Detection of the Characteristic Pion-Decay Signature in Supernova Remnants

Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, Luca; Ballet, J.; Barbiellini, G.; Baring, Matthew G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, Pascal; Buehler, R.; Busetto, G.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chaty, S.; Chaves, R. C. G.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Chiaro, G.; Cillis, A.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L.; Conrad, J.; Corbel, S.; Cutini, S.; D’Ammando, F.; Angelis, A. De; Palma, F. de; Dermer, C. D.; Silva, E. Do Couto E; Drell, P. S.; Drlica-Wagner, A.; Falletti, L.; Favuzzi, C.; Ferrara, E. C.; Franckowiak, A.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M.-H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hayashi, Katsuhiro; Hays, E.; Hewitt, John W.; Hill, A. B.; Hughes, R. E.; Jackson, M. S.; Jogler, T.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Kataoka, J.; Katsuta, J.; Knödlseder, J.; Kuss, M.; Landé, J.; Larsson, Stefan; Latronico, L.; Lemoine‐Goumard, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Madejski, G.; Massaro, F.; Mayer, M.; Mazziotta, M. N.; McEnery, J. E.; Méhault, J.; Michelson, P. F.; Mignani, Roberto; Mitthumsiri, W.; Mizuno, T.; Моисеев, А. А.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, Takeshi; Nemmen, R.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orienti, M.; Orlando, E.; Ormes, J. F.; Paneque, D.; Perkins, J. S.; Pesce-Rollins, M.; Piron, F.; Pivato, G.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Ritz, S.; Romoli, C.; Sánchez‐Conde, Miguel A.; Schulz, A.; Sgrò, C.; Simeon, Paul; Siskind, E. J.; Smith, David Stanley; Spandre, G.; Spinelli, P.; Stecker, F. W.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, Tadayuki; Tanaka, Takaaki; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Tinivella, M.; Troja, E.; Uchiyama, Y.; Usher, T.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Werner, M. W.; Winer, B. L.; Wood, K. S.; Wood, M.; Yamazaki, Ryo; Yang, Z.; Zimmer, S.

doi:10.1126/science.1231160

Cited by 759 publications

(587 citation statements)

References 37 publications

Supporting

Mentioning

556

Contrasting

Unclassified

Order By: Relevance

“…For comparison, the Superthermal and Thermal Ion Composition (STATIC) instrument aboard MAVEN measured the energy of planetary ions during peak flux to be ∼ 10 8 eV cm −2−1 s −1 (Dong et al 2015). For charged particles from nearby supernova, we took the spectral parameter values from Ackermann et al (2013) for W44 (measured by Fermi-LAT) assuming that 10% of the total energy was emitted in cosmic rays. We obtain 1.6×10 17 eV cm −2 spread over 100 years giving the rate of 2.6×10 8 eV cm −2 s −1 at 100 pc.…”

Section: Resultsmentioning

confidence: 99%

See 1 more Smart Citation

Did high-energy astrophysical sources contribute to Martian atmospheric loss?

Atri¹

2016

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

Mars is believed to have had a substantial atmosphere in the past. Atmospheric loss led to depressurization and cooling, and is thought to be the primary driving force responsible for the loss of liquid water from its surface. Recently, MAVEN observations have provided new insight into the physics of atmospheric loss induced by ICMEs and solar wind interacting with the Martian atmosphere. In addition to solar radiation, it is likely that its atmosphere has been exposed to radiation bursts from high-energy astrophysical sources which become highly probable on timescales of ∼Gy and beyond. These sources are capable of significantly enhancing the rates of photoionization and charged particle-induced ionization in the upper atmosphere. We use Monte Carlo simulations to model the interaction of charged particles and photons from astrophysical sources in the upper Martian atmosphere and discuss its implications on atmospheric loss. Our calculations suggest that the passage of the solar system though dense interstellar clouds is the most significant contributor to atmospheric loss among the sources considered here.

show abstract

Section: Resultsmentioning

confidence: 99%

“…Only a fraction of that energy is released in form of gamma rays and accelerated particles. Recent observations of IC 443 and W44 have suggested that the energy released in cosmic rays is between 1 to 10% of the total energy or 10 49 to 10 50 erg (Ackermann et al 2013).…”

Section: Nearby Supernovaementioning

confidence: 99%

Did high-energy astrophysical sources contribute to Martian atmospheric loss?

Atri¹

2016

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

show abstract

“…This theory has been taught so much at school that to even question the SNR origin of Galactic Cosmic Rays at this stage is treated as heresy. 2 In any event, this theory has received strong support from Fermi-LAT and AGILE observations of the π 0 → 2γ feature in IC 443 and W44 [15], as well as in the spectrum of a 3rd Fermi-LAT SNR, W51C, reported at this workshop by Dr. Jogler.…”

Section: The Cosmic-ray Spectrum In the Local Interstellar Mediummentioning

confidence: 99%

Impact of Fermi-LAT and AMS-02 results on cosmic-ray astrophysics

Dermer

2015

EPJ Web of Conferences

View full text Add to dashboard Cite

Abstract. This article reviews a few topics relevant to Galactic cosmic-ray astrophysics, focusing on the recent AMS-02 data release and Fermi Large Area Telescope data on the diffuse Galactic γ -ray emissivity. Calculations are made of the diffuse cosmic-ray induced p + p → π 0 → 2γ spectra, normalized to the AMS-02 cosmic-ray proton spectrum at ≈ 10 − 100 GV, with and without a hardening in the cosmic-ray proton spectrum at rigidities R 300 GV. A single power-law momentum "shock" spectrum for the local interstellar medium cosmic-ray proton spectrum cannot be ruled out from the γ -ray emissivity data alone without considering the additional contribution of electron bremsstrahlung. Metallicity corrections are discussed, and a maximal range of nuclear enhancement factors from 1.52 to 1.92 is estimated. Origins of the 300 GV cosmic-ray proton and α-particle hardening are discussed.

show abstract

“…The recent Fermi-LAT observations of the so-called molecular SNRs W44 and IC 443 (Abdo et al 2010a(Abdo et al ,2010bAckermann et al 2013) indicate that the spectra of the gamma-ray producing protons (integrated over the emission region) are typically steeper than the DSA predictions for the spectra of the CRs confined in the acceleration region. The steep photon spectra has been found in the high energy gamma-ray spectra of some other remnants measured by, e.g., the CANGAROO (Enomoto et al 2002), H.E.S.S (Aharonian et al 2006) and MAGIC (Carmona 2011) atmospheric Cherenkov telescopes.…”

Section: Gamma-ray Observationsmentioning

confidence: 99%

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

Bykov

Malkov

Raymond

et al. 2013

Microphysics of Cosmic Plasmas

View full text Add to dashboard Cite

In this review we discuss some observational aspects and theoretical models of astrophysical collisionless shocks in partly ionized plasma with the presence of nonthermal components. A specific feature of fast strong collisionless shocks is their ability to accelerate energetic particles that can modify the shock upstream flow and form the shock precursors. We discuss the effects of energetic particle acceleration and associated magnetic field amplification and decay in the extended shock precursors on the line and continuum multi-wavelength emission spectra of the shocks. Both Balmer-type and radiative astrophysical shocks are discussed in connection to supernova remnants interacting with partially neutral clouds. Quantitative models described in the review predict a number of observable line-like emission features that can be used to reveal the physical state of the matter in the shock precursors and the character of nonthermal processes in the shocks. Implications of recent progress of gamma-ray observations of supernova remnants in molecular clouds are highlighted.

show abstract

Detection of the Characteristic Pion-Decay Signature in Supernova Remnants

Cited by 759 publications

References 37 publications

Did high-energy astrophysical sources contribute to Martian atmospheric loss?

Did high-energy astrophysical sources contribute to Martian atmospheric loss?

Impact of Fermi-LAT and AMS-02 results on cosmic-ray astrophysics

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

Contact Info

Product

Resources

About