De-Excitation Nuclear Gamma-Ray Line Emission From Low-Energy Cosmic Rays in the Inner Galaxy

Benhabiles-Mezhoud, H.; Kiener, J.; Tatischeff, V.; Strong, A. W.

doi:10.1088/0004-637x/763/2/98

Cited by 33 publications

(49 citation statements)

References 43 publications

(13 reference statements)

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“…Inelastic collisions of LECRs with interstellar gas should produce a rich spectrum of gamma-ray lines between 0.3 and 10 MeV [27]. Spectroscopic observations of these lines with e-ASTROGAM are the only direct way to detect these elusive particles, to measure their energy density in and out of dense clouds, and to measure the production rate of light elements (Li, Be, and B) resulting from their interactions with gas.…”

Section: What Are the Cr Energy Distributions Produced Insidementioning

confidence: 99%

“…The relation with the Fermi Bubbles seen in gamma rays and possibly in microwaves and polarized radio waves is unclear despite their biconical structure and the finding of Predicted gamma-ray emission due to nuclear interactions of CRs in the inner Galaxy. The gamma-ray line emission below 10 MeV is due to LECRs, whose properties in the ISM have been adjusted such that the mean CR ionization rate deduced from H + 3 observations and the Fermi-LAT data (magenta band) at 1 GeV are simultaneously reproduced (adapted from [27]). The 1-year sensitivity of e-ASTROGAM (for Galactic background) is superimposed.…”

Section: The Origin and Energy Content Of Galactic Wind And Fermi Bubmentioning

confidence: 99%

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The e-ASTROGAM mission

et al. 2017

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e-ASTROGAM ('enhanced ASTROGAM') is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV -the lower energy limit can be pushed to energies as low as 150 keV, albeit with rapidly degrading angular resolution, for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA.

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Section: What Are the Cr Energy Distributions Produced Insidementioning

confidence: 99%

Section: The Origin and Energy Content Of Galactic Wind And Fermi Bubmentioning

confidence: 99%

The e-ASTROGAM mission

et al. 2017

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“…1 PeV) being the maximum realistic energy that could be reached by CRs accelerated in SN remnants (Bell 1978;Kotera & Olinto 2011;Bell et al 2013), while higher-energy particles would likely originate from outside the protogalaxy (Hillas 1984;Becker 2008;Kotera & Olinto 2011;Blasi 2014). With a power-law index of Γ = 2.1, the 1 − 10 6 GeV range harbours more than 99% of the total energy content of the CRs (see Benhabiles-Mezhoud et al 2013). CR is the CR energy density -see section 3.2.2 for details, and v CR is the characteristic velocity with which the CRs propagate macroscopically.…”

Section: Transportation and Spectral Evolutionmentioning

confidence: 99%

Hadronic Interactions of Energetic Charged Particles in Protogalactic Outflow Environments and Implications for the Early Evolution of Galaxies

Owen

Jin

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the interactions of energetic hadronic particles with the media in outflows from star-forming protogalaxies. These particles undergo pion-producing interactions which can drive a heating effect in the outflow, while those advected by the outflow also transport energy beyond the galaxy, heating the circumgalactic medium. We investigate how this process evolves over the length of the outflow and calculate the corresponding heating rates in advection-dominated and diffusion-dominated cosmic ray transport regimes. In a purely diffusive transport scenario, we find the peak heating rate reaches 10 −26 erg cm −3 s −1 at the base of the outflow where the wind is driven by core-collapse supernovae at an event rate of 0.1 yr −1 , but does not extend beyond 2 kpc. In the advection limit, the peak heating rate is reduced to 10 −28 erg cm −3 s −1 , but its extent can reach to tens of kpc. Around 10% of the cosmic rays injected into the system can escape by advection with the outflow wind, while the remaining cosmic rays deliver an important interstellar heating effect. We apply our cosmic ray heating model to the recent observation of the high-redshift galaxy MACS1149-JD1 and show that it could account for the quenching of a previous starburst inferred from spectroscopic observations. Re-ignition of later star-formation may be caused by the presence of filamentary circumgalactic inflows which are reinstated after cosmic ray heating has subsided.

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“…This is because less than 1% of the total CR energy is harboured in these lower energy particles (see, e.g. Benhabiles-Mezhoud et al 2013). Higher-energy CRs (i.e.…”

Section: Introductionmentioning

confidence: 99%

Interactions between ultra-high-energy particles and protogalactic environments

Owen

Jacobsen

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We investigate the interactions of energetic hadronic particles (cosmic ray protons) with photons and baryons in protogalactic environments, where the target photons are supplied by the first generations of stars to form in the galaxy and the cosmological microwave background, while the target baryons are the interstellar and circumgalactic medium. We show that pair-production and photo-pion processes are the dominant interactions at particle energies above 10 19 eV, while pp-interaction pion-production dominates at the lower energies in line with expectations from, for example γ-ray observations of star-forming galaxies and dense regions of our own galaxy's interstellar medium. We calculate the path lengths for the interaction channels and determine the corresponding rates of energy deposition. We have found that protogalactic magnetic fields and their evolution can significantly affect the energy transport and energy deposition processes of cosmic rays. Within a Myr after the onset of star-formation the magnetic field in a protogalaxy could attain a strength sufficient to confine all but the highest energy particles within the galaxy. This enhances the cosmic ray driven self-heating of the protogalaxy to a rate of around 10 −24 erg cm −3 s −1 for a galaxy with strong star-forming activity that yields 1 core collapse SN event per year. This heating power exceeds even that due to radiative emission from the protogalaxy's stellar populations. However, in a short window before the protogalaxy is fully magnetised, energetic particles could stream across the galaxy freely, delivering energy into the circumgalactic and intergalactic medium.

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De-Excitation Nuclear Gamma-Ray Line Emission From Low-Energy Cosmic Rays in the Inner Galaxy

Cited by 33 publications

References 43 publications

The e-ASTROGAM mission

The e-ASTROGAM mission

Hadronic Interactions of Energetic Charged Particles in Protogalactic Outflow Environments and Implications for the Early Evolution of Galaxies

Interactions between ultra-high-energy particles and protogalactic environments

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