Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field

Porter, Troy A; V, Moskalenko, Igor; Strong, Andrew W

doi:10.2172/888781

Cited by 19 publications

(29 citation statements)

References 19 publications

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“…The code solves a network of transport equations for Z≥1 nuclei as well as for electrons and positrons while computing energy losses using realistic maps of galactic gas [56] and of the far-infrared, optical and CMB photons that make up the Inter-Stellar Radiation Field (ISRF) [57]. One also has the ability to transfer tabulated Green's functions from GALPROP to DarkSUSY 5.0.4 [58], where the injected spectra of CREs from dark matter annihilations are calculated using all of the details of the SUSY model spectrum and couplings.…”

Section: Consistent Modeling Of the High-energy Skymentioning

confidence: 99%

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Cosmic ray anomalies from the MSSM?

Cotta

Conley

Gainer

et al. 2011

J. High Energ. Phys.

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Abstract:The recent positron excess in cosmic rays (CR) observed by the PAMELA satellite may be a signal for dark matter (DM) annihilation. When these measurements are combined with those from FERMI on the total (e + + e − ) flux and from PAMELA itself on thep/p ratio, these and other results are difficult to reconcile with traditional models of DM, including the conventional mSUGRA version of Supersymmetry even if boosts as large as 10 3−4 are allowed. In this paper, we combine the results of a previously obtained scan over a more general 19-parameter subspace of the MSSM with a corresponding scan over astrophysical parameters that describe the propagation of CR. We then ascertain whether or not a good fit to this CR data can be obtained with relatively small boost factors while simultaneously satisfying the additional constraints arising from gamma ray data. We find that a specific subclass of MSSM models where the LSP is mostly pure bino and annihilates almost exclusively into τ pairs comes very close to satisfying these requirements. The lightestτ in this set of models is found to be relatively close in mass to the LSP and is in some cases the nLSP. These models lead to a significant improvement in the overall fit to the data by an amount ∆χ 2 ∼ 1/dof in comparison to the best fit without Supersymmetry while employing boosts ∼ 100. The implications of these models for future experiments are discussed.

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Section: Consistent Modeling Of the High-energy Skymentioning

confidence: 99%

“…The ISRF is implemented in GALPROP as a multidimensional array split into three components that represent maps of optical (starlight), FIR (reprocessed) and CMB photons as generated in the work [57]. These ISRF-Factors, referred to as F op , F F IR and F CM B here, are simply global normalizations of the three components.…”

Section: Jhep01(2011)064mentioning

confidence: 99%

Cosmic ray anomalies from the MSSM?

Cotta

Conley

Gainer

et al. 2011

J. High Energ. Phys.

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“…The FRaNKIE code is used to calculate the Galaxy-wide spectral intensity distribution for the R12 and F98 models, which is necessary for the lepton IC energy losses and γ-ray production. Its solution method for the radiation transport has evolved from the ray-tracing method initially employed by [13] to using simulation techniques similar to other Monte Carlo radiation transfer codes (e.g., [22,24]) where luminosity packets are injected according to user-specified spatial and spectral distributions, and the propagation history of each packet is traced to produce observables that are recorded at observer locations. The propagation includes self-consistent scattering, absorption, and re-emission by dust , the optical properties and spatial distributions of which are also user-specified.…”

Section: Pos(icrc2017)737mentioning

confidence: 99%

“…Porter & Strong [13] describe the first work to combine the stellar emission with a self-consistent dust scattering/absorption/reemission radiation transfer calculation using the FRaNKIE 1 code. Porter et al [14] extended the calculations to produce also the spatially varying anisotropic intensity of the ISRF using a 2D stellar and dust density distribution.…”

Section: Introductionmentioning

confidence: 99%

The Interstellar Radiation Field of the Milky Way in Three Spatial Dimensions

Porter¹,

Jóhannesson²,

Moskalenko³

2017

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

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The interstellar radiation field (ISRF) of the Milky Way is the result of emission by stars and re-processing of the starlight by dust in the interstellar medium. The ISRF is an essential input to cosmic-ray (CR) propagation codes for calculating the energy losses by leptons from inverse Compton scattering, and the resulting interstellar γ-ray emission. To date, models for the ISRF have used a 2D Galactocentric cylindrical symmetric approximation, which neglects details of Galactic structure such as spiral arms and the asymmetric stellar bulge. In this contribution 3D spatial models for the ISRF are presented that incorporate such spatial elements. Because there is no consensus on the geometry of these structures the calculations presented in this contribution employ descriptions for the stellar luminosity and dust distribution taken from the literature and use the Fast Radiation Numerical Kalculation for Interstellar Emission (FRaNKIE) code to generate corresponding spectral intensity distributions throughout the Galaxy. Locally the models fairly successfully reproduce near-to far-infrared data, despite having distinctly different stellar and dust density distributions. Elsewhere in the Galaxy the 3D intensity distributions reflect the differences due to the input stellar and dust density distributions between the models.

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“…The γ-ray and synchrotron emissivities are calculated using the propagated CR distributions, including a contribution from secondary particles such as positrons and electrons from inelastic processes in the ISM that increases the γ-ray flux at MeV energies [26,27]. The inverse Compton (IC) scattering is treated using the appropriate formalism for an anisotropic radiation field [6] with the full spatial and angular distribution of the interstellar radiation field (ISRF) [26,28]. The electron bremsstrahlung cross section is calculated as described in [7].…”

Section: The Galprop Codementioning

confidence: 99%

GALPROP Code for Galactic Cosmic Ray Propagation and Associated Photon Emissions

Москаленко¹,

Jóhannesson²,

Porter³

2016

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

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Recent years are marked with many breakthroughs in astrophysics of cosmic rays (CRs), and more are expected in the nearest future. Their proper interpretation is impossible without a welldeveloped propagation code. The GALPROP project celebrates its 19th anniversary this year. Over these years the project has established itself as a standard self-consistent model for CR propagation in the Galaxy and associated diffuse emissions (radio, microwave, X-rays, γ-rays) that is widely used by the astrophysical community. The project stimulated independent studies of the interstellar radiation field, distribution of the interstellar gas (H2, H I, H II), synchrotron emission and the Galactic magnetic field, and a new study of the isotopic production cross sections. These studies provide necessary and unique input datasets for the GALPROP model. The code is optimized and parallelized and accessible as a standalone executable or library that can be linked to other codes enabling many other studies, such as Markov Chain Monte Carlo (MCMC), MultiNest, SuperBayeS, and DarkSUSY. We describe a new updated version of the code that has new capabilities and improved accuracy. As always, the latest release of the code is available through the WebRun, a service to the scientific community enabling easy use of the GALPROP code via web browsers.

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Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field

Cited by 19 publications

References 19 publications

Cosmic ray anomalies from the MSSM?

Cosmic ray anomalies from the MSSM?

The Interstellar Radiation Field of the Milky Way in Three Spatial Dimensions

GALPROP Code for Galactic Cosmic Ray Propagation and Associated Photon Emissions

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