Extreme Solar Events: Setting up a Paradigm

Usoskin, Ilya; Miyake, Fusa; Baroni, Melanie; Brehm, Nicolas; Dalla, Silvia; Hayakawa, Hisashi; Hudson, Hugh; Jull, A. J. Timothy; Knipp, Delores; Koldobskiy, Sergey; Maehara, Hiroyuki; Mekhaldi, Florian; Notsu, Yuta; Poluianov, Stepan; Rozanov, Eugene; Shapiro, Alexander; Spiegl, Tobias; Sukhodolov, Timofei; Uusitalo, Joonas; Wacker, Lukas

doi:10.1007/s11214-023-01018-1

Cited by 7 publications

(3 citation statements)

References 501 publications

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“…[69]) in the lunar environment allows us to assess its impact on the dynamics of the Earth's and the Moon's exospheres, on the dynamics of the Earth's magnetosphere, and on the sputtering, electrostatic charging and weathering of the Moon's surface. This can become of paramount importance during severe space weather events, when the solar wind and SEP parameters can take extreme values [70][71][72][73].…”

Section: Energetic Particle Environment Of the Moonmentioning

confidence: 99%

High-energy particle observations from the Moon

Dandouras,

Roussos

2024

Phil. Trans. R. Soc. A.

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The Moon is a unique natural laboratory for the study of the deep space plasma and energetic particles environment. During more than 3/4 of its orbit around the Earth it is exposed to the solar wind. Being an unmagnetized body and lacking a substantial atmosphere, solar wind and solar energetic particles bombard the Moon's surface, interacting with the lunar regolith and the tenuous lunar exosphere. Energetic particles arriving at the Moon's surface can be absorbed, or scattered, or can remove another particle from the lunar regolith by sputtering or desorption. A similar phenomenon occurs also with the galactic cosmic rays, which have fluxes and energy spectra representative of interplanetary space. During the remaining part of its orbit the Moon crosses the tail of the terrestrial magnetosphere. It then provides the opportunity to study in-situ the terrestrial magnetotail plasma environment as well as atmospheric escape from the Earth's ionosphere, in the form of heavy ions accelerated and streaming downtail. The lunar environment is thus a unique natural laboratory for analysing the interaction of the solar wind, the cosmic rays and the Earth's magnetosphere with the surface, the immediate subsurface, and the surface-bounded exosphere of an unmagnetized planetary body. This article is part of a discussion meeting issue ‘Astronomy from the Moon: the next decades (part 2)’.

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Section: Energetic Particle Environment Of the Moonmentioning

confidence: 99%

High-energy particle observations from the Moon

Dandouras,

Roussos

2024

Phil. Trans. R. Soc. A.

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“…Contrary to 10 Be, 36 Cl production has a production channel from low-energy particles. More details about extreme solar events are provided in the recent review by Usoskin et al (2023).…”

Section: Introductionmentioning

confidence: 99%

The Role of Deposition of Cosmogenic ¹⁰Be for the Detectability of Solar Proton Events

Schaar,

Spiegl,

Langematz

et al. 2024

JGR Atmospheres

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The manifestation of extreme solar proton events (SPEs) in Beryllium‐10 (10Be) ice core data contains valuable information about the strength and incidence of SPEs or local characteristics of the atmosphere. To extract this information, the signals of enhanced production of cosmogenic 10Be due to the SPEs have to be detected, hence distinguished from the variability of the background production by galactic cosmic rays (GCRs). Here, we study the transport and deposition of 10Be from GCRs, using the ECHAM/MESSy Atmospheric Chemistry climate model, and discuss the detectability of extreme SPEs (similar to the CE 774/775 SPE) in 10Be ice core data depending on the ice core location, seasonal appearance of the SPE, atmospheric aerosol size distribution and phase of the 11‐year solar cycle. We find that sedimentation can be a major deposition mechanism of GCR generated 10Be, especially at high latitudes, depending on the aerosols to which 10Be attaches after production. The comparison of our results to four ice core records of 10Be from Greenland and Antarctica shows good agreement for both 10Be from GCRs and solar energetic particles (SEP). From our results we deduce that the location of detection and the season of occurrence of the SPE have a considerable effect on its detectability, as well as the aerosol size distribution the produced cosmogenic nuclides meet in the atmosphere. Furthermore, we find that SPEs occurring in the phase of highest activity during the 11‐year solar cycle are more detectable than SPEs that arise in the phase of lowest activity.

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“…These events have had peak fluxes that are one or two orders of magnitude higher than either the August 1972 or the March 1989 event (Koldobskiy et al, 2023). See Usoskin et al (2023) for an excellent review. Can further knowledge about the two space-age SEP events (August 1972 and tell us more about what might have caused these more ancient possibly interplanetary particle events?…”

Section: Introductionmentioning

confidence: 99%

Review of the August 1972 and March 1989 (Allen) Space Weather Events: Can We Learn Anything New From Them?

Tsurutani,

Sen,

Hajra

et al. 2024

JGR Space Physics

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Updated summaries of the August 1972 and March 1989 space weather events have been constructed. The features of these two events are compared to the Carrington 1859 event and a few other major space weather events. It is concluded that solar active regions release energy in a variety of forms (X‐rays, EUV photons, visible light, coronal mass ejection (CME) plasmas and fields) and they in turn can produce other energetic effects (solar energetic particles (SEPs), magnetic storms) in a variety of ways. It is clear that there is no strong one‐to‐one relationship between these various energy sinks. The energy is often distributed differently from one space weather event to the next. Concerning SEPs accelerated at interplanetary CME (ICME) shocks, it is concluded that the Fermi mechanism associated with quasi‐parallel shocks is relatively weak and that the gradient drift mechanism (electric fields) at quasi‐perpendicular shocks will produce harder spectra and higher fluxes. If the 4 August 1972 intrinsic magnetic cloud condition (southward interplanetary magnetic field instead of northward) and the interplanetary Sun to 1 au conditions were different, a 4 August 1972 magnetic storm and magnetospheric dawn‐to‐dusk electric fields substantially larger than the Carrington event would have occurred. Under these special interplanetary conditions, a Miyake et al. (2012), https://doi.org/10.1038/nature11123‐like extreme SEP event may have been formed. The long duration complex 1989 storm was probably greater than the Carrington storm in the sense that the total ring current particle energy was larger.

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Extreme Solar Events: Setting up a Paradigm

Cited by 7 publications

References 501 publications

High-energy particle observations from the Moon

High-energy particle observations from the Moon

The Role of Deposition of Cosmogenic ¹⁰Be for the Detectability of Solar Proton Events

Review of the August 1972 and March 1989 (Allen) Space Weather Events: Can We Learn Anything New From Them?

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Extreme Solar Events: Setting up a Paradigm

Cited by 7 publications

References 501 publications

High-energy particle observations from the Moon

High-energy particle observations from the Moon

The Role of Deposition of Cosmogenic 10Be for the Detectability of Solar Proton Events

Review of the August 1972 and March 1989 (Allen) Space Weather Events: Can We Learn Anything New From Them?

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The Role of Deposition of Cosmogenic ¹⁰Be for the Detectability of Solar Proton Events