The search for antimatter in cosmic rays

Bogomolov, É. A.; Vasil’ev, G. I.; Krutkov, S. Y.; Романов, В. А.; Stepanov, S. V.; Shulakova, M. S.

doi:10.1134/1.1259478

Cited by 3 publications

(3 citation statements)

References 10 publications

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“…The first detections of antiprotons in CRs were reported 35 years ago by Bogomolov et al (1979) and Golden et al (1979). Both experiments reported a flux that was a factor of ∼3 above expectations (Gaisser & Levy 1974) and caused a stir at that time even though the reported excess was only at the ∼3σ level.…”

Section: Introductionmentioning

confidence: 96%

New Calculation of Antiproton Production by Cosmic Ray Protons and Nuclei

Kachelrieß¹,

Moskalenko

Ostapchenko

2015

ApJ

105

124

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A dramatic increase in the accuracy and statistics of space-borne cosmic ray (CR) measurements has yielded several breakthroughs over the last several years. The most puzzling is the rise in the positron fraction above ∼10 GeV over the predictions of the propagation models assuming pure secondary production. The accuracy of the antiproton production cross section is critical for astrophysical applications and searches for new physics since antiprotons in CRs seem to hold the keys to many puzzles including the origin of those excess positrons. However, model calculations of antiproton production in CR interactions with interstellar gas are often employing parameterizations that are out of date or are using outdated physical concepts. That may lead to an incorrect interpretation of antiproton data which could have broad consequences for other areas of astrophysics. In this work, we calculate antiproton production in pp-, pA-, and AA-interactions using EPOS-LHC and QGSJET-II-04, two of the most advanced Monte Carlo (MC) generators tuned to numerous accelerator data including those from the Large Hadron Collider (LHC). We show that the antiproton yields obtained with these MC generators differ by up to an order of magnitude from yields of parameterizations commonly used in astrophysics.

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Section: Introductionmentioning

confidence: 96%

New Calculation of Antiproton Production by Cosmic Ray Protons and Nuclei

Kachelrieß¹,

Moskalenko

Ostapchenko

2015

ApJ

105

124

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“…This was followed by experimental confirmation of the existence of antiprotons in the laboratory [3] and in the cosmic radiation [4,5]. The production of antinuclei in the laboratory with |Z| = 2 has now been confirmed [6].…”

Section: Introductionmentioning

confidence: 96%

Search for Antihelium with the BESS-Polar Spectrometer

Abe¹,

Fuke²,

Haino³

et al. 2012

Phys. Rev. Lett.

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In two long-duration balloon flights over Antarctica, the BESS-Polar collaboration has searched for antihelium in the cosmic radiation with higher sensitivity than any reported investigation. BESS- Polar I flew in 2004, observing for 8.5 days. BESS-Polar II flew in 2007-2008, observing for 24.5 days. No antihelium candidate was found in BESS-Polar I data among 8.4\times 10^6 |Z| = 2 nuclei from 1.0 to 20 GV or in BESS-Polar II data among 4.0\times 10^7 |Z| = 2 nuclei from 1.0 to 14 GV. Assuming antihelium to have the same spectral shape as helium, a 95% confidence upper limit of 6.9 \times 10^-8 was determined by combining all the BESS data, including the two BESS-Polar flights. With no assumed antihelium spectrum and a weighted average of the lowest antihelium efficiencies from 1.6 to 14 GV, an upper limit of 1.0 \times 10^-7 was determined for the combined BESS-Polar data. These are the most stringent limits obtained to date.Comment: 4 pages, 4 figure

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“…The CR leptons were identified in the early 60's with the first measurement of electrons -also called negatrons at that time - (Earl 1961;Meyer & Vogt 1961) and of the positron fraction (de Shong et al 1964;Hartman et al 1965;Agrinier et al 1965;Daniel & Stephens 1965b). Anti-protons are ∼10 −4 times less abundant than protons and were only observed in the late 70's (Bogomolov et al 1979;Golden et al 1979). Anti-deuterons, which are expected to be yet another factor ∼10 −4 below (Chardonnet et al 1997), are still to be detected: the best limit is given by the BESS balloon ; see also Abe et al 2012a for limits on anti-helium), and is still http://lpsc.in2p3.fr/crdb; Contact: crdatabase@lpsc.in2p3.fr three orders of magnitude above what is required to reach the expected astrophysical production.…”

Section: Introductionmentioning

confidence: 99%

A database of charged cosmic rays

Maurin

Melot

Taillet

2014

A&A

169

161

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Aims. This paper gives a description of a new online database and associated online tools (data selection, data export, plots, etc.) for charged cosmic-ray measurements. The experimental setups (type, flight dates, techniques) from which the data originate are included in the database, along with the references to all relevant publications. Methods. The database relies on the MySQL5 engine. The web pages and queries are based on PHP, AJAX and the jquery, jquery.cluetip, jquery-ui, and table-sorter third-party libraries.Results. In this first release, we restrict ourselves to Galactic cosmic rays with Z ≤ 30 and a kinetic energy per nucleon up to a few tens of TeV/n. This corresponds to more than 200 different sub-experiments (i.e., different experiments, or data from the same experiment flying at different times) in as many publications. Conclusions. We set up a cosmic-ray database (CRDB) and provide tools to sort and visualise the data. New data can be submitted, providing the community with a collaborative tool to archive past and future cosmic-ray measurements.

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The search for antimatter in cosmic rays

Cited by 3 publications

References 10 publications

New Calculation of Antiproton Production by Cosmic Ray Protons and Nuclei

New Calculation of Antiproton Production by Cosmic Ray Protons and Nuclei

Search for Antihelium with the BESS-Polar Spectrometer

A database of charged cosmic rays

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