Abundances of ultraheavy elements in the cosmic radiation - Results from HEAO 3

Binns, W. R.; Garrard, T. L.; Gibner, P. S.; Israel, M. H.; Kertzman, M.; Klarmann, J.; Newport, B. J.; Stone, E. C.

doi:10.1086/168082

Cited by 172 publications

(92 citation statements)

References 7 publications

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“…The elements around Z ~ 39, 57, and 82 are dominated by contributions from isotopes produced in the (slow) "s-process" in which production chains stop at short-lived P-decay isotopes. Data from HEAO-3 HNE [65,85] and Ariel-VI [86] show indications of enhancements for element groups which have contributions from nuclei formed predominately in the (rapid) "r-process" of explosive nucleosynthesis (e.g., in regions near Z~ 34, 53, 65, 77, and the actinides). Production of these isotopes requires an environment in which neutron capture rates dominate over nucleon decay.…”

Section: Resultsmentioning

confidence: 99%

“…Trajectory information is provided by a scintillating opticalfiber hodoscope on ACE/CRIS, position-sensitive silicon wafers on Ulysses/HET, or gas-filled drift chambers on ISEE-3. At higher energies, the HEAO-3 Heavy Nuclei Experiment (HNE) [64,65] and the French-Danish C2 [66,67] detectors used ionization chambers, Cherenkov counters and flash tubes to identify incident particles. Magnetic spectrometers have been flown as balloon payloads [68,69,70].…”

Section: Experimental Techniquementioning

confidence: 99%

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Galactic abundances: Report of working group 3

Klecker¹,

Bothmer²,

Cummings³

et al. 2001

AIP Conference Proceedings

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Abstract. We summarize the various methods and their limitations and strengths to derive galactic abundances from in-situ and remote-sensing measurements, both from ground-based observation s and from instruments in space. Because galactic abundances evolve in time and sp ace it is important to obtain information with a variety of different methods covering different regions from the Very Local Insterstellar M edium (VLISM) to the distant galaxy, and different times throughout the evolution of the galaxy. We discuss the study of the present-day VLISM with neutral gas, pickup ions, and Anomalous Cosmic Rays, the study of the local interstellar medium (ISM) at distances < 1.5 kpc utilizing absorption line me asurements in H I clouds, and the study of galactic cosmic rays, sampling contemporary (~ 15 Myr) s ources in the local ISM within a few kiloparsec of the solar system. Solar system abundances, derived from solar abundances and meteorite studies are discussed in several other chapters o f this volume. They provide samples of matter from the ISM from the time of solar system format ion, about 4.5 Gyr ago. The evolution of galactic abundances on longer time scales is discussed in the context of nuclear synthesis in the various contributing stellar objects.

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Section: Resultsmentioning

confidence: 99%

Section: Experimental Techniquementioning

confidence: 99%

Galactic abundances: Report of working group 3

Klecker¹,

Bothmer²,

Cummings³

et al. 2001

AIP Conference Proceedings

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“…• The HEAO-3 apparatus [16], with an exposure of 8 ×10 11 cm 2 sr s did not observe any event with Z > 92, providing an upper limit of 2.9 ×10 −12 cm 2 sr −1 s −1 .…”

Section: Pos(icrc2015)348mentioning

confidence: 90%

New upper limit on strange quark matter flux with the PAMELA space experiment

Ricci¹

2016

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

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In this work we present results for direct search of Strange Quark Matter in cosmic rays with the PAMELA space spectrometer. If this state of matter exists it may be present in cosmic rays as particles, called strangelets, having an anomalously high mass-to-charge (A/Z) ratio. A direct search in space is complementary to those from ground based spectrometers. Furthermore, it has the advantage of being potentially capable of directly identifying these particles, without any assumption on their interaction model with Earth's atmosphere and the long term stability in terrestrial and lunar rocks. In the energy range from 1 to ∼ 1.0 × 10 3 GV no such particles were found in the data collected by PAMELA between 2006 and 2009. An upper limit on the strangelet flux in cosmic rays was therefore set for particles with charge 1 ≤ Z ≤ 8 and in mass 4 ≤ A ≤ 1.2 × 10 5 . This limit as a function of mass and as a function of magnetic rigidity allows to constrain models of SQM production and propagation in the Galaxy.

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“…Two hypotheses are disputed in the literature: one is based on the CR composition controlled by volatility and mass-to-charge ratio Ellison et al 1997), and the other one is based on the first ionisation potential (FIP) of nuclei (e.g., Cassé & Goret 1973). In this work, for each configuration, the source abundances are initialised to the product of the solar system abundances (Lodders 2003), and the value of the FIP taken from Binns et al (1989). The final fluxes are obtained by an iterative calculation of the propagated fluxes, rescaling the element abundances -keeping fixed the relative isotopic abundancesto match experimental data at each step until convergence is reached (see Fig.…”

Section: Source Spectramentioning

confidence: 99%

A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays

Putze

Derome²,

Donato³

et al. 2011

Cosmic Rays for Particle and Astroparticle Physics

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Context. Propagation of charged cosmic-rays in the Galaxy depends on the transport parameters, whose number can be large depending on the propagation model under scrutiny. A standard approach for determining these parameters is a manual scan, leading to an inefficient and incomplete coverage of the parameter space. Aims. In analyzing the data from forthcoming experiments, a more sophisticated strategy is required. An automated statistical tool is used, which enables a full coverage of the parameter space and provides a sound determination of the transport and source parameters. The uncertainties in these parameters are also derived. Methods. We implement a Markov Chain Monte Carlo (MCMC), which is well suited to multi-parameter determination. Its specificities (burn-in length, acceptance, and correlation length) are discussed in the context of cosmic-ray physics. Its capabilities and performances are explored in the phenomenologically well-understood Leaky-Box Model. Results. From a technical point of view, a trial function based on binary-space partitioning is found to be extremely efficient, allowing a simultaneous determination of up to nine parameters, including transport and source parameters, such as slope and abundances. Our best-fit model includes both a low energy cut-off and reacceleration, whose values are consistent with those found in diffusion models. A Kolmogorov spectrum for the diffusion slope (δ = 1/3) is excluded. The marginalised probability-density function for δ and α (the slope of the source spectra) are δ ≈ 0.55−0.60 and α ≈ 2.14−2.17, depending on the dataset used and the number of free parameters in the fit. All source-spectrum parameters (slope and abundances) are positively correlated among themselves and with the reacceleration strength, but are negatively correlated with the other propagation parameters. Conclusions. The MCMC is a practical and powerful tool for cosmic-ray physic analyses. It can be used to confirm hypotheses concerning source spectra (e.g., whether α i α j ) and/or determine whether different datasets are compatible. A forthcoming study will extend our analysis to more physical diffusion models.

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Abundances of ultraheavy elements in the cosmic radiation - Results from HEAO 3

Cited by 172 publications

References 7 publications

Galactic abundances: Report of working group 3

Galactic abundances: Report of working group 3

New upper limit on strange quark matter flux with the PAMELA space experiment

A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays

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