摘要:

The size of the focal plane of an optical system is shown to be reduced through the use of re-imaging optics. The general principles of image segmentation and relay optics are discussed as well as trade-offs that must be performed to develop a practical system. A system of re-imaging optics is designed that reduces the necessary detector area of a proposed air shower detector by almost an order of magnitude. ©1998 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.56133

出版商:AIP    

年代:1998

数据来源: AIP

摘要:

We propose a statistical parameterization of hadron production which is verified up to the highest EAS energies. This parameterization leads to Stephan’s type equation of state relating the ‘temperature’ of the relativistic hadron gas with the collision energy if a power multiplicity law is assumed. A correspondence between the lattice theory expansion on the coupling constant and the statistical sum of temperature expansion in statistical mechanics reveals a simple relation between the multiplicity power law index and the coupling constant. Cosmic ray data yield estimates of the running values of the coupling constant beyond the range of collider experiments. These estimates indicate the asymptotic behavior of the running values of the coupling constant and provide a hint that color confinement and asymptotic freedom of quarks co exist in an unified phase of QCD. ©1998 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.56134

出版商:AIP    

年代:1998

数据来源: AIP

摘要:

The goal of space radiation receiver design is achievement of its maximal reflecting properties under some technological and financial restrictions. Optimal design problems of this type are characterized by nonconvex nondifferentiable objective functions. A numerical technique for optimal design of the structures and an applied softwareREFLEXunder development are proposed. ©1998 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.56146

出版商:AIP    

年代:1998

数据来源: AIP

摘要:

A study of space angles and temporal spacing was made for extremely-high energy (EHE) cosmic ray events to see if there are any correlation with Gamma Ray Bursts (GRB’s) recorded by the BATSE experiment on the Compton Gamma Ray Observatory. The results on the most generic correlation using all the recorded GRB’s and EHECR’s show no significant correlation. Nevertheless, the highest-energy cosmic ray “pair” events observed by the AGASA experiments appear to be correlated with the very high fluence GRB’s. Some basis to form a GRB and a fireball is discussed. Empirical analysis of the GRB events strongly implied that the photonic field energy density in the source region should have exceeded the electric energy density of Schwinger field. A possible generation of an initial GRB, its fireball and relativistic shocks therein, is considered in terms of Schwinger field generated by radiation pressure of transient, high luminosity photons provided by collective nuclear collisions of neutron matter. Acceleration of electrons, and some protons, may be possible in the radial electrostatic Schwinger field. Ultra-relativistic shocks might also accelerate particles to certain high energies(&ggr;⩽1012⋅15).Neutral secondaries, including gamma rays, neutrinos, “strangelets,” and Farrar’s SUSYS0particles, are discussed as plausible EHECR pair candidates from GRB fireballs. The OWL/AIRWATCH may be able to explore them from4×1019 eVto well beyond1021 eV.©1998 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.56135

出版商:AIP    

年代:1998

数据来源: AIP

摘要:

Understanding physical mechanisms by which Nature succeeds in bestowing ‘macroscopic’ amounts of energy on single ‘microscopic’ particles remains one of the greatest challenges for both, astrophysicists seeking to understand the functioning of cosmic objects, and accelerator designers inventing new conjectures for more powerful machines. The first and introductory chapter of this contribution is a short retrospective on our early research work, in the ‘Mathematical Physics Division’ at Kiel, on the origin of Ultra High Energy Cosmic Ray Particles (UHECRP), beginning in the sixties and seventies with studies on Atmospheric Particle Propagation, proceeding in the seventies and eighties to investigations on Galactic Particle Transfer, and leading in the eighties and nineties to our present work on mechanisms for particle acceleration in pulsar magnetospheres. Cosmic rays, more than many fields of research, are found to be closely related to other branches ofphysics2.When looking on powerful cosmic accelerators from the point of view of fundamental physics, one has to study charged particle dynamics in extremely strong electromagnetic fields, of a kind that is expected near the surface of rapidly rotating, strongly magnetized neutron stars. Conventional Maxwell Theory (MT), for clearly discernable reasons, does not provide an adequate theoretical means of description in this case. Selfconsistent Electrodynamics (SCED), distinguished from MT through some of its essential premises offers itself, alternatively, as an appropriate language. Therefore, in the second chapter of my talk, I shall outline some features of SCED and reproduce the equation of particle motion on these grounds. In the third and concluding chapter, I shall discuss a mechanism to create very narrow bundles of energetic particles in the polar regions of alignedrotators3.©1998 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.56136

出版商:AIP    

年代:1998

数据来源: AIP

摘要:

At its focal plane, an Orbiting Wide-Angle Light Collector (OWL) will require a highly segmented large area photon detector, able to detect ultraviolet light at the single photoelectron (few photon) level. Depending on the OWL field-of-view and collecting optics, the focal plane detector must have 6 to 20 square meters of contiguous active area segmented into between 0.4 and 1.7 million individual pixels. Each pixel must have a time response of ten nanoseconds to one microsecond, depending on the readout technique, and be able to resolve and record single photoelectrons. The technical requirements of the OWL focal plane detector and possible approaches to its realization will be presented and discussed. A baseline photodetector system is identified. ©1998 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.56137

出版商:AIP    

年代:1998

数据来源: AIP

摘要:

Optical quality polymers normally incorporate functional groups that provide physical integrity that are incompatible with deep UV radiation. Groups like the phenyl ring found in polystyrene (PS) increase the refractive index of the polymer, provide a bulky group that inhibits crystallization rendering the material amorphous, and adds impact strength to the polymer by coupling vibrations of the ring into fracture mechanisms. However these groups also absorb UV light at wavelengths starting at about 330 nm or longer repressing ultra-violet transparency. Our search for a polymer with properties similar to polystyrene or poly(methylmethacrylate) but with better ultraviolet transparency led us to study poly(methylpentene) as a potential lens material candidate. ©1998 American Institute of Physics.

ISSN:0094-243X    

DOI:10.1063/1.56138

出版商:AIP    

年代:1998

数据来源: AIP