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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 04045naa a2200457 4500 | |
| 001 | oai:DiVA.org:uu-518316 | |
| 003 | SwePub | |
| 008 | 231220s2022 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-5183162 URI |
| 024 | 7 | a https://doi.org/10.22323/1.395.12422 DOI |
| 040 | a (SwePub)uu | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a kon2 swepub-publicationtype |
| 100 | 1 | a Nuntiyakul, W.u Chiang Mai Univ, Dept Phys & Mat Sci, Fac Sci, Chiang Mai 50200, Thailand.;Natl Astron Res Inst Thailand NARIT, Chiang Mai 50180, Thailand.4 aut |
| 245 | 1 0 | a Direct Determination of a Bare Neutron Counter Yield Function |
| 264 | 1 | a Trieste, Italy :b Proceedings of Science,c 2022 |
| 338 | a electronic2 rdacarrier | |
| 520 | a 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 twelve 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 vs. 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. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 650 | 7 | a NATURVETENSKAPx Fysikx Subatomär fysik0 (SwePub)103012 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Subatomic Physics0 (SwePub)103012 hsv//eng |
| 700 | 1 | a Mangeard, P. -S4 aut |
| 700 | 1 | a Ruffolo, D.u Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.4 aut |
| 700 | 1 | a Evenson, P.u Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.4 aut |
| 700 | 1 | a Bieber, J. W.u Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.4 aut |
| 700 | 1 | a Clem, J.u Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.4 aut |
| 700 | 1 | a Hallgren, Allan,d 1951-u Uppsala universitet,Högenergifysik4 aut0 (Swepub:uu)allahall |
| 700 | 1 | a Madsen, J.u Univ Wisconsin Madison, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53703 USA.4 aut |
| 700 | 1 | a Pyle, R.u Pyle Consulting Grp Inc, St Charles, IL 60174 USA.4 aut |
| 700 | 1 | a Saiz, A.u Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.4 aut |
| 700 | 1 | a Tilav, S.u Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.4 aut |
| 710 | 2 | a Chiang Mai Univ, Dept Phys & Mat Sci, Fac Sci, Chiang Mai 50200, Thailand.;Natl Astron Res Inst Thailand NARIT, Chiang Mai 50180, Thailand.b Mahidol Univ, Dept Phys, Fac Sci, Bangkok 10400, Thailand.4 org |
| 773 | 0 | t 37th International Cosmic Ray Conference, ICRC2021d Trieste, Italy : Proceedings of Science |
| 856 | 4 | u https://doi.org/10.22323/1.395.1242y Fulltext |
| 856 | 4 | u https://uu.diva-portal.org/smash/get/diva2:1821541/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print |
| 856 | 4 | u https://pos.sissa.it/395/1242/pdf |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-518316 |
| 856 | 4 8 | u https://doi.org/10.22323/1.395.1242 |
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