Advertisement

X-Rays Associated with High Energy Particles

  • Paul Gorenstein

Abstract

A number of recent results in X-ray astronomy, particularly from the Einstein Observatory, are relevant to the acceleration or interaction of high energy particles. X-ray observations of M stars by the Einstein Observatory indicate that their frequent flares include X-ray emission. The correspondence of the flux and duration of M star X-ray flares to those of solar flares can be used to estimate the rate of >200 MeV proton injection into the galaxy. Given the uncertainties, there is no disagreement with the cosmic ray density. Thus, a two stage acceleration process may be viable at least for protons.

Supernova remnants (SNR’s) are characterized by hot, turbulent shock waves with temperatures in excess of 106 K to age 104 years as seen, for example, in the Vela SNR. Thus, SNR’s are good candidates as cosmic ray acceleration sites. X-ray jets due to particle beams are seen to emanate from SS433 and G109.1–1.0, two objects where SNR’s are associated with compact X-ray sources.

Among extragalactic X-ray sources, the radio galaxies, Cen A and M87, have X-ray jet features emanating from their centers. M87 has more extended X-ray lobes in addition. These M87 features are due to synchrotron radiation of very high energy electrons and inverse Compton scattering of moderately high energy electrons against the 2.7K background.

Keywords

Neutron Star Radio Galaxy High Energy Electron Supernova Remnant High Energy Particle 
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.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Becker, R.H., et al., 1980, Ap.J. (Letters), 235 L5.ADSCrossRefGoogle Scholar
  2. Eichler, D., 1979, Ap.J., 229, 419.ADSCrossRefGoogle Scholar
  3. Fabricant, D., Lecar, M., and Gorenstein, P., 1980, Ap.J., 241, 552.ADSCrossRefGoogle Scholar
  4. Feigelson, E., et al., 1979, Ap.J. (Letters), 234, L69.CrossRefGoogle Scholar
  5. Gorenstein, P., Tucker, W.H., and Seward, F., in preparation.Google Scholar
  6. Gregory, P. and Fahlman, G., 1980, Nature, 287, 805.ADSCrossRefGoogle Scholar
  7. Haisch, B.M., et al., 1980, Ap.J. (Letters), 242, L99.ADSCrossRefGoogle Scholar
  8. Lanzerotti, L.O., 1977, article in The Solar Output and Its Variation, O.R. White (ed.), Colorado Associated University Press, Boulder, CO.Google Scholar
  9. Margon, B., 1982, article to appear in Accretion Driven Stellar X-ray Sources, W.H.G. Lewin and E.P.J. van den Heuvel (eds.), Cambridge university Press.Google Scholar
  10. Murray, S.S., et al., 1979, Ap.J. (Letters), 234, L69.ADSCrossRefGoogle Scholar
  11. Rosner, R. and Vaiana, G., 1978, Ap.J., 222, 1104.ADSCrossRefGoogle Scholar
  12. Sargent, W.L.W., et al., 1978, Ap.J., 221, 731.ADSCrossRefGoogle Scholar
  13. Schreier, E., Feigelson, E., and Gorenstein, P., to be submitted to Ap.J.Google Scholar
  14. Seward, F., Grindlay, J., Seaquist, E., and Gilmore, W., 1980, Nature, 281, 806.ADSCrossRefGoogle Scholar
  15. Stern, R.A., Underwood, J.H. and Antiochos, S.K., 1981, I.A.U. Circular No. 3585.Google Scholar
  16. Topka, K.P., 1980, Ph.D. thesis, Harvard university.Google Scholar
  17. Van Speybroeck, et al., 1979, Ap.J. (Letters), 234, L45.ADSCrossRefGoogle Scholar
  18. Young, P.J., et al., 1978, Ap.J., 221, 721.ADSCrossRefGoogle Scholar

Copyright information

© Springer-Verlag Berlin Heidelberg 1969

Authors and Affiliations

  • Paul Gorenstein
    • 1
  1. 1.Harvard/Smithsonian Center for AstrophysicsCambridgeUSA

Personalised recommendations