Astrophysical Aspects in the Studies of Solar Cosmic Rays

Miroshnichenko, L. I.; Pérez‐Peraza, J.

doi:10.1142/s0217751x08037312

Cited by 64 publications

(45 citation statements)

References 196 publications

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“…Substantial summaries of flares observations related to the RHESSI X-ray mission may be found in Emslie et al (2011), a short general review in Aschwanden (2002). Reviews in more specialized fields have been published by Bastian et al (1998), Nindos et al (2008), and Pick and Vilmer (2008) on radio emissions, Fletcher and Warren (2003) on ultraviolet emissions, Ryan et al (2000), Schwenn (2006), and Miroshnichenko and Perez-Peraza (2008) on flare effects and energetic flare particles in interplanetary space. Somov (1992), Shibata andMagara (2011), andForbes (2000) have reviewed theory.…”

Section: Organization Of Reviewmentioning

confidence: 99%

Flare Observations

Benz

2016

Living Rev Sol Phys

491

317

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Solar flares are observed at all wavelengths from decameter radio waves to gamma-rays beyond 1 GeV. This review focuses on recent observations in EUV, soft and hard X-rays, white light, and radio waves. Space missions such as RHESSI, Yohkoh, TRACE, SOHO, and more recently Hinode and SDO have enlarged widely the observational base. They have revealed a number of surprises: Coronal sources appear before the hard X-ray emission in chromospheric footpoints, major flare acceleration sites appear to be independent of coronal mass ejections, electrons, and ions may be accelerated at different sites, there are at least 3 different magnetic topologies, and basic characteristics vary from small to large flares. Recent progress also includes improved insights into the flare energy partition, on the location(s) of energy release, tests of energy release scenarios and particle acceleration. The interplay of observations with theory is important to deduce the geometry and to disentangle the various processes involved. There is increasing evidence supporting magnetic reconThis article is a revised version of https://doi.org/10.12942/lrsp-2008-1. Change summary Major revision, updated and expanded. Change details Significant new results from RHESSI and SDO are included. In particular, Sect. 3.4 on "Emissions from above the coronal source" was added (including two new figures) and Sect. 3.2 on "Coronal hard X-ray sources" was expanded. New observations of flares in white light are reported (replaced Fig. 25 with a movie), as well as recent multi-wavelength observations in radio waves and gamma-rays combined with hard X-rays. Four references were removed and 49 new references added. Arnold O. Benz nection as the basic cause. While this process has become generally accepted as the trigger, it is still controversial how it converts a considerable fraction of the energy into non-thermal particles. Flare-like processes may be responsible for large-scale restructuring of the magnetic field in the corona as well as for its heating. Large flares influence interplanetary space and substantially affect the Earth's ionosphere. Flare scenarios have slowly converged over the past decades, but every new observation still reveals major unexpected results, demonstrating that solar flares, after 150 years since their discovery, remain a complex problem of astrophysics including major unsolved questions. Electronic supplementary material

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Section: Organization Of Reviewmentioning

confidence: 99%

Flare Observations

Benz

2016

Living Rev Sol Phys

491

317

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“…Furthermore, they may help to evaluate the solar capability to produce high energy protons. In particular, these results may help to refine the upper limit spectrum for protons (Miroshnichenko 1996;Miroshnichenko and Pérez-Peraza 2008). Also, a more accurate knowledge of GLE spectra could lead to find a relationship with the solar cycle.…”

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confidence: 86%

“…To validate our claimed detection of a GLE signal on event 54, we also analyzed pressure corrected five minute count rates of Calgary, Deep River, Goose Bay, Hermanus, Inuvik, LARC, Lomnicky Stit, Oulu, Potchefstroom, SANAE and Tsumeb neutron monitors, as suggested by the Australian Antarctic Data Center (http://data.aad.gov.au/aadc/gle/); all these data were downloaded from the FTP site of IZMIRAN (ftp://cr0.izmiran.rssi.ru/). Dates and onset times of the events were taken from Miroshnichenko & Pérez-Peraza (2008), and Shea et al (1995). We used the baseline intervals suggested by the Bartol Research Institute (http://neutronm.bartol.udel.edu/).…”

Section: Data and Qualitative Analysismentioning

confidence: 99%

“…The instrument's mean counting rate of 76,470 counts/hour = 6,373 counts/5 min with a corresponding standard deviation of 0.88% are an additional validation of the statistical results presented in this work. We calculate that under such disturbed geomagnetic conditions, the cutoff rigidity of the Mexico City site got lowered to a value of 7.5 GV; likewise, we have computed the median response energy of the instrument for the combined galactic and solar spectrum, using the upper limit spectum for protons (Miroshnichenko & Pérez-Peraza 2008) and got a value of 10.7 GV. Thus, we can infer that the Sun emitted particles with energies of at least 7.5 and most probably 10.7 GeV during the X9.0 flare that occurred on November 2, 1992.…”

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confidence: 99%

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Search for solar energetic particle signals in the Mexico City neutron monitor database

Vargas-Cárdenas¹,

Galicia²

2011

Proc. IAU

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Abstract. We performed a search for ground level solar cosmic ray enhancements on the full five minute database of the Mexico City neutron monitor using wavelet filters and two different statistical tests. We present a detailed analysis of the time series of November 2, 1992, where we found a previously unreported increment matching the onset time of the impulsive phase of the Ground Level Enhancement No. 54, thus providing evidence of an effective detection of high energy solar cosmic rays. This technique may help to find still undiscovered GLE signals in the Worldwide Neutron Monitor Database, to refine GLE spectra and, probably, to find a relationship between the latter and the solar cycle.

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“…The importance to study the energy spectra of solar proton events is useful for identification the origins of the particles and for estimations the possible maxi mum energies and fluxes (Getselev et al, 2004;Belov et al, 1995;Miroshnichenko, 1996;Miroshnichenko et al, 2001Miroshnichenko et al, , 2008. Currently, researchers are trying to establish if there is a possibility of proton events fore cast in order to have enough time to pursue practical goals, such as warning of radiation dangers in near Earth and interplanetary space (Mavromikhalaki et al, 2009;Laurenza et al, 2009;Kane, 2011).…”

Section: Introductionmentioning

confidence: 99%

Dynamics of the energy spectra of solar proton events observed in solar cycle 23

2012

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The proton energy spectra I(E, t) as functions of time were obtained and analyzed in the energy range of a few tens of MeV on the basis of GOES observations of proton enhancements during solar cycle 23. The energy spectra were approximated by power law functions. We found a wide variety of functions I(E, t) for studied events. The spectra cannot be described by a universal function of time, although three groups of proton events seem to have some common features. This allows us to outline an approach to their empirical classification in future using a number of dimensionless scaling parameters. The regularities we observe may be partly due to the dynamical processes occurring on the Sun, in the heliosphere, and magnetosphere.

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Astrophysical Aspects in the Studies of Solar Cosmic Rays

Cited by 64 publications

References 196 publications

Flare Observations

Flare Observations

Search for solar energetic particle signals in the Mexico City neutron monitor database

Dynamics of the energy spectra of solar proton events observed in solar cycle 23

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