High-Energy Astrophysics

By F. Melia. Undergraduate Lecture Notes in Physics, 2009

830 citations recorded by the source corpus.

During a dramatic development of the field over the last decade, German groups and institutions have played central, often decisive, roles in high-energy astrophysics. Both spatially resolved and temporal studies of gamma-ray sources are conducted with unprecedented sensitivity, deciphering the physical processes in Galactic and extragalactic sources of high-energy emission, and providing new insights into fundamental physics. Radio observations of compact objects, especially black holes and neutron stars, permit exploring physics under extreme conditions and testing for fundamental properties such as the existence of event horizons around black holes. Observations of ultra-high energy cosmic rays provide information on particle acceleration at the highest energy. The first detection in 2013 of cosmic high-energy neutrinos was named the Physics World breakthrough of the year.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1319b53ab8507ddaa020898cc4e03a8d338bccac

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In Astronomy and Astrophysics

1. A. Banday
2. H. Eriksen
3. E. Quataert
4. Bing Zhang
5. F. Hansen
6. P. Hopkins
7. P. Lilje
8. Andrey V. Kravtsov

In Nuclear and High Energy Physics

1. M. Hardcastle
2. E. Quataert
3. Bing Zhang
4. A. Banday
5. H. Eriksen
6. P. Lilje
7. F. Hansen
8. D. Harris

Citations in the corpus

• Implications of High-Resolution Simulations on Indirect Dark Matter Searches (2009, background): “The energy loss rate ascribed to positrons will be dE/dt = −b(E) = −b0E(2), with b0 = (τloss × 1 GeV)−1 = 10−16s−1GeV−1, which is a reasonable approximation accounting for the inverse Compton loss on CMB, starlight and dust radiation and for the synchrotron loss [62, 78, 85].”
• THE PHYSICS OF THE FAR-INFRARED–RADIO CORRELATION. I. CALORIMETRY, CONSPIRACY, AND IMPLICATIONS (2009, methodology): “…electrons and protons in equation (1) is uncertain, and probably varies from normal spirals like our own, where losses are mainly diffusive (e.g., Longair 1994), to dense starbursts like M82 and Arp 220, where CRs are likely advected in a large-scale galactic wind (e.g., Seaquist & Odegard 1991).”
• Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization (2014, background): “Recently, Liu et al. (2014) have argued that MDE may be contributing to the microwave emission of Galactic radio loops, in particular Loop I.”
• Numerical modelling of the lobes of radio galaxies in cluster environments (2013, methodology): “1, described by Mignone et al. (2007). We chose to use PLUTO because of its good handling of high Mach number flows and the simplicity with which new problems can be defined.”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “There are excellent books that cover this topic in detail such as the monograph by Rybicki and Lightman [123], and books on high energy astrophysics by Longair [124], Krolik [125], Dermer andMenon [126], Kulsrud [127].”
• Pulsars as the sources of high energy cosmic ray positrons (2008, neutral): “[24]):”
• The Westerbork SINGS survey - II Polarization, Faraday rotation, and magnetic fields (2009, background): “G A ] 2 5 M ay 2 00 9 where α is the spectral index (e.g., Longair 1994).”
• New potentialities of the Liege intranuclear cascade (INCL) model for reactions induced by nucleons and light charged particles (2012, background): “In the last years, there has been a very strong development of applications involving spallation reactions, including neutron sources for condensed matter and material studies [1], transmutation of nuclear waste [2, 3], simulation of experimental set-ups in nuclear and particle physics [4], producti”
• The Origins of X-Ray Emission from the Hot Spots of FR II Radio Sources (2004, background): “Even if the proton to electron energy densiti s were of the order of their number ratios as observed in cosmic rays at the Earth (an energy-d pendent factor of∼ 50–100, Longair 1992) we would expectR to increase by a factor∼ 5–10.”
• PARTICLE ACCELERATION AND PLASMA DYNAMICS DURING MAGNETIC RECONNECTION IN THE MAGNETICALLY DOMINATED REGIME (2015, methodology): “In order to estimate the acceleration rate α, the energy change of each particle can be approximated by a relativistic collision formula (e.g., Longair 1994) ∆ε = ( Γ2V (1 + 2V vx c2 + V 2 c2 )− 1 ) ε, (7) where V is the outflow speed, Γ2V = 1/(1− V 2/c2), and vx is the particle velocity in the x…”