E. L. Chupp

Gamma-Ray Astronomy (eBook, PDF)

Nuclear Transition Region

• Format: PDF

Produktbeschreibung

Observation of discrete energy electromagnetic emissions from celestial objects in the radio, IR, optical, lN, and X-ray spectral regions has dramatically advanced our know ledge in the field of astrophysics. It is expected that identification of nuclear 'Y-ray line emissions from any cosmic source would also prove to be a powerful new tool for probing the Universe. Since the publication of Morrison's work in 1958, many experiments were carried out searching for evidence of 'Y-ray lines from cosmic sources, however with little success. Only a few positive experimental results have been reported, in spite of an expenditure of considerable effort by many people: in particular, the possible Galactic Center emission line (473 to 530keV) and 'Y-ray lines at several energies (e. g. , 0. 5 MeV and 2. 2 MeV) associated with large solar flares. Both of these observations are unconfirmed by indepen dent observations (ca. 1975). The high energy 'Y-rays (>30MeV) from the Galactic Center are at least partly due to the decay of 1[0 mesons, which are of unique energy (67. 5 MeV) in the 1[0 rest frame only. The reasons for the limited amount of data avail able in this field, even though early theoretical predictions were very optimistic regarding fluxes of nuclear lines, are that experimental efforts are plagued with high backgrounds and low fluxes, and that development of instruments with telescopic properties in the energy range of interest is difficult.

---

Dieser Download kann aus rechtlichen Gründen nur mit Rechnungsadresse in A, B, BG, CY, CZ, D, DK, EW, E, FIN, F, GR, HR, H, IRL, I, LT, L, LR, M, NL, PL, P, R, S, SLO, SK ausgeliefert werden.

Produktdetails

• Verlag: Springer Netherlands
• Seitenzahl: 336
• Erscheinungstermin: 6. Dezember 2012
• Englisch
• ISBN-13: 9789401014960
• Artikelnr.: 44173450

Inhaltsangabe

I. Introduction.
1.1. Brief History of Attempts to Detect Celestial ?
Rays < 50 MeV.
1.2. Astrophysical Significance of ?
Ray Line Astronomy.
II. Mechanisms for ?
Ray Line and Continuum Production.
2.1. Basic Mechanisms and Sources.
2.2. Thermal Radiation Field.
2.3. Particle
Field Interactions.
2.4. Particle
Matter Interactions.
2.5. Special Effects.
2.6. Summary of ?
Ray Spectra.
III. Theoretical Estimates of ?
Ray Emission.
3.1. Solar ?
Rays.
3.2. Cosmic Sources (Point and Localized).
3.3. Cosmic Diffuse Sources.
IV. Interaction of ?
Rays with Matter.
4.1. ?
Ray Properties.
4.2. Interaction Processes.
V. ?
Ray Flux Observations.
5.1. Solar Observations.
5.2. Cosmic Observations (Point and Localized Sources).
5.3. Diffuse ?
Ray Flux Observations (100 keV to 100 MeV).
5.4. Transient ?
Ray Bursts.
VI. Experimental Considerations for Nuclear ?
Ray Astronomy.
6.1. Background Factors.
6.2. Design Limitations.
6.3. Current Detection Methods.
VII. Conclusions.
Notes Added in Proof.
Appendices.
A. Attenuation Coefficients for ?
Ray Interactions.
B. Conversion Factors for Energy Units.
References.

---

I. Introduction.- 1.1. Brief History of Attempts to Detect Celestial ?-Rays < 50 MeV.- 1.2. Astrophysical Significance of ?-Ray Line Astronomy.- II. Mechanisms for ?-Ray Line and Continuum Production.- 2.1. Basic Mechanisms and Sources.- 2.2. Thermal Radiation Field.- 2.3. Particle-Field Interactions.- 2.4. Particle-Matter Interactions.- 2.5. Special Effects.- 2.6. Summary of ?-Ray Spectra.- III. Theoretical Estimates of ?-Ray Emission.- 3.1. Solar ?-Rays.- 3.2. Cosmic Sources (Point and Localized).- 3.3. Cosmic Diffuse Sources.- IV. Interaction of ?-Rays with Matter.- 4.1. ?-Ray Properties.- 4.2. Interaction Processes.- V. ?-Ray Flux Observations.- 5.1. Solar Observations.- 5.2. Cosmic Observations (Point and Localized Sources).- 5.3. Diffuse ?-Ray Flux Observations (100 keV to 100 MeV).- 5.4. Transient ?-Ray Bursts.- VI. Experimental Considerations for Nuclear ?-Ray Astronomy.- 6.1. Background Factors.- 6.2. Design Limitations.- 6.3. Current Detection Methods.- VII. Conclusions.- Notes Added in Proof.- Appendices.- A. Attenuation Coefficients for ?-Ray Interactions.- B. Conversion Factors for Energy Units.- References.