Relativistic Solar Protons on 1989 October 22: Injection and Transport along Both Legs of a Closed Interplanetary Magnetic Loop

Ruffolo, D.; Tooprakai, P.; Rujiwarodom, M.; Khumlumlert, T.; Wechakama, Maneenate; Bieber, J. W.; Evenson, P. A.; Pyle, R.

doi:10.1086/499419

Cited by 56 publications

(60 citation statements)

References 66 publications

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“…Magnetic mirroring, as evidenced by bidirectional flow of relativistic particles following intense solar activity, has been previously reported by Cramp et al (1997a) and Bieber et al (2002) and bidirectional flow in a closed interplanetary magnetic loop has been reported by Ruffolo et al (2006).…”

Section: State Of the Interplanetary Medium: Gle 69mentioning

confidence: 67%

An Improved Model for Relativistic Solar Proton Acceleration Applied to the 2005 January 20 and Earlier Events

Bombardieri

Duldig

Humble

et al. 2008

ApJ

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This paper presents results on modeling the ground-level response of the higher energy protons for the 2005 January 20 ground-level enhancement (GLE). This event, known as GLE 69, produced the highest intensity of relativistic solar particles since the famous event on 1956 February 23. The location of recent X-ray and -ray emission (N14 W61 ) was near Sun-Earth connecting magnetic field lines, thus providing the opportunity to directly observe the acceleration source from Earth. We restrict our analysis to protons of energy !450 MeV to avoid complications arising from transport processes that can affect the propagation of low-energy protons.

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Section: State Of the Interplanetary Medium: Gle 69mentioning

confidence: 67%

An Improved Model for Relativistic Solar Proton Acceleration Applied to the 2005 January 20 and Earlier Events

Bombardieri

Duldig

Humble

et al. 2008

ApJ

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“…Some solar particle events were observed inside magnetic clouds of previous CMEs, and the particle transport was correspondingly modeled in a kind of interplanetary magnetic loop (Kocharov et al 2005;Ruffolo et al 2006). However, for the 2003 November 2 event, an interplanetary magnetic cloud has not been identified with in situ plasma data, even though the solar wind was strongly distorted by previous solar eruptions (Appendix A).…”

Section: Interplanetary Transport Modelingmentioning

confidence: 99%

Investigating the Origins of Two Extreme Solar Particle Events: Proton Source Profile and Associated Electromagnetic Emissions

Kocharov

Pohjolainen

Mishev

et al. 2017

ApJ

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We analyze the high-energy particle emission from the Sun in two extreme solar particle eventsin which protons are accelerated to relativistic energies and can cause a significant signal even in the ground-based particle detectors. Analysis of a relativistic proton event is based on modeling of the particle transport and interaction, from a nearSun source through the solar wind and the Earth's magnetosphere and atmosphere to a detector on the ground. This allows us to deduce the time profile of the proton source at the Sun and compare it with observed electromagnetic emissions. The 1998 May 2 event is associated with aflare and a coronal mass ejection (CME), which were well observed by the Nançay Radioheliograph, thusthe images of theradio sources are available. For the 2003 November 2 event, the low corona images of the CME liftoff obtained at the Mauna Loa Solar Observatoryare available. Those complementary data sets are analyzed jointly with the broadband dynamic radio spectra, EUV images, and other data available for both events. We find a common scenario for both eruptions, including the flare's dual impulsive phase, the CME-launch-associated decimetric-continuum burst, and the late, low-frequency type III radio bursts at the time of the relativistic proton injection into the interplanetary medium. The analysis supports the idea that the two considered events start with emission of relativistic protons previously accelerated during the flare and CME launch, then trapped in large-scale magnetic loops and later released by the expanding CME.

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“…To our knowledge a double-injection scenario could never be proven unambiguously, although it was often presumed (e.g., Richardson & Cane 1996;Leske et al 2012). Only modeling results of neutron monitor measurements of the 22 October 1989 event by Ruffolo et al (2006) strongly suggested such a scenario.…”

Section: Introductionmentioning

confidence: 90%

Injection of solar energetic particles into both loop legs of a magnetic cloud

Dresing

Gómez-Herrero

Heber

et al. 2016

A&A

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Context. Each of the two Solar TErrestrial RElations Observatory (STEREO) spacecraft carries a Solar Electron and Proton Telescope (SEPT) which measures electrons and protons. Anisotropy observations are provided in four viewing directions: along the nominal magnetic field Parker spiral in the ecliptic towards the Sun (SUN) and away from the Sun (Anti-Sun/ASUN), and towards the north (NORTH) and south (SOUTH). The solar energetic particle (SEP) event on 7 November 2013 was observed by both STEREO spacecraft, which were longitudinally separated by 68• at that time. While STEREO A observed the expected characteristics of an SEP event at a well-connected position, STEREO B detected a very anisotropic bi-directional distribution of near-relativistic electrons and was situated inside a magnetic-cloud-like structure during the early phase of the event. Aims. We examine the source of the bi-directional SEP distribution at STEREO B. On the one hand this distribution could be caused by a double injection into both loop legs of the magnetic cloud (MC). On the other hand, a mirroring scenario where the incident beam is reflected in the opposite loop leg could be the reason. Furthermore, the energetic electron observations are used to probe the magnetic structure inside the magnetic cloud. Methods. We investigate in situ plasma and magnetic field observations and show that STEREO B was embedded in an MC-like structure ejected three days earlier on 4 November from the same active region. We apply a Graduated Cylindrical Shell (GCS) model to the coronagraph observations from three viewpoints as well as the Global Magnetic Cloud (GMC) model to the in situ measurements at STEREO B to determine the orientation and topology of the MC close to the Sun and at 1 AU. We also estimate the path lengths of the electrons propagating through the MC to estimate the amount of magnetic field line winding inside the structure. Results. The relative intensity and timing of the energetic electron increases in the different SEPT telescopes at STEREO B strongly suggest that the bi-directional electron distribution is formed by SEP injections in both loop legs of the MC separately instead of by mirroring farther away beyond the STEREO orbit. Observations by the Nançay Radioheliograph (NRH) of two distinct radio sources during the SEP injection further support the above scenario. The determined electron path lengths are around 50% longer than the estimated lengths of the loop legs of the MC itself (based on the GCS model) suggesting that the amount of field line winding is moderate.

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Relativistic Solar Protons on 1989 October 22: Injection and Transport along Both Legs of a Closed Interplanetary Magnetic Loop

Cited by 56 publications

References 66 publications

An Improved Model for Relativistic Solar Proton Acceleration Applied to the 2005 January 20 and Earlier Events

An Improved Model for Relativistic Solar Proton Acceleration Applied to the 2005 January 20 and Earlier Events

Investigating the Origins of Two Extreme Solar Particle Events: Proton Source Profile and Associated Electromagnetic Emissions

Injection of solar energetic particles into both loop legs of a magnetic cloud

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