Experimental Investigation of a High‐Energy Density, High‐Pressure Arc Plasma
dc.contributor.author | Martin, Edward Anthony | en_US |
dc.date.accessioned | 2010-05-06T21:37:15Z | |
dc.date.available | 2010-05-06T21:37:15Z | |
dc.date.issued | 1960-02 | en_US |
dc.identifier.citation | Martin, Edward A. (1960). "Experimental Investigation of a High‐Energy Density, High‐Pressure Arc Plasma." Journal of Applied Physics 31(2): 255-267. <http://hdl.handle.net/2027.42/70092> | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/70092 | |
dc.description.abstract | The underwater spark is utilized to study the fundamental parameters of a plasma at 30 000°K and 10 000 atmos pressure. The 25‐kv spark is obtained by underwater discharge of capacitors having a stored energy of 1800 joules, the inertia of the water providing the confinement necessary to develop high pressures. Phenomena relating to the initiating wire (exploded wire) are discussed. Kerr cell photographs show that spherical structures are formed around both electrodes under certain conditions. A possible explanation is postulated. A detailed energy balance and particle balance are carried out. The results show that the plasma has great capability to store energy in dissociation, excitation, and ionization without a corresponding increase in temperature. The plasma is 30% ionized and the total particle density is about 2×1027 per cubic meter. At this density the plasma radiates a blackbody spectrum. Pressures are obtained by calculation based on the rate of spark channel expansion and the shock properties of water. The plasma is found to have an internal pressure of the same order of magnitude as the external pressure because of interparticle Coulomb forces. Plasma conductivity calculated from equations of Gvosdover and Spitzer and Harm agree very well with the experimental value. The study is basically experimental, with the emphasis in interpretation being placed on reliability of the conclusions rather than on refined accuracy. | en_US |
dc.format.extent | 3102 bytes | |
dc.format.extent | 1357157 bytes | |
dc.format.mimetype | text/plain | |
dc.format.mimetype | application/pdf | |
dc.publisher | The American Institute of Physics | en_US |
dc.rights | © The American Institute of Physics | en_US |
dc.title | Experimental Investigation of a High‐Energy Density, High‐Pressure Arc Plasma | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Physics | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationum | The University of Michigan, Ann Arbor, Michigan | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/70092/2/JAPIAU-31-2-255-1.pdf | |
dc.identifier.doi | 10.1063/1.1735555 | en_US |
dc.identifier.source | Journal of Applied Physics | en_US |
dc.identifier.citedreference | H. C. Early and E. A. Martin, Communication and Electronics (American Institute of Electrical Engineers, New York, 1956), Vol. 22, p. 788. | en_US |
dc.identifier.citedreference | H. H. Rust and H. Drubba, Z. angew. Phys. 5, 251 (1953). | en_US |
dc.identifier.citedreference | Lord Rayleigh, Proc. London Math. Soc. 10, 4 (1878). | en_US |
dc.identifier.citedreference | W. Kleen, Ann. Physik 403, 579 (1931). | en_US |
dc.identifier.citedreference | A star at 29 000 °K should have a greater absorption coefficient for red light than for blue light. See L. H. Aller, Astrophysics, the Atmospheres of the Sun and Stars (Ronald Press Company, New York, 1953), p. 186. | en_US |
dc.identifier.citedreference | G. E. Gibson and W. Heitler, Z. Physik 49, 465 (1928). | en_US |
dc.identifier.citedreference | R. H. Fowler, Statistical Mechanics (Cambridge University Press, Cambridge, 1936), second edition. | en_US |
dc.identifier.citedreference | H. Maecker, Ergeb. exakt. Naturw. 25, 310 (1951). | en_US |
dc.identifier.citedreference | L. Spitzer and R. Harm, Phys. Rev. 89, 977 (1953). | en_US |
dc.owningcollname | Physics, Department of |
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