Observation of Cosmic-Ray Antiprotons at Energies below 500 MeV

Yoshimura, K.; Orito, S.; Ueda, I.; Anraku, K.; Golden, R. L.; Imori, M.; Inaba, S.; Kimbell, B.; Kimura, N.; Makida, Y.; Matsumoto, H.; Matsunaga, H.; Mitchell, J. W.; Motoki, M.; Nishimura, Jun; Nozaki, M.; Ormes, J. F.; Saeki, T.; Streitmatter, R. E.; Suzuki, Jun–ichi; Tanaka, Kenichi; Yajima, N.; Yamagami, T.; Yamamoto, A.; Yoshida, Tetsuya

doi:10.1103/physrevlett.75.3792

Cited by 80 publications

(55 citation statements)

References 17 publications

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“…Figure 3(a) presents the measured (p=p) flux ratio. Compared with earlier experiments [2,6], the AMS results extend the rigidity range to 450 GV with increased precision. Figure 2 of Supplemental Material [18] shows the low energy (< 10 GeV) part of our measured (p=p) flux ratio.…”

Section: 091103 (2016) P H Y S I C a L R E V I E W L E T T E R Smentioning

confidence: 54%

“…Of the four charged elementary particles traveling through the cosmos-protons, electrons, positrons, and antiprotons-the experimental data on antiprotons are limited because for each antiproton there are approximately 10 4 protons. Since the observation of antiprotons in cosmic rays [1], many studies of cosmic ray antiprotons have been performed [2][3][4][5][6]. However, to measure the antiproton flux to 1% accuracy requires a…”

mentioning

confidence: 99%

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Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

Aguilar¹,

Cavasonza²,

Alpat³

et al. 2016

Phys. Rev. Lett.

474

560

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International audienceA precision measurement by AMS of the antiproton flux and the antiproton-to-proton flux ratio inprimary cosmic rays in the absolute rigidity range from 1 to 450 GV is presented based on 3.49 × 105antiproton events and 2.42 × 109 proton events. The fluxes and flux ratios of charged elementary particlesin cosmic rays are also presented. In the absolute rigidity range ∼60 to ∼500 GV, the antiproton ¯p, protonp, and positron eþ fluxes are found to have nearly identical rigidity dependence and the electron e− fluxexhibits a different rigidity dependence. Below 60 GV, the ( ¯ p=p), ( ¯ p=eþ), and (p=eþ) flux ratios eachreaches a maximum. From ∼60 to ∼500 GV, the ( ¯ p=p), ( ¯ p=eþ), and (p=eþ) flux ratios show no rigiditydependence. These are new observations of the properties of elementary particles in the cosmos

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Section: 091103 (2016) P H Y S I C a L R E V I E W L E T T E R Smentioning

confidence: 54%

mentioning

confidence: 99%

Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

Aguilar¹,

Cavasonza²,

Alpat³

et al. 2016

Phys. Rev. Lett.

474

560

View full text Add to dashboard Cite

show abstract

“…As another example, let us consider PBHs responsible for antiproton fluxes observed by the BESS experiments [21] or short gamma ray bursts [22]. Such PBHs are evaporating now, which leads to the initial mass M ∼ 3 × 10 −19 M ⊙ .…”

Section: B Primordial Black Holes Formationmentioning

confidence: 99%

“…Furthermore, PBHs are responsible for antiproton fluxes observed by the BESS experiments [21] or short gamma ray bursts [22].…”

Section: B Primordial Black Holes Formationmentioning

confidence: 99%

“…Massive compact halo objects (MACHOs) are observed through gravitational microlensing effects [20], which are a possible candidate of dark matter. Furthermore, PBHs evaporating now may be a source of antiproton flux observed by the BESS experiment [21] or responsible for short gamma ray bursts (GRBs) [22]. Though many double inflations have been considered, they are often discussed in a simple toy model with two massive scalar fields.…”

Section: Introductionmentioning

confidence: 99%

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Density fluctuations and primordial black hole formation in natural double inflation in supergravity

Yamaguchi

2001

Phys. Rev. D

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We investigate the recently proposed natural double inflation model in supergravity. Chaotic inflation first takes place by virtue of the Nambu-Goldstonelike shift symmetry. During chaotic inflation, an initial value of second inflation (new inflation) is set, which is adequately far from the local maximum of the potential due to the small linear term in the Kähler potential. Then, primordial fluctuations within the present horizon scale may be produced during both inflations. Primordial fluctuations responsible for anisotropies of the cosmic microwave background radiation and the large scale structure are produced during chaotic inflation, while fluctuations on smaller scales are produced during new inflation. Because of the peculiar nature of new inflation, they can become as large as 10 −1 -10 −2 , which may lead to the formation of primordial black holes. PACS number(s): 98.80. Cq,04.65.+e,12.60.Jv

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Primordial Black Holes as a Probe of Cosmology and High Energy Physics

Carr

2003

Quantum Gravity

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Observation of Cosmic-Ray Antiprotons at Energies below 500 MeV

Cited by 80 publications

References 17 publications

Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

Density fluctuations and primordial black hole formation in natural double inflation in supergravity

Primordial Black Holes as a Probe of Cosmology and High Energy Physics

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