Gamma-Ray Astronomy: Nuclear Transition Region

摘要: I. Introduction.- 1.1. Brief History of Attempts to Detect Celestial ?-Rays 100 MeV).- e. Supernovae (Prompt Emission).- 3.2.2. Neutron Stars.- 3.2.3. Flare 3.2.4. Galactic Core and Disk.- a. $$ \tilde > 30 MeV.- b. 0.51 MeV Line Radiation.- c. ?-Ray Lines from Cosmic Rays.- 3.2.5. Black Holes.- 3.2.6. Bursts (Vela Class).- 3.3. Diffuse Sources.- IV. Interaction with Matter.- 4.1. Properties.- 4.2. Processes.- 4.2.1. Photoelectric Effect.- 4.2.2. The Compton Polarized Incident Unpolarized 4.2.3. Pair Production.- V. Flux Observations.- 5.1. Solar 5.1.1. OSO-7 Observations in August 1972.- 4 event.- Time Profiles the Positron Annihilation Capture - Event.- Preflare Upper Limits d. Shape 0.5 Continuum f. 7 g. Conclusions Regarding ?-Rays.- 5.2. (Point Localized Sources).- 5.2.1. Supernova Remnants.- Supernovae.- 5.2.2. Disk Center.- 5.2.3. Center lines.- 5.3. (100 keV 5.3.1. 10 5.3.2. (10 5.4. Transient Bursts.- VI. Experimental Considerations for Nuclear Astronomy.- 6.1. Background Factors.- 6.1.1. Ambient Neutral Backgrounds.- Flux.- Atmospheric Intrinsic Activity.- Neutrons.- 6.1.2. Instrument Activation (Local Production).- 6.1.3. Satellite Orbits.- Intermediate Latitudes.- Polar 6.1.4. Space Probes.- 6.1.5. Observed Backgrounds Specific Balloon Experiments.- Alkali Halide Spectrometers.- Solid State Detector Measurements.- Telescope.- 6.2. Design Limitations.- 6.3. Current Detection Methods.- 6.3.1. Shielded Detectors.- HEAO-A Collimated X- Spectrometer.- Collimator Shutter-Occulter (Large Telescope).- Anti-Collimator HEAO-C 6.3.2. Telescopes.- VII. Conclusions.- Notes Added Proof.- Appendices.- A. Attenuation Coefficients Interactions.- B. Conversion Factors Energy Units.- References.