PAMELA Measurements of Cosmic-Ray Proton and Helium Spectra

Adriani, O.; Barbarino, G. C.; Bazilevskaya, G. A.; Bellotti, R.; Boezio, M.; Bogomolov, É. A.; Bonechi, L.; Bongi, M.; Bonvicini, V.; Борисов, С. В.; Bottai, S.; Bruno, A.; Cafagna, F.; Campana, D.; Carbone, R.; Carlson, P.; Casolino, M.; Castellini, G.; Consiglio, L.; Pascale, M. P. De; Santis, C. De; Simone, N. De; Felice, V. Di; Galper, A. M.; Gillard, W.; Grishantseva, L.; Jerse, G.; Karelin, A. V.; Koldashov, S. V.; Krutkov, S. Y.; Kvashnin, A. N.; Leonov, A.; Malakhov, V.; Malvezzi, V.; Marcelli, L.; Mayorov, A. G.; Menn, W.; Mikhailov, V. V.; Mocchiutti, E.; Monaco, A.; Mori, N.; Nikonov, N.; Osteria, G.; Palma, F.; Papini, P.; Pearce, Mark; Picozza, P.; Pizzolotto, C.; Ricci, M.; Ricciarini, S.; Rossetto, L.; Sarkar, R.; Simon, M.; Sparvoli, R.; Спиллантини, П.; Stozhkov, Y. I.; Vacchi, A.; Vannuccini, E.; Vasilyev, G.; Voronov, S. A.; Yurkin, Y. T.; Wu, J.; Zampa, G.; Zampa, N.; Zverev, V. G.

doi:10.1126/science.1199172

Cited by 844 publications

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“…4, we show the predicted HERD spectra for protons, helium nuclei, carbon nuclei and iron nuclei, in comparison with all previous direct measurements in space. Clearly HERD will surpass all previous results of directly measured cosmic rays from, e.g., AMS02 [13], ATIC-2 [14], BESS [15], CREAM, [16,17] HEAO [18], JACEE [19], PAMELA [20], RUNJOB [21], SOKOL [22] and TRACER [23], with much better statistics and up to much higher energies even beyond PeV and into the "knee" region. For example, at least ten events will be recorded from 900 TeV to 2 PeV for each specie, which means that the expected energy spectra of most nuclei will be directly extended to the knee range with much smaller error bars than previous direct measurements in space.…”

Section: Item Value Detectormentioning

confidence: 83%

“…Ground-based extensive air shower experiments [6,7,8] continue to make progress [9]; however, these experiments have difficulties in making composition-resolved high-energy resolution measurements of the fine structure of the "knee". On the other hand, experiments based on balloons [14,16], satellites [20], or the international space station [13] can measure the particle energy and charge directly; however, these experiments suffer from small geometrical factor and limited energy range to make statistically meaningful measurements of the "knee".…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Zhang¹,

Adriani²,

Albergo³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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PoS(ICRC2017)1077The High Energy cosmic-Radiation Detection (HERD) facility is one of several space astronomy payloads onboard China's Space Station, which is planned for operation starting around 2025 for about 10 years. The main scientific objectives of HERD are searching for signals of dark matter annihilation products, precise cosmic electron (plus positron) spectrum and anisotropy measurements up to 10 TeV, precise cosmic ray spectrum and composition measurements up to the knee energy, and high energy gamma-ray monitoring and survey. HERD is composed of a 3-D cubic calorimeter (CALO) surrounded by microstrip silicon trackers (STKs) from five sides except the bottom. CALO is made of about 7,500 cubes of LYSO crystals, corresponding to about 55 radiation lengths and 3 nuclear interaction lengths, respectively. The top STK microstrips of six X-Y layers are sandwiched with tungsten converters to make precise directional measurements of incoming electrons and gamma-rays. In the baseline design, each of the four side STKs is made of only three layers microstrips. All STKs will also be used for measuring the charge and incoming directions of cosmic rays, as well as identifying back scattered tracks. With this design, HERD can achieve the following performance: energy resolution of 1% for electrons and gamma-rays beyond 100 GeV and 20% for protons from 100 GeV to 1 PeV; electron/proton separation power better than 10 −5 ; effective geometrical factors of >3 m 2 sr for electron and diffuse gamma-rays, >2 m 2 sr for cosmic ray nuclei. R&D is under way for reading out the LYSO signals with optical fiber coupled to image intensified IsCMOS and CALO prototype of 250 LYSO crystals.

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Section: Item Value Detectormentioning

confidence: 83%

Section: Introductionmentioning

confidence: 99%

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Zhang¹,

Adriani²,

Albergo³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…In turn, the diffusion coefficient affects the CR spectrum observed at Earth. This phenomenon, discussed by [6,7] might play an important role in understanding features on the CR spectrum recently reported by PAMELA [8] and CREAM [9]. This paper is organized as follows: in §2 I will discuss the implications of the NLDSA in terms of magnetic field amplification and how this might mitigate the spectral problem illustrated above.…”

Section: Introductionmentioning

confidence: 94%

“…The PAMELA [8] experiment has provided evidence that the spectra of CR protons and helium nuclei have a break at rigidity ∼ 200 GV. The spectrum of protons measured by PAMELA has a slope 2.85 ± 0.015(stat) ± 3 0.004(syst) at R < 240 GV and 2.67 ± 0.03 ± 0.05 at R > 240 GV.…”

Section: Propagation Of Crs In the Galaxymentioning

confidence: 99%

Origin of Galactic Cosmic Rays

Blasi

2013

Nuclear Physics B - Proceedings Supplements

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The origin of the bulk of cosmic rays (CRs) observed at Earth is the topic of a century long investigation, paved with successes and failures. From the energetic point of view, supernova remnants (SNRs) remain the most plausible sources of CRs up to rigidity ∼ 10 6 − 10 7 GV. This confidence somehow resulted in the construction of a paradigm, the so-called SNR paradigm: CRs are accelerated through diffusive shock acceleration in SNRs and propagate diffusively in the Galaxy in an energy dependent way. Qualitative confirmation of the SNR acceleration scenario has recently been provided by gamma ray and X-ray observations. Diffusive propagation in the Galaxy is probed observationally through measurement of the secondary to primary nuclei flux ratios (such as B/C). There are however some weak points in the paradigm, which suggest that we are probably missing some physical ingredients in our models. The theory of diffusive shock acceleration at SNR shocks predicts spectra of accelerated particles which are systematically too hard compared with the ones inferred from gamma ray observations. Moreover, hard injection spectra indirectly imply a steep energy dependence of the diffusion coefficient in the Galaxy, which in turn leads to anisotropy larger than the observed one. Moreover recent measurements of the flux of nuclei suggest that the spectra have a break at rigidity ∼ 200 GV, which does not sit well with the common wisdom in acceleration and propagation. In this paper I will review these new developments and suggest some possible implications.

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“…This form of source spectrum is chosen so as to reproduce the recently measured proton spectrum by various experiments such as the ATIC [22], CREAM [23], and PAMELA, [24] which exhibit a spectral hardening above ∼ 250 GeV. The observed hardening might be due to the effect of local sources, propagation effects or signature of the cosmicray source spectrum itself (see e.g., Refs.…”

Section: Cosmic-ray Injectionmentioning

confidence: 99%

A possible origin of gamma rays from the Fermi Bubbles

Thoudam¹

2014

Nuclear Physics B - Proceedings Supplements

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One of the most exciting discoveries of recent years is a pair of gigantic gamma-ray emission regions, the socalled Fermi bubbles, above and below the Galactic center. The bubbles, discovered by the Fermi space telescope, extend up to ∼ 50 • in Galactic latitude and are ∼ 40 • wide in Galactic longitude. The gamma-ray emission is also found to correlate with radio, microwave and X-rays emission. The origin of the bubbles and the associated non-thermal emissions are still not clearly understood. Possible explanations for the non-thermal emission include cosmic-ray injection from the Galactic center by high speed Galactic winds/jets, acceleration by multiple shocks or plasma turbulence present inside the bubbles, and acceleration by strong shock waves associated with the expansion of the bubbles. In this paper, I will discuss the possibility that the gamma-ray emission is produced by the injection of Galactic cosmic-rays mainly protons during their diffusive propagation through the Galaxy. The protons interact with the bubble plasma producing π • -decay gamma rays, while at the same time, radio and microwave synchrotron emissions are produced by the secondary electrons/positrons resulting from the π ± decays.

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PAMELA Measurements of Cosmic-Ray Proton and Helium Spectra

Cited by 844 publications

References 33 publications

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Origin of Galactic Cosmic Rays

A possible origin of gamma rays from the Fermi Bubbles

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