GALPROP WebRun: an internet-based service for calculating galactic

 cosmic ray propagation and associated photon emissions

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Abstract

GALPROP is a numerical code for calculating the galactic propagation of relativistic charged particles and the diffuse emissions produced during their propagation. The code incorporates as much realistic astrophysical input as possible together with latest theoretical developments and has become a de facto standard in astrophysics of cosmic rays. We present GALPROP WebRun, a service to the scientific community enabling easy use of the freely available GALPROP code via web browsers. In addition, we introduce the latest GALPROP version 54, available through this service.

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The Leiden/Argentine/Bonn (LAB) Survey of Galactic HI: Final data release of the combined LDS and IAR surveys with improved stray-radiation corrections

W. Poppel, E. Arnal, P. Kalberla … (2005)

We present the final data release of observations of lambda 21-cm emission from Galactic neutral hydrogen over the entire sky, merging the Leiden/Dwingeloo Survey (LDS: Hartmann & Burton, 1997) of the sky north of delta = -30 deg with the Instituto Argentino de Radioastronomia Survey (IAR: Arnal et al., 2000, and Bajaja et al., 2005) of the sky south of delta = -25 deg. The angular resolution of the combined material is HPBW ~ 0.6 deg. The LSR velocity coverage spans the interval -450 km/s to +400 km/s, at a resolution of 1.3 km/s. The data were corrected for stray radiation at the Institute for Radioastronomy of the University of Bonn, refining the original correction applied to the LDS. The rms brightness-temperature noise of the merged database is 0.07 - 0.09 K. Residual errors in the profile wings due to defects in the correction for stray radiation are for most of the data below a level of 20 - 40 mK. It would be necessary to construct a telescope with a main beam efficiency of eta_{MB} > 99% to achieve the same accuracy. The merged and refined material entering the LAB Survey of Galactic HI is intended to be a general resource useful to a wide range of studies of the physical and structural characteristices of the Galactic interstellar environment. The LAB Survey is the most sensitive Milky Way HI survey to date, with the most extensive coverage both spatially and kinematically.

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Cosmic-ray propagation and interactions in the Galaxy

Igor V. Moskalenko, Andrew W. Strong, Vladimir S. Ptuskin (2007)

We survey the theory and experimental tests for the propagation of cosmic rays in the Galaxy up to energies of 10^15 eV. A guide to the previous reviews and essential literature is given, followed by an exposition of basic principles. The basic ideas of cosmic-ray propagation are described, and the physical origin of its processes are explained. The various techniques for computing the observational consequences of the theory are described and contrasted. These include analytical and numerical techniques. We present the comparison of models with data including direct and indirect - especially gamma-ray - observations, and indicate what we can learn about cosmic-ray propagation. Some particular important topics including electrons and antiparticles are chosen for discussion.

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Propagation of cosmic-ray nucleons in the Galaxy

I Moskalenko, A. Strong (1998)

We describe a method for the numerical computation of the propagation of primary and secondary nucleons, primary electrons, and secondary positrons and electrons. Fragmentation and energy losses are computed using realistic distributions for the interstellar gas and radiation fields, and diffusive reacceleration is also incorporated. The models are adjusted to agree with the observed cosmic-ray B/C and 10Be/9Be ratios. Models with diffusion and convection do not account well for the observed energy dependence of B/C, while models with reacceleration reproduce this easily. The height of the halo propagation region is determined, using recent 10Be/9Be measurements, as >4 kpc for diffusion/convection models and 4-12 kpc for reacceleration models. For convection models we set an upper limit on the velocity gradient of dV/dz < 7 km/s/kpc. The radial distribution of cosmic-ray sources required is broader than current estimates of the SNR distribution for all halo sizes. Full details of the numerical method used to solve the cosmic-ray propagation equation are given.

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Author and article information

Journal

Publication date Created: 2010-08-21

Publication date Updated: 2011-08-08

Article

DOI: 10.1016/j.cpc.2011.01.017

ArXiV ID: 1008.3642

SO-VID: 84dd2910-c9d5-4d43-804d-6a45c1824577

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http://arxiv.org/licenses/nonexclusive-distrib/1.0/

History

Custom metadata

Journal reference Computer Physics Communications Volume 182, Issue 5, May 2011, Pages 1156-1161

Comments Accepted for publication in Computer Physics Communications. Version 2 includes improvements suggested by the referee. Metadata completed in version 3 (no changes to the manuscript)

Categories astro-ph.HE astro-ph.GA physics.comp-ph

ScienceOpen disciplines: Galaxy astrophysics,Mathematical & Computational physics,High energy astrophysical phenomena

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ScienceOpen disciplines: Galaxy astrophysics, Mathematical & Computational physics, High energy astrophysical phenomena

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