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Title: Stars in Photographic Emulsions Initiated by Deuterons Part II. Theoretical

Abstract

The theory of high energy nuclear stars depends on a theory of nuclear transparency and on a theory of nuclear evaporation. The transparency can be computed on the basis of a model proposed by R. Serber as soon as the interactions between the nucleons and the incident particle are known. The evaporation can be computed on the basis of the statistical model of the nucleus as soon as the nuclear entropy and binding energies of the evaporated particles are known. With approximate values for the above interactions, entropies, and binding energies, a probability distribution has been computed for the number of prongs per star. The results are in qualitative agreement with the observations on photographic emulsions described in Part 1.

Authors:
;
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
Physics Division
OSTI Identifier:
971343
Report Number(s):
UCRL-29-Rev
TRN: US201004%%438
DOE Contract Number:  
DE-AC02-05CH11231
Resource Type:
Technical Report
Country of Publication:
United States
Language:
English
Subject:
99; DEUTERONS; DISTRIBUTION; ENTROPY; EVAPORATION; EVAPORATION MODEL; NUCLEONS; PHOTOGRAPHIC EMULSIONS; PROBABILITY; STARS; STATISTICAL MODELS

Citation Formats

Horning, W., and Baumhoff, L. Stars in Photographic Emulsions Initiated by Deuterons Part II. Theoretical. United States: N. p., 1948. Web. doi:10.2172/971343.
Horning, W., & Baumhoff, L. Stars in Photographic Emulsions Initiated by Deuterons Part II. Theoretical. United States. doi:10.2172/971343.
Horning, W., and Baumhoff, L. Tue . "Stars in Photographic Emulsions Initiated by Deuterons Part II. Theoretical". United States. doi:10.2172/971343. https://www.osti.gov/servlets/purl/971343.
@article{osti_971343,
title = {Stars in Photographic Emulsions Initiated by Deuterons Part II. Theoretical},
author = {Horning, W. and Baumhoff, L.},
abstractNote = {The theory of high energy nuclear stars depends on a theory of nuclear transparency and on a theory of nuclear evaporation. The transparency can be computed on the basis of a model proposed by R. Serber as soon as the interactions between the nucleons and the incident particle are known. The evaporation can be computed on the basis of the statistical model of the nucleus as soon as the nuclear entropy and binding energies of the evaporated particles are known. With approximate values for the above interactions, entropies, and binding energies, a probability distribution has been computed for the number of prongs per star. The results are in qualitative agreement with the observations on photographic emulsions described in Part 1.},
doi = {10.2172/971343},
journal = {},
number = ,
volume = ,
place = {United States},
year = {1948},
month = {9}
}