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Journal articles on the topic 'Cosmic rays; Gamma rays'

Author: Grafiati

Published: 4 June 2021

Last updated: 13 February 2022

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1

Osborne, J. L., A. W. Wolfendale, and L. Zhang. "Soft X-rays and cosmic gamma-rays." Monthly Notices of the Royal Astronomical Society 276, no. 2 (September 15, 1995): 409–16. http://dx.doi.org/10.1093/mnras/276.2.409.

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2

KUSENKO, ALEXANDER. "COSMIC CONNECTIONS: FROM COSMIC RAYS TO GAMMA RAYS, COSMIC BACKGROUNDS AND MAGNETIC FIELDS." Modern Physics Letters A 28, no. 02 (January 20, 2013): 1340001. http://dx.doi.org/10.1142/s0217732313400014.

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Combined data from gamma-ray telescopes and cosmic-ray detectors have produced some new surprising insights regarding intergalactic and galactic magnetic fields, as well as extragalactic background light. We review some recent advances, including a theory explaining the hard spectra of distant blazars and the measurements of intergalactic magnetic fields based on the spectra of distant sources. Furthermore, we discuss the possible contribution of transient galactic sources, such as past gamma-ray bursts and hypernova explosions in the Milky Way, to the observed flux of ultrahigh-energy cosmic-rays nuclei. The need for a holistic treatment of gamma rays, cosmic rays, and magnetic fields serves as a unifying theme for these seemingly unrelated phenomena.

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3

Dermer, C. D., and G. Powale. "Gamma rays from cosmic rays in supernova remnants." Astronomy & Astrophysics 553 (April 26, 2013): A34. http://dx.doi.org/10.1051/0004-6361/201220394.

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4

Van Der Walt, D. J., and A. W. Wolfendale. "Gamma rays and the origin of cosmic rays." Space Science Reviews 47, no. 1-2 (March 1988): 1–45. http://dx.doi.org/10.1007/bf00223236.

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5

Szabelski, J., D. J. van der Walt, J. Wdowczyk, and A. W. Wolfendale. "Gamma rays and the origin of cosmic rays." Advances in Space Research 9, no. 12 (January 1989): 129–41. http://dx.doi.org/10.1016/0273-1177(89)90320-7.

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6

Levinson, Amir. "Probing Cosmic Accelerators Using VHE Gamma Rays and UHE Cosmic Rays." Nuclear Physics A 827, no. 1-4 (August 2009): 561c—566c. http://dx.doi.org/10.1016/j.nuclphysa.2009.05.123.

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7

Diehl, Roland, Dieter H. Hartmann, and Nikos Prantzos. "Gamma rays from cosmic radioactivities." Meteoritics & Planetary Science 42, no. 7-8 (August 2007): 1145–57. http://dx.doi.org/10.1111/j.1945-5100.2007.tb00566.x.

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8

Trubnikov, B. A. "Cosmic rays and gamma-ray bursts." Uspekhi Fizicheskih Nauk 167, no. 3 (1997): 345. http://dx.doi.org/10.3367/ufnr.0167.199703k.0345.

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9

Xinyu, Chi, Charles Dahanayake, Jerzy Wdowczyk, and Arnold W. Wolfendale. "Cosmic gamma rays from collapsing cosmic strings." Astroparticle Physics 1, no. 2 (March 1993): 239–43. http://dx.doi.org/10.1016/0927-6505(93)90024-8.

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10

INOUE, SUSUMU, MASAHIRO NAGASHIMA, TAKERU K. SUZUKI, and WAKO AOKI. "COSMIC RAYS AND GAMMA-RAYS IN LARGE-SCALE STRUCTURE." Journal of The Korean Astronomical Society 37, no. 5 (December 1, 2004): 447–54. http://dx.doi.org/10.5303/jkas.2004.37.5.447.

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11

TOMOZAWA, YUKIO. "HIGH ENERGY COSMIC RAYS, GAMMA RAYS AND NEUTRINOS FROM AGN." Modern Physics Letters A 23, no. 24 (August 10, 2008): 1991–97. http://dx.doi.org/10.1142/s0217732308027278.

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The author reviews a model for the emission of high energy cosmic rays, gamma-rays and neutrinos from AGN (Active Galactic Nuclei) that he has proposed since 1985. Further discussion of the knee energy phenomenon of the cosmic ray energy spectrum requires the existence of a heavy particle with mass in the knee energy range. A possible method of detecting such a particle in the Pierre Auger Project is suggested. Also presented is a relation between the spectra of neutrinos and gamma-rays emitted from AGN. This relation can be tested by high energy neutrino detectors such as ICECUBE, the Mediterranean Sea Detector and possibly by the Pierre Auger Project.

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12

Prantzos, N., and M. Casse. "Cosmic rays and gamma rays in early galaxian phases and the cosmic gamma-ray background." Astrophysical Journal Supplement Series 92 (June 1994): 575. http://dx.doi.org/10.1086/192018.

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13

Trubnikov, B. A. "Cosmic rays and gamma-ray bursts." Physics-Uspekhi 40, no. 3 (March 31, 1997): 325–31. http://dx.doi.org/10.1070/pu1997v040n03abeh000220.

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14

Wolfendale, A. W., and L. Zhang. "Cosmic gamma rays and molecular clouds." Journal of Physics G: Nuclear and Particle Physics 20, no. 7 (July 1, 1994): 1083–87. http://dx.doi.org/10.1088/0954-3899/20/7/009.

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15

Roland, Diehl. "New insights from cosmic gamma rays." Journal of Physics: Conference Series 703 (April 2016): 012001. http://dx.doi.org/10.1088/1742-6596/703/1/012001.

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16

Diehl, Roland. "Observing cosmic nuclei in gamma rays." Journal of Physics G: Nuclear and Particle Physics 35, no. 1 (December 13, 2007): 014023. http://dx.doi.org/10.1088/0954-3899/35/1/014023.

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17

Young, E. C. M., and K. N. Yu. "Cosmic gamma rays from extragalactic objects." Journal of Physics G: Nuclear Physics 14, no. 5 (May 1988): L115—L121. http://dx.doi.org/10.1088/0305-4616/14/5/009.

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18

Martinez, Manel. "Fundamental physics with cosmic gamma rays." Journal of Physics: Conference Series 171 (June 1, 2009): 012013. http://dx.doi.org/10.1088/1742-6596/171/1/012013.

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19

Meli, A. "Cosmic-Rays and Gamma Ray Bursts." EAS Publications Series 61 (2013): 663–65. http://dx.doi.org/10.1051/eas/1361104.

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20

Vilenkin, Alexander. "Gamma-rays from superconducting cosmic strings." Nature 332, no. 6165 (April 1988): 610–11. http://dx.doi.org/10.1038/332610a0.

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21

Wolfendale, A. W. "Gamma rays and cosmic ray gradiants." Advances in Space Research 13, no. 12 (December 1993): 687–93. http://dx.doi.org/10.1016/0273-1177(93)90180-j.

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22

Sinitsyna, V. G., V. Y. Sinitsyna, and Yu I. Stozhkov. "Galactic Cosmic Rays: The first detection of TeV gamma-rays from Red Dwarfs." EPJ Web of Conferences 208 (2019): 14007. http://dx.doi.org/10.1051/epjconf/201920814007.

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The present point of view on the sources of cosmic rays in Galaxy considers explosions of supernovae as sources of these particles up to energies of 1017 eV. However, the experimental data obtained with Pamela, Fermi, AMS-02 spectrometers requires the existence of nearby sources of cosmic rays at distances less then 1 kpc from the solar system. These sources could explain such experimental data as the growth of the ratio of galactic positrons to electrons with increasing energy, the complex dependence of the exponent of the proton and alpha spectra from the energy of these particles, the appearance of an anomaly component in cosmic rays. We consider active dwarf stars as possible sources of galactic cosmic rays in the energy range up to 1014 eV. These stars produce powerful stellar flares. The generation of high-energy cosmic rays has to be accompanied by high-energy gamma-ray emission. Here we present the SHALON long-term observation data aimed at searching for gamma-ray emission above 800 GeV from active red dwarf stars. The data obtained during more than 10 years observations of the dwarf stars V962 Tau, V780 Tau, V388 Cas and V1589 Cyg were analyzed. The high-energy gamma-ray emission in the TeV energy range, mostly of the flaring type from the sources mentioned above, was detected. This result confirms that active dwarf stars are also the sources of high-energy galactic cosmic rays.

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23

Brose, R., M. Pohl, I. Sushch, O. Petruk, and T. Kuzyo. "Cosmic-ray acceleration and escape from post-adiabatic supernova remnants." Astronomy & Astrophysics 634 (February 2020): A59. http://dx.doi.org/10.1051/0004-6361/201936567.

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Context. Supernova remnants are known to accelerate cosmic rays on account of their nonthermal emission of radio waves, X-rays, and gamma rays. Although there are many models for the acceleration of cosmic rays in supernova remnants, the escape of cosmic rays from these sources has not yet been adequately studied. Aims. We aim to use our time-dependent acceleration code RATPaC to study the acceleration of cosmic rays and their escape in post-adiabatic supernova remnants and calculate the subsequent gamma-ray emission from inverse-Compton scattering and Pion decay. Methods. We performed spherically symmetric 1D simulations in which we simultaneously solved the transport equations for cosmic rays, magnetic turbulence, and the hydrodynamical flow of the thermal plasma in a volume large enough to keep all cosmic rays in the simulation. The transport equations for cosmic rays and magnetic turbulence were coupled via the cosmic-ray gradient and the spatial diffusion coefficient of the cosmic rays, while the cosmic-ray feedback onto the shock structure can be ignored. Our simulations span 100 000 years, thus covering the free-expansion, the Sedov–Taylor, and the beginning of the post-adiabatic phase of the remnant’s evolution. Results. At later stages of the evolution, cosmic rays over a wide range of energy can reside outside of the remnant, creating spectra that are softer than predicted by standard diffusive shock acceleration, and feature breaks in the 10 − 100 GeV-range. The total spectrum of cosmic rays released into the interstellar medium has a spectral index of s ≈ 2.4 above roughly 10 GeV which is close to that required by Galactic propagation models. We further find the gamma-ray luminosity to peak around an age of 4000 years for inverse-Compton-dominated high-energy emission. Remnants expanding in low-density media generally emit more inverse-Compton radiation, matching the fact that the brightest known supernova remnants – RCW86, Vela Jr., HESS J1731−347 and RX J1713.7−3946 – are all expanding in low density environments.

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24

Gabici, Stefano. "Interaction of escaping cosmic rays with molecular clouds." Proceedings of the International Astronomical Union 9, S296 (January 2013): 320–27. http://dx.doi.org/10.1017/s1743921313009654.

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AbstractThe study of the gamma–ray radiation produced by cosmic rays that escape their accelerators is of paramount importance for (at least) two reasons: first, the detection of those gamma–ray photons can serve to identify the sources of cosmic rays and, second, the characteristics of that radiation give us constraints on the way in which cosmic rays propagate in the interstellar medium. This paper reviews the present status of the field.

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25

Petrukhin, A. A., and S. Yu Matveev. "Gamma-Rays from magellanic clouds and origin of cosmic rays." Bulletin of the Russian Academy of Sciences: Physics 73, no. 5 (May 2009): 584–87. http://dx.doi.org/10.3103/s1062873809050153.

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26

Clayton, Donald D., and Liping Jin. "Gamma Rays, Cosmic Rays, and Extinct Radioactivity in Molecular Clouds." Astrophysical Journal 451 (October 1995): 681. http://dx.doi.org/10.1086/176254.

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27

Orlando, Elena. "Cosmic rays, gamma rays and synchrotron radiation from the Galaxy." Journal of Physics: Conference Series 375, no. 5 (July 30, 2012): 052025. http://dx.doi.org/10.1088/1742-6596/375/1/052025.

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28

Krennrich, Frank. "TeV GAMMA RAYS: OBSERVATIONS VERSUS EXPECTATIONS & THEORY." Acta Polytechnica 53, A (December 18, 2013): 635–40. http://dx.doi.org/10.14311/ap.2013.53.0635.

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The scope of this paper is to discuss two important questions relevant for TeV γ-ray astronomy; the pursuit to reveal the origin of cosmic rays in our galaxy, and the opacity of the universe in γ-rays. The origin of cosmic rays stipulated the field of TeV astronomy in the first place, and led to the development of the atmospheric Cherenkov technique; significant progress has been made in the last decade through the detection of several supernova remnants, the primary suspects for harboring the acceleration sites of cosmic rays. TeV γ-rays propagate mostly unhindered through the galactic plane, making them excellent probes of processes in SNRs and other galactic sources. Key results related to the SNR origin of cosmic rays are discussed. TeV γ-ray spectra from extragalactic sources experience significant absorption when traversing cosmological distances. The opacity of the universe to γ-rays above 10 GeV progressively increases with energy and redshift; the reason lies in their pair production with ambient soft photons from the extragalactic background light (EBL). While this limits the γ-ray horizon, it offers the opportunity to gain information about cosmology, i.e. the EBL intensity, physical conditions in intergalactic space, and potentially new interaction processes. Results and implications pertaining to the EBL are given.

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29

DOMAINKO, WILFRIED, DALIBOR NEDBAL, JAMES A. HINTON, and OLIVIER MARTINEAU-HUYNH. "NEW RESULTS FROM H.E.S.S. OBSERVATIONS OF GALAXY CLUSTERS." International Journal of Modern Physics D 18, no. 10 (October 2009): 1627–31. http://dx.doi.org/10.1142/s021827180901545x.

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Clusters of galaxies are believed to contain a significant population of cosmic rays. From the radio and probably hard X-ray bands it is known that clusters are the spatially most extended emitters of non-thermal radiation in the Universe. Due to their content of cosmic rays, galaxy clusters are also potential sources of VHE (> 100 GeV) gamma rays. Recently, the massive, nearby cluster Abell 85 has been observed with the H.E.S.S. experiment in VHE gamma rays with a very deep exposure as part of an ongoing campaign. No significant gamma-ray signal has been found at the position of the cluster. The non-detection of this object with H.E.S.S. constrains the total energy of cosmic rays in this system. For a hard spectral index of the cosmic rays of -2.1 and if the cosmic-ray energy density follows the large scale gas density profile, the limit on the fraction of energy in these non-thermal particles with respect to the total thermal energy of the intra-cluster medium is 8% for this particular cluster. This value is at the lower bounds of model predictions.

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30

RAZZAQUE, SOEBUR, PETER MÉSZÁROS, and ELI WAXMAN. "DETECTING GAMMA-RAY BURSTS WITH ULTRA-HIGH ENERGY NEUTRINOS." International Journal of Modern Physics A 20, no. 14 (June 10, 2005): 3099–101. http://dx.doi.org/10.1142/s0217751x0502584x.

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Gamma-ray bursts are candidate sources of ultra-high energy cosmic rays and neutrinos. While cosmic rays are scattered in the intervening magnetic field, neutrinos point back to their sources being charge neutral and make neutrino astronomy possible. Detection of ultrahigh energy neutrinos by future experiments such as ANITA, ANTARES, Ice-Cube and RICE can provide useful information such as particle acceleration, radiation mechanism and magnetic field about the sources and their progenitors. Detection of ultrahigh energy neutrinos which point back to their sources may establish gamma-ray bursts as the sources of GZK cosmic rays.

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31

STANEV, TODOR. "ULTRA HIGH ENERGY COSMIC RAYS: ORIGIN AND PROPAGATION." Modern Physics Letters A 25, no. 18 (June 14, 2010): 1467–81. http://dx.doi.org/10.1142/s0217732310033530.

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We introduce the highest energy cosmic rays and briefly review the powerful astrophysical objects where they could be accelerated. We then introduce the interactions of different cosmic ray particles with the photon fields of the Universe and the formation of the cosmic ray spectra observed at Earth. The last topic is the production of secondary gamma rays and neutrinos in the interactions of the ultrahigh energy cosmic rays.

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32

Zhou Da-zhuang and K. K. Tang. "Cosmic ray and hydrogen distributions and cosmic gamma — rays." Chinese Astronomy and Astrophysics 15, no. 4 (December 1991): 416–22. http://dx.doi.org/10.1016/0275-1062(91)90042-v.

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33

Cesarsky, Catherine J. "High Energy Processes in the Interstellar Medium." Highlights of Astronomy 9 (1992): 87–92. http://dx.doi.org/10.1017/s1539299600008777.

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AbstractThe relationship between high energy phenomena and the interstellar medium is wide. I had to make a selection, and only cover a few aspects: cosmic rays, gamma rays, correlation between radio synchrotron and infra red emission and its influence on cosmic rays; and finally some new observational results.

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34

HALZEN, FRANCIS. "THE HIGHEST ENERGY COSMIC RAYS, GAMMA-RAYS AND NEUTRINOS: FACTS, FANCY AND RESOLUTION." International Journal of Modern Physics A 17, no. 24 (September 30, 2002): 3432–45. http://dx.doi.org/10.1142/s0217751x02012831.

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Although cosmic rays were discovered 90 years ago, we do not know how and where they are accelerated. There is compelling evidence that the highest energy cosmic rays are extra-galactic — they cannot be contained by our galaxy's magnetic field anyway because their gyroradius exceeds its dimensions. Elementary elementary-particle physics dictates a universal upper limit on their energy of 5 × 1019 eV, the so-called Greisen-Kuzmin-Zatsepin cutoff; however, particles in excess of this energy have been observed, adding one more puzzle to the cosmic ray mystery. Mystery is nonetheless fertile ground for progress: we will review the facts and mention some very speculative interpretations. There is indeed a realistic hope that the oldest problem in astronomy will be resolved soon by ambitious experimentation: air shower arrays of 104 km2 area, arrays of air Cerenkov detectors and kilometer-scale neutrino observatories.

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35

Bednarek, W. "Gamma-rays and cosmic rays from a pulsar in Cygnus OB2." Monthly Notices of the Royal Astronomical Society 345, no. 3 (November 2003): 847–53. http://dx.doi.org/10.1046/j.1365-8711.2003.06997.x.

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36

Atoyan, Armen, and Charles D. Dermer. "Gamma Rays from Ultra-High-Energy Cosmic Rays in Cygnus A." Astrophysical Journal 687, no. 2 (October 3, 2008): L75—L78. http://dx.doi.org/10.1086/593202.

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37

Gavish, Eyal, and David Eichler. "ON ULTRA-HIGH-ENERGY COSMIC RAYS AND THEIR RESULTANT GAMMA-RAYS." Astrophysical Journal 822, no. 1 (May 5, 2016): 56. http://dx.doi.org/10.3847/0004-637x/822/1/56.

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38

BRECHER, K., and G. CHANMUGAM. "Ultrahigh Energy Gamma Rays and Cosmic Rays from Accreting Degenerate Stars." Annals of the New York Academy of Sciences 470, no. 1 Twelfth Texas (May 1986): 365. http://dx.doi.org/10.1111/j.1749-6632.1986.tb47991.x.

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39

Ulmer, Andrew. "Gamma rays from grazing incidence cosmic rays in the earth's atmosphere." Astrophysical Journal 429 (July 1994): L95. http://dx.doi.org/10.1086/187422.

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40

Waxman, Eli. "Gamma-ray bursts, cosmic-rays and neutrinos." Nuclear Physics B - Proceedings Supplements 87, no. 1-3 (June 2000): 345–54. http://dx.doi.org/10.1016/s0920-5632(00)00697-6.

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41

Kifune, Tadashi. "VHE Gamma-ray Astronomy and Cosmic Rays." Journal of the Physical Society of Japan 77, Suppl.B (January 2, 2008): 36–40. http://dx.doi.org/10.1143/jpsjs.77sb.36.

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42

Agaronyan, F. A., �. A. Mamidzhanyan, and S. I. Nikol'skii. "Primary cosmic gamma rays of ultrahigh energies." Astrophysics 31, no. 1 (1990): 534–48. http://dx.doi.org/10.1007/bf01004403.

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43

Young, E. C. M., and K. N. Yu. "Cosmic gamma rays from active galactic nuclei." Vistas in Astronomy 31 (1988): 579–83. http://dx.doi.org/10.1016/0083-6656(88)90270-x.

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44

Bhattacharjee, Pijushpani, and Nayantara Gupta. "Ultra-high energy cosmic rays and prompt TeV gamma rays from gamma ray bursts." Pramana 62, no. 3 (March 2004): 789–92. http://dx.doi.org/10.1007/bf02705371.

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45

Martineau-Huynh, Olivier. "The GRAND project and GRANDProto300 experiment." EPJ Web of Conferences 210 (2019): 06007. http://dx.doi.org/10.1051/epjconf/201921006007.

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The Giant Array for Neutrino Detection (GRAND) is a proposal for a giant observatory of ultra-high energy cosmic particles (neutrinos, cosmic rays and gamma rays). It will be composed of twenty subarrays of 10 000 antennas each, totaling a detection area of 200 000 km2. GRAND will reach unprecedented sensitivity to neutrinos allowing to detect cosmogenic neutrinos while its sub-degree angular resolution will also make it possible to hunt for point sources and possibly start neutrino astronomy. Combined with its gigantic exposure to ultra-high energy cosmic rays and gamma rays, GRAND will be a powerful tool to solve the century-long mistery of the nature and origin of the particles with highest energy in the Universe. On the path to GRAND, the GRANDProto300 experiment will be deployed in 2020 over a total area of 200 km2. It primarly aims at validating the detection concept of GRAND, but also proposes a rich science program centered on a precise and complete measurement of the air showers initiated by cosmic rays with energies between 1016.5 and 1018 eV, a range where we expect to observe the transition between the Galactic and extra-galactic origin of cosmic rays.

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46

Hermsen, W., and J. B. G. M. Bloemen. "High-energy gamma rays and the large-scale distribution of gas and cosmic rays." Symposium - International Astronomical Union 106 (1985): 213–18. http://dx.doi.org/10.1017/s0074180900242484.

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The COS-B gamma-ray survey is compared with 12CO and HI surveys in a region containing the Orion complex and in the outer Galaxy. The observed gamma-ray intensities in the Orion region (100 MeV<E<5 GeV) can be ascribed to the interaction of uniformly distributed cosmic rays with the interstellar gas. Calibration of the ratio between H2 column-density and integrated CO line intensity resulted in the value: (3.0±0.7)x102 0 molecules cm-2K -1km -1s. In the outer Galaxy HI column-density maps in three galacto-centric distance ranges are used in combination with COS-B gamma-ray data to determine the radial distribution of the gamma-ray emissivity. A steep negative gradient of the emissivity for the 70 MeV-150 MeV range and an approximately constant (within ~20%) emissivity for the 300 MeV-5 GeV range is found. The result is interpreted as a strong decrease in the cosmic-ray electron density and a near constancy of the nuclear component.

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47

Prodanović, Tijana, and Brian D. Fields. "Lithium-6 and Gamma-Rays: Constraints on Primordial Lithium, Cosmic Rays and Cosmic Star Formation." Nuclear Physics A 758 (July 2005): 799–802. http://dx.doi.org/10.1016/j.nuclphysa.2005.05.162.

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48

Tanimori, Toru. "Detection of TeV Gamma Rays from SN1006." Symposium - International Astronomical Union 188 (1998): 121–24. http://dx.doi.org/10.1017/s0074180900114585.

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In spite of the recent progress of high energy gamma-ray astronomy, there still remains quite unclear and important problem about the origin of cosmic rays. Supernova remnants (SNRs) are the favoured site for cosmic rays up to 1016 eV, as they satisfy the requirements such as an energy input rate. But direct supporting evidence is sparse. Recently intense non-thermal X-ray emission from the rims of the Type Ia SNR SN1006 (G327.6+14.6) has been observed by ASCA (Koyama et al. 1995)and ROSAT (Willingale et al. 1996), which is considered, by attributing the emission to synchrotron radiation, to be strong evidence of shock acceleration of high energy electrons up to ~100 TeV. If so, TeV gamma rays would also be expected from inverse Compton scattering (IC) of low energy photons (mostly attributable to the 2.7 K cosmic background photons) by these electrons. By assuming the magnetic field strength (B) in the emission region of the SNR, several theorists (Pohl 1996; Mastichiadis 1996; Mastichiadis & de Jager 1996; Yoshida & Yanagita 1997) calculated the expected spectra of TeV gamma rays using the observed radio/X-ray spectra. Observation of TeV gamma rays would thus provide not only the further direct evidence of the existence of very high energy electrons but also the another important information such as the strength of the magnetic field and diffusion coefficient of the shock acceleration. With this motivation, SN1006 was observed by the CANGAROO imaging air Cerenkov telescope in 1996 March and June, also 1997 March and April.

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49

Bednarek, W., J. Pabich, and T. Sobczak. "Gamma-rays, neutrinos and cosmic rays from dense regions in open clusters." Nuclear Physics B - Proceedings Supplements 256-257 (November 2014): 107–16. http://dx.doi.org/10.1016/j.nuclphysbps.2014.10.013.

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50

Chi, X., and A. W. Wolfendale. "Gamma rays from the magellanic clouds and the origin of cosmic rays." Journal of Physics G: Nuclear and Particle Physics 19, no. 5 (May 1, 1993): 795–804. http://dx.doi.org/10.1088/0954-3899/19/5/013.

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