Bare Neutron Counter and Neutron Monitor Response to Cosmic Rays During a 1995 Latitude Survey

Nuntiyakul, Waraporn; Sáiz, A.; Ruffolo, D.; Mangeard, P.-S.; Evenson, P. A.; Bieber, J. W.; Clem, J.; Pyle, R.; Duldig, M. L.; Humble, J. E.

doi:10.1029/2017ja025135

Cited by 31 publications

(38 citation statements)

References 31 publications

(49 reference statements)

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“…The result for sea level is nearly identical to that of Mishev et al (). The computed YF is consistent with the results of NM latitude surveys, specifically in the low‐energy range (Nuntiyakul et al, ).…”

Section: Nm Yield Functionsupporting

confidence: 86%

Updated Neutron‐Monitor Yield Function: Bridging Between In Situ and Ground‐Based Cosmic Ray Measurements

Mishev

Koldobskiy

Kovaltsov³

et al. 2020

JGR Space Physics

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An updated yield function for a standard NM64 neutron monitor (NM) is computed and extended to different atmospheric depths from sea level to 500 g/cm 2 ( ∼5.7 km altitude) and is presented as lookup tables and a full parametrization. The yield function was validated using the cosmic ray spectra directly measured in space by the AMS‐02 experiment during the period May 2011 through May 2017 and confronted with count rates of all NM64‐type NMs being in operation during this period. Using this approach, stability of all the selected NMs was analyzed for the period 2011–2017. Most of NMs appear very stable and suitable for studies of long‐term solar modulation of cosmic rays. However, some NMs suffer from instabilities like trends, apparent jumps, or strong seasonal waves in the count rates.

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Section: Nm Yield Functionsupporting

confidence: 86%

Updated Neutron‐Monitor Yield Function: Bridging Between In Situ and Ground‐Based Cosmic Ray Measurements

Mishev

Koldobskiy

Kovaltsov³

et al. 2020

JGR Space Physics

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“…As in our previous bare neutron detector survey (Nuntiyakul et al, ) and in the 1996 survey (Villoresi et al, ), the detectors showed major increases of the count rate ratio of the bare neutron detectors to the neutron monitor whenever the ship was in port. We removed those time periods from our analysis and also removed time periods with a clear effect of proximity to land near Göteborg Sweden, in the estuary of the river Plate in Uruguay and in the Magellan Strait.…”

Section: Datasupporting

confidence: 74%

“…Nuntiyakul et al () showed that for fixed stations the coefficient for bare neutron detectors and neutron monitors is typically slightly different but did not find a consistent pattern as a function of cutoff. Attempts to derive a bare neutron detector coefficient for that survey produced results that, within large statistical errors, were indistinguishable from the NM64 result.…”

Section: Datamentioning

confidence: 99%

“…From 1977 to 2005, BP‐28 (BF 3 ) detectors were operated nearby as bare neutron counters. The YFs of the bare neutron detectors and NM64 have a different energy dependence so the counting rate ratio changes in response to changes in the primary spectrum (Nuntiyakul et al, ; Potgieter et al, ; Stoker, ). In particular, we have made extensive use of this to estimate the spectral index and intensity of solar energetic particles (Bieber & Evenson, ; Bieber et al, ; Bieber, Clem, Evenson, Oh, Pyle, et al, ; Ruffolo et al, ).…”

Section: Introductionmentioning

confidence: 99%

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Direct Determination of a Bare Neutron Counter Yield Function

et al. 2020

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Ground-based neutron counters are a standard tool for detecting atmospheric showers from GeV range primary cosmic rays of either solar or galactic origin. Bare neutron counters, a type of lead-free neutron monitor, function much like standard neutron monitors but have different yield functions primarily because they are more sensitive to neutrons of lower energy. When operated together with standard monitors, the different yield functions allow estimates to be made of the energy spectrum of galactic or solar particles. In 2010 a new array of 12 bare neutron detectors was installed at the South Pole to operate together with the neutron monitor there. Prior to installation, two of the detectors were operated on a ship that traveled from Sweden to Antarctica and back from November 2009 to April 2010. The purpose of this latitude survey was to use Earth's magnetic field as a spectrometer, blocking cosmic rays below the local cutoff rigidity (momentum per unit charge), from which we determined the response function versus rigidity of these bare counters. By comparing that measured response function to direct measurements of the cosmic ray spectrum taken by the PAMELA spacecraft, we were able to make a direct determination of the yield function for these detectors.

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“…Here, we modeled the NM response using a new NM yield function computed for several altitudes by Mishev et al [2013Mishev et al [ , 2020, which is fully consistent with the experimental latitude and altitude surveys and was recently validated by achieving good agreement between model results and space-borne with AMS 02 and ground-based NM measurements [for details see Gil et al, 2015;Lara et al, 2016;Usoskin et al, 2017;Nuntiyakul et al, 2018;Koldobskiy et al, 2019b;Mishev et al, 2020]. Therefore, the response of each NM was modeled with a yield function corresponding to the exact station's altitude a.s.l., which allowed us to reduce model uncertainties related to the application of the double-attenuation-lengths method, i.e.…”

Section: Analysis Of # Gle 71 Using Nm Recordsmentioning

confidence: 90%

Application of the Verified Neutron Monitor Yield Function for an Extended Analysis of the GLE # 71 on 17 May 2012

et al. 2021

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Intense solar activity was observed in May 2012. A notable ground level enhancement (GLE) was registered on 17 May 2012 by several space‐borne instruments as well as on ground by neutron monitors (NMs). This event is known as GLE # 71. Here, we derived the spectral and angular characteristics, and apparent source position of the solar protons during the GLE # 71, employing verified newly computed NM yield function and sophisticated unfolding procedure. We considerably improved the previously derived information about the spectra and angular distribution, namely, the precision, time span, and time resolution of the derived characteristics, specifically during the event onset and late phase. A comparison with direct measurements, with the Payload for Antimatter Matter Exploration and Light‐nuclei Astrophysics (PAMELA) experiment, of the particle fluence was performed, and good agreement between NM and direct space‐borne data analysis was achieved. Subsequently, we computed the effective dose rates in the polar region at several altitudes during the event using the derived rigidity spectra of the solar protons as a reliable input for the corresponding radiation model. The contribution of the galactic cosmic rays and solar protons to the exposure is explicitly considered. We computed the integrated exposure during the event and discussed the exposure of crew members/passengers to radiation at several altitudes.

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Bare Neutron Counter and Neutron Monitor Response to Cosmic Rays During a 1995 Latitude Survey

Cited by 31 publications

References 31 publications

Updated Neutron‐Monitor Yield Function: Bridging Between In Situ and Ground‐Based Cosmic Ray Measurements

Updated Neutron‐Monitor Yield Function: Bridging Between In Situ and Ground‐Based Cosmic Ray Measurements

Direct Determination of a Bare Neutron Counter Yield Function

Application of the Verified Neutron Monitor Yield Function for an Extended Analysis of the GLE # 71 on 17 May 2012

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