Modelling of the radio emission from the Vela supernova remnant

Sushch, I.; Hnatyk, B.

doi:10.1051/0004-6361/201322569

Cited by 34 publications

(44 citation statements)

References 33 publications

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“…The best fit parameters are: γ Vela = 2.47 ± 0.10, E tot,Vela = (2.28 ± 0.06) · 10 47 erg, γ Cygnus = 2.04 ± 0.04 and E tot,Cygnus = (1.18 ± 0.16) · 10 47 erg. The numbers for the Vela YZ are in agreement with the findings of [42]. The parameter space E totγ selected by the fit to the radio spectrum is reported in the left panel of Fig.…”

Section: Results On the Snr Properties From Radio Datasupporting

confidence: 86%

Multi-messenger constraints to the local emission of cosmic-ray electrons

Manconi

Mauro

Donato

2019

J. Cosmol. Astropart. Phys.

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The data on the inclusive flux of cosmic positrons and electrons (e + + e − ) have been recently collected from GeV to tens of TeV energies by several experiments with unprecedented precision. In addition, the Fermi-LAT Collaboration has provided a new energy spectrum for the upper bounds on the e + + e − dipole anisotropy. This observable can bring information on the emission from local Galactic sources, notably measured with high precision at radio frequencies. We develop a framework in which e − and e + measured at Earth from GeV up to tens of TeV energies have a composite origin. A dedicated analysis is deserved to Vela YZ and Cygnus Loop Supernova Remnants (SNRs), for which we consider two different models for the injection of e − . We investigate the consistency of these models using the three physical observables: the radio flux from Vela YZ and Cygnus Loop at all the available frequencies, the e + + e − flux from five experiments from the GeV to tens of TeV energy, the e + + e − dipole anisotropy upper limits from 50 GeV to about 1 TeV. We find that the radio flux for these nearby SNRs strongly constraints the properties of the injection electron spectrum, partially compatible with the looser constraints derived from the e + + e − flux data. We also perform a multi-wavelength multi-messenger analysis by fitting simultaneously the radio flux on Vela YZ and Cygnus Loop and the e + +e − flux, and checking the outputs against the e + + e − dipole anisotropy data. Remarkably, we find a model which is compatible with all the e + + e − flux data, the radio data for Vela YZ and Cygnus Loop, and with the anisotropy upper bounds. We show the severe constraints imposed by the most recent data on the e + + e − dipole anisotropy.

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Section: Results On the Snr Properties From Radio Datasupporting

confidence: 86%

Multi-messenger constraints to the local emission of cosmic-ray electrons

Manconi

Mauro

Donato

2019

J. Cosmol. Astropart. Phys.

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“…[46][47][48][49][50]). The value of Q 0 is by far non trivial to fix, but can in principle be estimated from radio data on single sources, assuming that the radio flux B ν r at a specific frequency ν is entirely due to synchrotron emission of the ambient electrons in the SNR magnetic field B [14,51,52]: where d is the distance of the source from the observer. The well-known relation between the radio and electron flux index α r = (γ − 1)/2 is here manifest.…”

Section: Primary Electrons From Snrmentioning

confidence: 99%

Interpretation of AMS-02 electrons and positrons data

Mauro

Donato

Fornengo

et al. 2014

J. Cosmol. Astropart. Phys.

163

216

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We perform a combined analysis of the recent AMS-02 data on electrons, positrons, electrons plus positrons and positron fraction, in a self-consistent framework where we realize a theoretical modeling of all the astrophysical components that can contribute to the observed fluxes in the whole energy range. The primary electron contribution is modeled through the sum of an average flux from distant sources and the fluxes from the local supernova remnants in the Green catalog. The secondary electron and positron fluxes originate from interactions on the interstellar medium of primary cosmic rays, for which we derive a novel determination by using AMS-02 proton and helium data. Primary positrons and electrons from pulsar wind nebulae in the ATNF catalog are included and studied in terms of their most significant (while loosely known) properties and under different assumptions (average contribution from the whole catalog, single dominant pulsar, a few dominant pulsars). We obtain a remarkable agreement between our various modeling and the AMS-02 data for all types of analysis, demonstrating that the whole AMS-02 leptonic data admit a self-consistent interpretation in terms of astrophysical contributions.

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“…The latest result of the radio spectrum of Vela Y and Vela Z can be found in Alvarez et al (2001). Sushch & Hnatyk (2014) merge the radio spectrum of Vela Y and Vela Z and obtain a electron spectral index of 2.47. In this case, the electron flux of Vela YZ is about 10 times less than the previous model, mainly due to the much softer spectral index.…”

Section: Monogem Ringmentioning

confidence: 99%

Discriminating local sources of high-energy cosmic electrons and positrons by current and future anisotropy measurements

Fang

Yin

2018

Monthly Notices of the Royal Astronomical Society

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The Fermi-LAT detects no significant anisotropy of the cosmic-ray (CR) electrons and positrons (e − + e + ) with seven years of data, which provides the strongest restriction to the e − + e + anisotropy up to now. As next generation CR observatory, HERD is expected to have a better capability of anisotropy detection than Fermi-LAT. In this paper, we discuss several models aimed to explain the AMS-02 data by the present and future anisotropy measurements. We find that the upper limits of Fermi-LAT disfavor Vela SNR as the dominant source in sub-TeV, while other cases that remain safe under the constraint of Fermi-LAT are expected to be distinguished from each other by HERD. We then discuss the possibilities of remarkable TeV spectral features, and test the corresponding anisotropies. We find the conditions under which the TeV model can have a prominent spectral feature and avoid the constraint of Fermi-LAT at the same time. Furthermore, the expected performance of HERD is sensitive enough to detect the anisotropies of all these TeV models, and even for the case of a featureless TeV spectrum. Thus HERD may play a crucial part in the study of the origin of cosmic electrons and positrons.

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Modelling of the radio emission from the Vela supernova remnant

Cited by 34 publications

References 33 publications

Multi-messenger constraints to the local emission of cosmic-ray electrons

Multi-messenger constraints to the local emission of cosmic-ray electrons

Interpretation of AMS-02 electrons and positrons data

Discriminating local sources of high-energy cosmic electrons and positrons by current and future anisotropy measurements

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