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Shock Waves

  • Lawrence H. Aller
Chapter
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Part of the Astrophysics and Space Science Library book series (ASSL, volume 112)

Abstract

Early successes of the theory of stellar radiative excitation of gaseous nebulae led to an expectation that the emission from all galactic gaseous nebulae could be explained in this way. One well-known object which resisted this interpretation was the Network Nebula in Cygnus, now recognized as a supernova remnant. Already by the 1930s intensive searches for an illuminating star had proven fruitless. No plausible candidate could be found and the suggestion that such an object might be hidden behind a dark cloud is not substantiated by star counts in the region.

Keywords

Shock Wave Shock Front Interstellar Medium Supernova Remnant Shock Velocity 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

  1. The classical reference on shock waves is Supersonic Flow and Shock Waves, Courant, R., and Friedrichs, K.O., 1948, New York, Interscience.zbMATHGoogle Scholar

Our discussion is hased largely on basic papers by:

  1. Cox, D.P. 1972, Ap. J., 178, 143, 169.ADSCrossRefGoogle Scholar
  2. Raymond, J.C. 1979, Ap. J. Suppl., 39, 1.ADSCrossRefGoogle Scholar
  3. See also Spitzer, L. 1968, Diffuse Matter in Space, New York: Interscience.Google Scholar
  4. That the excitation of the Network Nebula was probably caused by a shock wave of velocity ~ 100 km/sec passing through the interstellar medium was suggested by J. Oort (1946, M.N.R.A.S., 106, 159). Extensive optical observational studies by E. Hubble (1937), J.W. Chamberlain (1953, Ap. J., 117, 399), R. Minkowski (1958, Rev. Mod. Phys., 30, 1048; 1968. Stars and Stellar Systems, 9), D.E. Harris (1962, Ap. J., 135, 661), S.B. Pikel’ner (1954, Crimea Obs. Publ., 12, 93), R.A. Parker (1967, Ap. J., 139, 493; 149, 363; 1969, 155, 359), A. Poveda (1965, Bol. Tonanzintla y Tacubaya, 27, 49), and J. Miller (1974, Ap. J., 189, 239) have been extended to X-ray, radio and ultraviolet regions; see, e.g., P. Benvenuti, S. D’Odorico and M.A. Dopita (1979, Nature, 277, 99), S. Rappaport et_ al. (1974, Ap. J., 194, 329), B.E. Woodgate et al. (1974, Ap. J., 188, L79). For further SNRs see, e.g., D. Osterbrock and R. Dufour (1973, Ap. J., 185, 441), N49 in LMC, D.E. Osterbrock and R. Costero (1973, Ap. J., 184, L71). Other references may be found in papers cited below.Google Scholar

For a review on interstellar shock waves, see:

  1. Shull, J.M., and McKee, C.F. 1979, Ap. J., 227, 131.ADSCrossRefGoogle Scholar
  2. McKee, CF., and Hollenback, D.J. 1980, Ann. Rev. Astr. Astrophys., 18, 219, and references therein.ADSCrossRefGoogle Scholar

Attempts to derive chemical element abundances in SNRs have been made, for example, by:

  1. Dopita, M.A. 1976, Ap. J., 209, 395ADSCrossRefGoogle Scholar
  2. Dopita, M.A.1977, Ap. J. Suppl., 33, 437.ADSCrossRefGoogle Scholar

Supernova remnants have been discussed by many writers. Some useful references are:

  1. Chevalier, R.A. 1977, Ann. Rev. Astr. Astrophys., 15, 175 (Interaction of SNR and interstellar medium).ADSCrossRefGoogle Scholar
  2. Chevalier, R.A., Kirshner, R.P., and Raymond, J.C. 1980, Ap. J., 235, 186 (Optical Emission of a Fast Shock Wave).ADSCrossRefGoogle Scholar

Copyright information

© D. Reidel Publishing Company, Dordrecht, Holland 1984

Authors and Affiliations

  • Lawrence H. Aller
    • 1
  1. 1.University of CaliforniaLos AngelesUSA

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