Constraining Galactic cosmic-ray parameters with<i>Z</i>  ≤  2 nuclei

Coste, B.; Derome, L.; Maurin, D.; Putze, A.

doi:10.1051/0004-6361/201117927

Cited by 84 publications

(109 citation statements)

References 99 publications

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“…An initiative to improve them is described by Moskalenko (2011). A new treatment of the complicated processes involving the light (Z≤ 2) nuclei is given in Coste et al (2012), including for example Deuterium production by p-p fusion reactions. Antiproton production physics also requires improvements to take advantage of current and future data (Kappl & Winkler 2014).…”

Section: Advances In Propagation Modelsmentioning

confidence: 99%

The Nine Lives of Cosmic Rays in Galaxies

Grenier

Black

Strong

2015

Annu. Rev. Astron. Astrophys.

317

294

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Cosmic-ray astrophysics has advanced rapidly in recent years, and its impact on other astronomical disciplines has broadened. Many new experiments, measuring the particles both directly in the atmosphere or space, and indirectly via γ rays and synchrotron radiation, have widened the range and quality of the information available on their origin, propagation, and interactions. The impact of low-energy cosmic rays on interstellar chemistry is a fast-developing topic, including the propagation of these particles into the clouds where the chemistry occurs. Cosmic rays, via their γ-ray production, also provide a powerful way to probe the gas content of the interstellar medium. Substantial advances have been made in the observations and modelling of the interplay between cosmic rays and the interstellar medium. Focussing on energies up to 1 TeV, these inter-relating aspects are covered at various levels of detail, giving a guide to the state of the subject. CONTENTS

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Section: Advances In Propagation Modelsmentioning

confidence: 99%

The Nine Lives of Cosmic Rays in Galaxies

Grenier

Black

Strong

2015

Annu. Rev. Astron. Astrophys.

317

294

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“…These parameter sets result from a secondaryto-primary ratio analysis (Maurin et al 2001) where 26 data points of the boron-to-carbon (B/C) ratio were fitted over the energy range from 0.1 to 35 GeV/n leading to a χ 2 less than 40. The advantage of choosing this study over more recent studies (Putze et al 2010;Coste et al 2012;Trotta et al 2011) J1745 − 3040…”

Section: The Effect Of Cosmic Ray Propagation Uncertaintiesmentioning

confidence: 99%

A new look at the cosmic ray positron fraction

Boudaud

Aupetit

Caroff

et al. 2015

A&A

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130

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Context. The positron fraction in cosmic rays has recently been measured with improved accuracy up to 500 GeV, and it was found to be a steadily increasing function of energy above ∼10 GeV. This behaviour contrasts with standard astrophysical mechanisms, in which positrons are secondary particles, produced in the interactions of primary cosmic rays during their propagation in the interstellar medium. The observed anomaly in the positron fraction triggered a lot of excitement, as it could be interpreted as an indirect signature of the presence of dark matter species in the Galaxy, the so-called weakly interacting massive particles (WIMPs). Alternatively, it could be produced by nearby sources, such as pulsars. Aims. These hypotheses are probed in light of the latest AMS-02 positron fraction measurements. As regards dark matter candidates, regions in the annihilation cross section to mass plane, which best fit the most recent data, are delineated and compared to previous measurements. The explanation of the anomaly in terms of a single nearby pulsar is also explored. Methods. The cosmic ray positron transport in the Galaxy is described using a semi-analytic two-zone model. Propagation is described with Green functions as well as with Bessel expansions. For consistency, the secondary and primary components of the positron flux are calculated together with the same propagation model. The above mentioned explanations of the positron anomaly are tested using χ 2 fits. The numerical package MicrOMEGAs is used to model the positron flux generated by dark matter species. The description of the positron fraction from conventional astrophysical sources is based on the pulsar observations included in the Australia Telescope National Facility (ATNF) catalogue. Results. The masses of the favoured dark matter candidates are always larger than 500 GeV, even though the results are very sensitive to the lepton flux. The Fermi measurements point systematically to much heavier candidates than the recently released AMS-02 observations. Since the latter are more precise, they are much more constraining. A scan through the various individual annihilation channels disfavours leptons as the final state. On the contrary, the agreement is excellent for quark, gauge boson, or Higgs boson pairs, with best-fit masses in the 10 to 40 TeV range. The combination of annihilation channels that best matches the positron fraction is then determined at fixed WIMP mass. A mixture of electron and tau lepton pairs is only acceptable around 500 GeV. Adding b-quark pairs significantly improves the fit up to a mass of 40 TeV. Alternatively, a combination of the four-lepton channels provides a good fit between 0.5 and 1 TeV, with no muons in the final state. Concerning the pulsar hypothesis, the region of the distance-to-age plane that best fits the positron fraction for a single source is determined. Conclusions. The only dark matter species that fulfils the stringent gamma ray and cosmic microwave background bounds is a particle annihilating into...

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“…Although the program is already very complete and contains many physical processes and cross sections, some may be missing, incomplete, or obsolete for specific species. The study of hydrogen and helium isotopes has been shown to be as constraining on propagation models and parameters as the widely used Boron-to-Carbon ratio [14]. Cosmic-ray 2 H and 3 He are mostly secondary particles mainly produced after interactions of 1 H through fusion interaction (for 2 H) and 4 He through fragmentation (for 2 H and 3 He) in the interstellar medium.…”

Section: Introductionmentioning

confidence: 99%

Study of Cosmic-Ray Transport with the GALPROP Code

Picot-Clémente¹,

Seo²,

Strong

et al. 2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The isotopes 2 H and 3 He in the cosmic radiation are mainly secondary products from interactions of primary cosmic rays in the interstellar medium. Secondary-to-primary ratios give important information on processes that occurred during the propagation of cosmic rays, independent of the unknown source spectrum. Boron-to-Carbon ratio data have been primarily used to study cosmicray transport. As statistics have increased and mass resolution have improved, recent measurements on cosmic-ray hydrogen and helium isotopes provide another probe for their propagation in the Galaxy. In this paper, we use the GALPROP program for calculating the propagation of relativistic charged particles. The standard GALPROP software had to be modified to be suitable for hydrogen and helium isotopes in the energy region 0.2 to 1.5 GeV/n. The proton fusion process for production of 2 H had to be implemented, and production cross sections for light isotopes had to be updated at these energies. We will present the modifications made on GALPROP for its application to proton and helium isotopes.

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Constraining Galactic cosmic-ray parameters withZ ≤ 2 nuclei

Cited by 84 publications

References 99 publications

The Nine Lives of Cosmic Rays in Galaxies

The Nine Lives of Cosmic Rays in Galaxies

A new look at the cosmic ray positron fraction

Study of Cosmic-Ray Transport with the GALPROP Code

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