Fluxes and nuclear abundances of cosmic rays inside the magnetosphere using a transmission function approach

Bobík, P.; Boella, G.; Boschini, M.; Gervasi, M.; Grandi, D.; Kudela, K.; Pensotti, S.; Rancoita, P.G.

doi:10.1016/j.asr.2008.11.020

Cited by 4 publications

(1 citation statement)

References 28 publications

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“…Allowed and forbidden rigidity: penumbra. A better description of the transmission function is the use of a sigmoid function, as done in the context of NMs (Kudela et al, 2008), or the CR experiments HEAO-3 (Ferrando et al, 1988) and AMS-01 (Bobik et al, 2006(Bobik et al, , 2009). The step function H(R − R eff c ) is the limit of a sigmoid of zero width.…”

Section: Uncertainties From Transmission Function Tmentioning

confidence: 99%

Neutron monitors and muon detectors for solar modulation studies: Interstellar flux, yield function, and assessment of critical parameters in count rate calculations

Maurin

Cheminet

Derome

et al. 2015

Advances in Space Research

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Particles count rates at given Earth location and altitude result from the convolution of (i) the interstellar (IS) cosmic-ray fluxes outside the solar cavity, (ii) the time-dependent modulation of IS into Top-of-Atmosphere (TOA) fluxes, (iii) the rigidity cut-off (or geomagnetic transmission function) and grammage at the counter location, (iv) the atmosphere response to incoming TOA cosmic rays (shower development), and (v) the counter response to the various particles/energies in the shower. Count rates from neutron monitors or muon counters are therefore a proxy to solar activity. In this paper, we review all ingredients, discuss how their uncertainties impact count rate calculations, and how they translate into variation/uncertainties on the level of solar modulation φ (in the simple Force-Field approximation). The main uncertainty for neutron monitors is related to the yield function. However, many other effects have a significant impact, at the 5 − 10% level on φ values. We find no clear ranking of the dominant effects, as some depend on the station position and/or the weather and/or the season. An abacus to translate any variation of count rates (for neutron and µ detectors) to a variation of the solar modulation φ is provided.

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Section: Uncertainties From Transmission Function Tmentioning

confidence: 99%

Neutron monitors and muon detectors for solar modulation studies: Interstellar flux, yield function, and assessment of critical parameters in count rate calculations

Maurin

Cheminet

Derome

et al. 2015

Advances in Space Research

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Distribution of secondary particles intensities over Earth’s surface: Effect of the geomagnetic field

Bobík

Kudela

Pastirčák

et al. 2012

Advances in Space Research

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We use a Corsika package (Heck et al., 1998) and an AMS-01 flight data (Alcaraz et al., 2000) to evaluate a distribution of secondary particles in the Earth atmosphere. Distribution covers all longitudes and latitudes of STS-91 Space Shuttle flight trajectory to Mir Space Station. Moreover distribution covers all depth in the atmosphere in evaluated area. We show distributions for e-, e+, μ+, μ-, gammas, hadrons and Cherenkov light from primary protons component of cosmic rays flux. Our results compare favorably with other estimates made by different techniques. We also estimate a UV light production (300-400 nm) by electron component of secondaries at the top of the atmosphere and at ISS orbit. IntroductionCosmic Ray (CR hereafter) particles come to the vicinity of Earth from outer space. The flux of these particles is isotropic outside Earth's magnetosphere; inside the magnetosphere the flux is affected by the strength of the geomagnetic field. The influence of the geomagnetic field is such that the flux of galactic cosmic ray at the top of the atmosphere is not constant being the highest in the polar regions and lowest in the equatorial regions. The most precise measurement of this distribution to date has been provided from an analysis of the AMS-01 data (Alcaraz et al. 2000) who published the intensities for primary and secondary protons at low orbit for ten geomagnetic regions.

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A quantitative study on the effects of external geomagnetic fields by using the GeoMagSphere back-tracing code

Boschini¹,

Torre²,

Gervasi

et al. 2021

Advances in Space Research

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Fluxes and nuclear abundances of cosmic rays inside the magnetosphere using a transmission function approach

Cited by 4 publications

References 28 publications

Neutron monitors and muon detectors for solar modulation studies: Interstellar flux, yield function, and assessment of critical parameters in count rate calculations

Neutron monitors and muon detectors for solar modulation studies: Interstellar flux, yield function, and assessment of critical parameters in count rate calculations

Distribution of secondary particles intensities over Earth’s surface: Effect of the geomagnetic field

A quantitative study on the effects of external geomagnetic fields by using the GeoMagSphere back-tracing code

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