Precision Measurement of Boron to Carbon flux ratio in Cosmic Rays from 2 GV to 1.8 TV with the Alpha Magnetic Spectrometer on the International Space Station.

Oliva, A.

doi:10.22323/1.236.0265

Cited by 3 publications

(4 citation statements)

References 15 publications

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“…6. While measurements performed by balloonborn experiments suffer from small statistics and large systematic errors (due to short exposure times and to the effects of the residual overburden atmosphere, respectively), data from space spectrometers like PAMELA and AMS-02, can provide an accurate spectral measurement up to about 1 TeV/n [6,62]. Also in this case, from the experimental point of view, the challenge is then to extend the energy range to the multi TeV/n region by using large geometric factor instruments in space.…”

Section: Ekn [Gev/n]mentioning

confidence: 99%

Selected Topics in Cosmic Ray Physics

Aloisio

Blasi

Mitri

et al. 2018

Multiple Messengers and Challenges in Astroparticle Physics

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The search for the origin of cosmic rays is as active as ever, mainly driven by new insights provided by recent pieces of observation. Much effort is being channelled in putting the so called supernova paradigm for the origin of galactic cosmic rays on firmer grounds, while at the highest energies we are trying to understand the observed cosmic ray spectra and mass composition and relating them to potential sources of extragalactic cosmic rays. Interestingly, a topic that has acquired a dignity of its own is the investigation of the transition region between the galactic and extragalactic components, once associated with the ankle and now increasingly thought to be taking place at somewhat lower energies. Here we summarize recent developments in the observation and understanding of galactic and extragalactic cosmic rays and we discuss the implications of such findings for the modelling of the transition between the two.

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Section: Ekn [Gev/n]mentioning

confidence: 99%

Selected Topics in Cosmic Ray Physics

Aloisio

Blasi

Mitri

et al. 2018

Multiple Messengers and Challenges in Astroparticle Physics

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“…The intrinsic spectral index of CRs s is unobservable and different from the observed one by the diffusion coefficient index, which is usually obtained from observations of the boron-to-carbon ratio(Evoli et al 2015;Oliva 2016;Genolini et al 2015).…”

mentioning

confidence: 99%

GW 150914-like black holes as Galactic high-energy sources

Ioka

Matsumoto

Teraki

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The first direct detections of gravitational waves (GWs) from black hole (BH) mergers, GW150914, GW151226 and LVT151012, give a robust lower limit ∼ 70000 on the number of merged, highly-spinning BHs in our Galaxy. The total spin energy is comparable to all the kinetic energy of supernovae that ever happened in our Galaxy. The BHs release the spin energy to relativistic jets by accreting matter and magnetic fields from the interstellar medium (ISM). By considering the distributions of the ISM density, BH mass and velocity, we calculate the luminosity function of the BH jets, and find that they can potentially accelerate TeV-PeV cosmic-ray particles in our Galaxy with total power ∼ 10 37±3 erg s −1 as PeVatrons, positron factories and/or unidentified TeV gamma-ray sources. Additional ∼ 300 BH jet nebulae could be detectable by CTA (Cherenkov Telescope Array). We also argue that the accretion from the ISM can evaporate and blow away cold material around the BH, which has profound implications for some scenarios to predict electromagnetic counterparts to BH mergers.

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“…To measure the p flux to 1% accuracy requires a separation power between p and p of 10 6 . We use all the AMS detector elements [7] for particle identification and selection among the 65 billion CR triggers recorded.…”

Section: The Ams Detector and Event Selectionmentioning

confidence: 99%

“…The data on e ± have already generated many interesting theoretical models. These models will be constrained by further measurements by AMS such as those described in [6].…”

Section: Introductionmentioning

confidence: 99%