An estimation of the yield and response functions for the mini neutron monitor

Caballero─López, R. A.

doi:10.1002/2016ja022690

Cited by 18 publications

(13 citation statements)

References 16 publications

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“…During quiet times the energy spectra of protons can be approximated by the force field solution (FFS, see Gleeson & Axford 1968;Caballero-Lopez & Moraal 2004, and references therein). As local interstellar spectrum (LIS) we used the one given by Burger et al (2000),…”

Section: Experiments 6 Modellingmentioning

confidence: 99%

Galactic cosmic ray hydrogen spectra and radial gradients in the inner heliosphere measured by the HELIOS Experiment 6

Marquardt

Heber

2019

A&A

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Context. The HELIOS solar observation probes provide unique data regarding their orbit and operation time. One of the onboard instruments, the Experiment 6 (E6), is capable of measuring ions from 4 to several hundred MeV/nuc. Aims. In this paper we aim to demonstrate the relevance of the E6 data for the calculation of galactic cosmic ray (GCR), anomalous cosmic ray (ACR), and solar energetic particle (SEP) fluxes for different distances from the sun and time periods Methods. Several corrections have been applied to the raw data: determination of the Quenching factor of the scintillator, correction of the temperature dependent electronics, degradation of the scintillator as well as the effects on the edge of semi-conductor detectors. Results. Fluxes measured by the E6 are in accordance with the force field solution for the GCR and match models of the anomalous cosmic ray propagation. GCR radial gradients in the inner heliosphere show a different behaviour than in the outer heliosphere

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Section: Experiments 6 Modellingmentioning

confidence: 99%

Galactic cosmic ray hydrogen spectra and radial gradients in the inner heliosphere measured by the HELIOS Experiment 6

Marquardt

Heber

2019

A&A

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“…Above 10 GV, the simulated results CD00, MAT09, and MAN16b provide a better estimate. More details about comparison between simulated yields can be found in Maurin et al (2015) and Caballero-Lopez (2016). Figure 9(c) compares determinations of the BC response.…”

Section: Comparison With 1976 and 1996 Surveysmentioning

confidence: 99%

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

et al. 2018

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Neutron monitors of standard design (IGY or NM64) are employed worldwide to study variations in the flux of galactic cosmic rays and solar energetic particles in the GeV range. The design minimizes detector response to neutrons below ∼10 MeV produced by cosmic ray interactions in the ambient medium. Increasingly, however, such neutrons are of interest as a means of obtaining spectral information on cosmic rays, for studies of soil moisture, and for nuclear threat detection. Bare neutron counters, a type of lead‐free neutron monitor, can detect such neutrons, but comparatively little work has been done to characterize the dependence of their count rate on cutoff rigidity. We analyze data from three bare neutron counters operated on a ship together with a three‐tube NM64 monitor from November 1995 to March 1996 over a wide range of magnetic latitude, that is, a latitude survey. The bare counter design used foamed‐in‐place polyurethane insulation to keep the temperature uniform and to some extent moderate high‐energy neutrons. When the ship was near land, the bare/NM64 count rate ratio was dramatically higher. Considering only data from open sea, the bare and NM64 pressure coefficients are not significantly different. We determine the response function of these bare counters, which is weighted to Galactic cosmic rays of lower energy than the NM64. This measurement of the response function may improve determination of the spectral index of solar energetic particles and Galactic cosmic rays from a comparison of bare and NM64 count rates.

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“…High stellar activity, e.g., corresponds to strong modulation, i.e., high φ values and, thus, low GCR fluxes and vice versa. According to Caballero-Lopez & Moraal (2004), φ can be derived via:…”

Section: Introductionmentioning

confidence: 99%

A new model suite to determine the influence of cosmic rays on (exo)planetary atmospheric biosignatures

Herbst

Grenfell

Sinnhuber

et al. 2019

A&A

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Context. The first opportunity to detect indications for life outside the Solar System may be provided already within the next decade with upcoming missions such as the James Webb Space Telescope (JWST), the European Extremely Large Telescope (E-ELT) and/or the Atmospheric Remote-sensing Infrared Exoplanet Large-survey (ARIEL) mission, searching for atmospheric biosignatures on planets in the habitable zone of cool K-and M-stars. Nevertheless, their harsh stellar radiation and particle environment could lead to photochemical loss of atmospheric biosignatures. Aims. We aim to study the influence of cosmic rays on exoplanetary atmospheric biosignatures and the radiation environment considering feedbacks between energetic particle precipitation, climate, atmospheric ionization, neutral and ion chemistry, and secondary particle generation. Methods. We describe newly-combined state-of-the-art modeling tools to study the impact of the radiation and particle environment, in particular of cosmic rays, on atmospheric particle interaction, the influence on the atmospheric chemistry and the climate-chemistry coupling in a self-consistent model suite. To this end, models like the Atmospheric Radiation Interaction Simulator (AtRIS), the Exoplanetary Terrestrial Ion Chemistry model (ExoTIC), and the updated coupled climate-chemistry model are combined. Results. Besides comparing our results to Earth-bound measurements, we investigate the ozone-production and -loss cycles as well as the atmospheric radiation dose profiles during quiescent solar periods and during the strong solar energetic particle event of February 23, 1956. Further, the scenario-dependent terrestrial transit spectra, as seen by the NIR-Spec infrared spectrometer onboard the JWST, are modeled. Amongst others, we find that the comparatively weak solar event (i) drastically increases the spectral signal of HNO 3 , while (ii) significantly suppressing the spectral feature of ozone. Because of the slow recovery after such events, the latter indicates that ozone might not be a good biomarker for planets orbiting stars with high flaring rates.

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An estimation of the yield and response functions for the mini neutron monitor

Cited by 18 publications

References 16 publications

Galactic cosmic ray hydrogen spectra and radial gradients in the inner heliosphere measured by the HELIOS Experiment 6

Galactic cosmic ray hydrogen spectra and radial gradients in the inner heliosphere measured by the HELIOS Experiment 6

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

A new model suite to determine the influence of cosmic rays on (exo)planetary atmospheric biosignatures

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