/806/1/80

Cited by 22 publications

(18 citation statements)

References 56 publications

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“…The authors find that the number of >500 MeV SEP protons is on average about 100 times the number returning to the Sun to produce the sustained -ray emission. This is consistent with what shock wave models estimate (Kocharov et al 2015).…”

Section: :00supporting

confidence: 91%

Solar Particle Radiation Storms Forecasting and Analysis

Malandraki¹,

Crosby²

2018

Astrophysics and Space Science Library

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Section: :00supporting

confidence: 91%

Solar Particle Radiation Storms Forecasting and Analysis

Malandraki¹,

Crosby²

2018

Astrophysics and Space Science Library

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“…The SEP transit through the shock may be possible via fast transport channels/quiet magnetic tubes penetrating the shock (similar to model by Kocharov et al 2014). Such channels could also provide a way for the back precipitation of the shock-accelerated particles to the Sun to produce there, via nuclear interactions, a variety of secondary emissions (Kocharov et al 2015b).…”

Section: Discussionmentioning

confidence: 96%

Interplanetary Protons versus Interacting Protons in the 2017 September 10 Solar Eruptive Event

Kocharov

Pesce-Rollins

Laitinen

et al. 2020

ApJ

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We analyze the relativistic proton emission from the Sun during the eruptive event on 2017 September 10, which caused a ground-level enhancement (GLE 72) registered by the worldwide network of neutron monitors. Using the neutron monitor data and interplanetary transport modeling both along and across interplanetary magnetic field (IMF) lines, we deduce parameters of the proton injection into the interplanetary medium. The inferred injection profile of the interplanetary protons is compared with the profile of the >100 MeV γ-ray emission observed by the Fermi Large Area Telescope, attributed to pion production from the interaction of >300 MeV protons at the Sun. GLE 72 started with a prompt component that arrived along the IMF lines. This was followed by a more prolonged enhancement caused by protons arriving at the Earth across the IMF lines from the southwest. The interplanetary proton event is modeled using two sources-one source at the root of the Earth-connected IMF line and another source situated near the solar western limb. The maximum phase of the second injection of interplanetary protons coincides with the maximum phase of the prolonged >100 MeV γ-ray emission that originated from a small area at the solar western limb, below the current sheet trailing the associated coronal mass ejection (CME). A possible common source of interacting protons and interplanetary protons is discussed in terms of proton acceleration at the CME bow shock versus coronal (re-)acceleration in the wake of the CME.

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“…For instance, a shock can produce different energy spectra and time profiles depending on the environment met, which may include different magnetic structures, plasma turbulence and seed particle populations [3,4]. Possible scenario is illustrated with Figure 2.…”

Section: Discussionmentioning

confidence: 99%

Resolving multiple sources of solar relativistic particles

Kocharov¹,

Klassen²,

Usoskin³

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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We consider the time-profile morphology of solar high-energy particle emissions, including relativistic electrons in three energy channels of SOHO/EPHIN, relativistic protons as registered by the worldwide network of neutron monitors, and ∼ 100 MeV/n protons and helium in several energy channels of SOHO/ERNE. Based on numerical modeling of the interplanetary transport, we formulate a simple method for investigation of the high-energy particle sources operating at / near the Sun during the first hour of particle event. The method is applied to Ground Level Enhancement (GLE) and Solar Energetic Particle (SEP) events of the solar cycle 23. We conclude that depending on the GLE-SEP event scenario and detector vantage point, the observed particles originate from at least three sources. Possible nature of the sources is discussed in the framework of previous and new models of the high-energy particle production associated with global coronal (EIT) waves and CME shocks within about five solar radii from the Sun. PoS(ICRC2015)057GLE origins Leon Kocharov Method and resultsWe start with modeling of the SEP transport from a source near the Sun to a detector at 1 AU. Interplanetary propagation of high-energy particles is modeled in the framework of focused transport [1] for the Kolmogorov turbulence spectrum in the standard solar wind. The energy dependence of the proton mean free path is according to the standard quasi-linear theory, while the mean free path of ≈ 1 MeV electrons is equal to that of the 1 MeV protons [2]. For analysis of real events, we simulate particle transport and registration with actual energy spectra, energy channels, aperture and viewing direction of a particular instrument. At large values of the mean free path, λ 3 AU, the particle source profile may be estimated by a proper shifting of the instrument's counting rate profile back in time. The mean free path value is estimated using the flux anisotropy measurements.Based on the results of particle transport and registration modeling, we shift the observed time-intensity profiles in time back to the Sun but add eight minutes to facilitate a comparison with electromagnetic emissions observed at 1 AU: t S = t − ∆t + 8 min. The time-shifted and renormalised profiles of the 13 December 2006 event (GLE 70) are shown in Figure 1. Plotted only the neutron monitor profile revealing the earliest and steepest onset in this GLE. For a convenience of comparison of different particle species and energy channels, the background levels are reduced to one and the same level that is 1% of the real neutron monitor background.

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Solar Interacting Protons Versus Interplanetary Protons in the Core Plus Halo Model of Diffusive Shock Acceleration and Stochastic Re-Acceleration

Cited by 22 publications

References 56 publications

Solar Particle Radiation Storms Forecasting and Analysis

Solar Particle Radiation Storms Forecasting and Analysis

Interplanetary Protons versus Interacting Protons in the 2017 September 10 Solar Eruptive Event

Resolving multiple sources of solar relativistic particles

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