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Relevant bibliographies by topics / Hard Electron Energy Spectra

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Journal articles

Academic literature on the topic 'Hard Electron Energy Spectra'

Author: Grafiati

Published: 6 September 2023

Last updated: 7 September 2023

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Journal articles on the topic "Hard Electron Energy Spectra"

1

Godleski, John J., Rebecca C. Stearns, and Emil J. Millet. "Electron spectroscopic imaging and analysis of electron energy loss spectra with an energy filtering Electron Microscope." Proceedings, annual meeting, Electron Microscopy Society of America 47 (August 6, 1989): 404–5. http://dx.doi.org/10.1017/s0424820100153993.

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The Zeiss CEM902, energy filtering electron microscope, can be used to image the structure of unstained 30 nm sections of biologic materials, to image the distribution of selected elements in such sections, and to determine electron energy loss spectra (EELS) of elements in areas as small as 10 nm. Although the integrated computer in the latest version of the CEM902 can collect and display signals from the scintillation detector for recording EELS, our instrument did not have this capability. Therefore, we have added a Leading Edge Model D personal computer with a 20 Mbyte hard disk, Hercules

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2

Wadiasingh, Zorawar, Matthew G. Baring, Peter L. Gonthier, and Alice K. Harding. "Hard Spectral Tails in Magnetars." Proceedings of the International Astronomical Union 13, S337 (2017): 108–11. http://dx.doi.org/10.1017/s1743921317009073.

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AbstractPulsed non-thermal quiescent emission between 10 keV and around 150 keV has been observed in ~10 magnetars. For inner magnetospheric models of such hard X-ray signals, resonant Compton upscattering of soft thermal photons from the neutron star surface is the most efficient radiative process. We present angle-dependent hard X-ray upscattering model spectra for uncooled monoenergetic relativistic electrons. The spectral cut-off energies are critically dependent on the observer viewing angles and electron Lorentz factor. We find that electrons with energies less than around 15 MeV will em

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3

Khangulyan, Dmitry, Andrew M. Taylor, and Felix Aharonian. "The Formation of Hard Very High Energy Spectra from Gamma-ray Burst Afterglows via Two-zone Synchrotron Self-Compton Emission." Astrophysical Journal 947, no. 2 (2023): 87. http://dx.doi.org/10.3847/1538-4357/acc24e.

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Abstract Electron Compton scattering of target photons into the gamma-ray energy band (inverse Compton scattering; IC) is commonly expected to dominate the very high energy (VHE) spectra in gamma-ray bursts (GRBs) especially during the afterglow phase. For sufficiently large center-of-mass energies in these collisions, the effect of the electron recoil starts reducing the scattering cross-section (the Klein–Nishina regime). The IC spectra generated in the Klein–Nishina regime is softer and has a smaller flux level compared to the synchrotron spectra produced by the same electrons. The detectio

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4

Breuhaus, Mischa, Joachim Hahn, Carlo Romoli, et al. "Ultra-high energy inverse Compton emission from Galactic electron accelerators." EPJ Web of Conferences 280 (2023): 02001. http://dx.doi.org/10.1051/epjconf/202328002001.

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It is generally held that >100 TeV emission from astrophysical objects unambiguously demonstrates the presence of PeV protons or nuclei, due to the unavoidable Klein–Nishina suppression of inverse Compton emission from electrons. However, in the presence of inverse Compton dominated cooling, hard high-energy electron spectra are possible. We show that the environmental requirements for such spectra can naturally be met in spiral arms, and in particular in regions of enhanced star formation activity, the natural locations for the most promising electron accelerators: powerful young pulsars.

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5

Rudawy, P., M. Siarkowski, and R. Falewicz. "Plasma heating in the initial phase of solar flares." Proceedings of the International Astronomical Union 5, S264 (2009): 282–84. http://dx.doi.org/10.1017/s1743921309992791.

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AbstractIn this paper we analyze soft and hard X-ray emission of the 2002 September 20 M1.8 GOES class solar flare observed by RHESSI and GOES satellites, where soft X-ray emission precedes the onset of the main bulk hard X-ray emission by ~5 min. This suggests that an additional heating mechanism may be at work at the early beginning of the flare. However RHESSI spectra indicate presence of the non-thermal electrons also before impulsive phase. So, we assumed that a dominant energy transport mechanism during rise phase of solar flares is electron beam-driven evaporation. We used non-thermal e

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6

Kundu, M. R., S. M. White, N. Gopalswamy, and J. Lim. "Millimeter, Microwave, Hard X-Ray, and Soft X-Ray Observations of Energetic Electron Populations in Solar Flares." International Astronomical Union Colloquium 142 (1994): 599–610. http://dx.doi.org/10.1017/s0252921100077873.

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AbstractWe present comparisons of multiwavelength data for a number of solar flares observed during the major campaign of 1991 June. The different wavelengths are diagnostics of energetic electrons in different energy ranges: soft X-rays are produced by electrons with energies typically below 10 keV, hard X-rays by electrons with energies in the range 10-200 keV, microwaves by electrons in the range 100 keV-1 MeV, and millimeter-wavelength emission by electrons with energies of 0.5 MeV and above. The flares in the 1991 June active period were remarkable in two ways: all have very high turnover

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7

Bespalov, P. A., V. V. Zaitsev, and A. V. Stepanov. "Energetic Particles in a Flare Loop: Spectra and Radiation Signatures." Symposium - International Astronomical Union 142 (1990): 421–27. http://dx.doi.org/10.1017/s0074180900088343.

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It has been shown that high energy particle spectra, particle dynamics, and radiation in a flare loop are determined by wave-particle interactions. The electron-whistler interaction occurs under conditions of strong pitch angle diffusion that makes the particle distribution function isotropic. The flare loop electrons retain information about the particle source spectrum. The interaction of energetic ions with Alfven waves is characterized by strong, moderate, and weak diffusion. The time delays in hard X-ray and gamma-ray emission during one-step acceleration processes might be understood in

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8

Hu, Wen, Da-Hai Yan, and Qiang-Lin Hu. "Two-injection Scenario for the Hard X-Ray Excess Observed in Mrk 421." Astrophysical Journal 948, no. 2 (2023): 82. http://dx.doi.org/10.3847/1538-4357/accc2e.

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Abstract An interesting result that was recently reported for Mrk 421 is the detection of a significant excess at hard X-ray energies, which could provide useful information to investigate particle acceleration and emission mechanisms in the relativistic jet. Considering a two-injection scenario, we develop a self-consistent one-zone leptonic model to understand the origin of the hard X-ray excess in Mrk 421 during the period of extremely low X-ray and very high-energy flux in 2013 January. In the model, two populations of mono-energetic ultra-relativistic electrons are injected into the emiss

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9

Zhang, S. N. "High Energy Continuum Spectra from X-Ray Binaries." International Astronomical Union Colloquium 163 (1997): 41–52. http://dx.doi.org/10.1017/s0252921100042482.

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AbstractA variety of high energy (>1 keV) spectra have been observed in recent years from Black Hole (BH) and Neutron Star (NS) X-ray Binaries (XB). Some common physical components exist between BHXBs and NSXBs, resulting in some high energy spectral features. A common component between a BHXB and a weakly magnetized NSXB is the inner accretion disk region extending very close to the surface (for a NS) or the horizon (for a BH). The inner disk radiation can be described by a multi-color blackbody (MCB) spectral model. The surface radiation of the NS can be approximated by a Single Color Bla

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10

Ham, Seunggi, Jonghyeon Ryu, Hakmin Lee, et al. "Estimation of plasma parameters of X-pinch with time-resolved x-ray spectroscopy." Matter and Radiation at Extremes 8, no. 3 (2023): 036901. http://dx.doi.org/10.1063/5.0131369.

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We estimate the parameters of a Cu plasma generated by an X-pinch by comparing experimentally measured x-rays with synthetic data. A filtered absolute extreme ultraviolet diode array is used to measure time-resolved x-ray spectra with a spectral resolution of ∼1 keV in the energy range of 1–10 keV. The synthetic spectra of Cu plasmas with different electron temperatures, electron densities, and fast electron fractions are calculated using the FLYCHK code. For quantitative comparison with the measured spectrum, two x-ray power ratios with three different spectral ranges are calculated. We obser

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