Skip to main content
SpringerLink
Log in

Delay between the circularly polarized components in fine structures during solar type IV events

  • Published:
Solar Physics Aims and scope Submit manuscript

Abstract

We analyzed intermediately polarized (20–80%) fine structures (pulsations, sudden reductions, fiber bursts and zebras) that were recorded in type IV events. The mean polarization degree was practically the same for all the fine structures recorded in an interval lasting a few minutes and it was similar to the polarization of the continuum. A detailed analysis during the evolution of single structures reveals changes in polarization (in particular an ‘undulation’ at flux density minima) even stronger than 20%. They were caused by a delay, up to 0.1 s, between the two circularly polarized components. The weaker polarimetric component was delayed in 2 sets and the stronger one in 1 set. In the event of April 24, 1985 different types of fine structures were sporadically detected in more than one hour long time interval. Short delays of the stronger or of the weaker component were sometimes observed.

The events characterized by fine structures are generally totally polarized in the ordinary mode. We assume that this holds also for the phenomena studied here. The observed intermediate polarization therefore requires a depolarization due to propagation effects. We discuss the mode coupling and the reflection of the original radio signal that could also generate the delay of the weaker and the stronger component respectively. The possibility of polarization variation due to the change of the angle between the direction of the propagation and the magnetic field in a quasi-transversal region and in a low intensity magnetic field in a current sheet is also given.

This is a preview of subscription content, log in via an institution to check access.

Access this article

Log in via an institution

Price excludes VAT (USA)
Tax calculation will be finalised during checkout.

Instant access to the full article PDF.

Institutional subscriptions

Similar content being viewed by others

References

  • Aurass, H., Chernov, G. P., Karlický, M., Kurths, J., and Mann, G.: 1987,Solar Phys. 112, 347.

    Google Scholar 

  • Bernold, T.: 1980,Astron. Astrophys. Suppl. Ser. 42, 43.

    Google Scholar 

  • Benz, A.: 1993,Plasma Astrophysics, Kinetic Processes in Solar and Stellar Coronae, Kluwer Academic Publishers, Dordrecht, Holland.

    Google Scholar 

  • Chernov, G. P.: 1976,Soviet Astron. 20, 75.

    Google Scholar 

  • Chernov, G. P.: 1990,Kinematika i Fizika Nebesnyh Tel 6, 27.

    Google Scholar 

  • Chernov, G. P. and Zlobec, P.: 1994,Seventh European Meeting on Solar Physics ‘Advances in Solar Physics’, special publication Catania Astrophysical Observatory, p. 177.

  • Chernov, G. P., Korolev, O. S., and Markeev, A. K.: 1975,Solar Phys. 44, 435

    Google Scholar 

  • Chernov, G. P., Klein, K.-L., Zlobec, P., and Aurass, H.: 1994,Solar Phys. 155, 373.

    Google Scholar 

  • Cyr, O. C. V and Burkepile, J. T.: 1990,A Catalog of Mass Ejections Observed by the SMM Coronograph, NAO, NCAR, Boulder.

    Google Scholar 

  • Cohen, H. M.: 1960,Astrophys. J. 131, 665.

    Google Scholar 

  • Comari, M.: 1994, private communication.

  • Hanasz, J., Schreiber, R., and Aksenov, V. I.: 1980,Astron. Astrophys. 91, 311.

    Google Scholar 

  • Hayes, L. M.: 1985,Australian J. Phys. 38, 705.

    Google Scholar 

  • Kattenberg, A. and Van der Burg, G.: 1982,Solar Phys. 77, 231.

    Google Scholar 

  • Klein, K.-L.: 1995, private communication.

  • Kuijpers, J.: 1980, in M. R. Kundu and T. E. Gergely (eds.), ‘Radio Physics of the Sun’,IAU Symp. 86, 341.

    Google Scholar 

  • Markeev, A. K., Fomichev, V. V., Chernov, G. P., and Chertok, I. M.: 1976,Soviet Astron. 19, 598.

    Google Scholar 

  • Melrose, D. B.: 1980,Plasma Astrophysics, Vol. 2,Astrophysical Applications, Gordon and Breach Sci. Publ., New York.

    Google Scholar 

  • Melrose, D. B.: 1989,Solar Phys. 119, 143.

    Google Scholar 

  • Melrose, D. B. and Robinson, P. A.: 1994,Proc. Astron. Soc. Australia 11, 16.

    Google Scholar 

  • Nonino, M., Messerotti, M., Zlobec, P., Comari, M., and Fornasari, L.: 1987,Report UAG 96, 97.

    Google Scholar 

  • Slottje, C.: 1981,Atlas of Fine Structures of Dynamic Spectra of Solar Type IV and Some Type II Radio Bursts, Dwingeloo.

  • Wentzel, D., Zlobec, P., and Messerotti, M.:Astron. Astrophys. 159, 40.

  • White, S. M., Thejappa, G., and Kundu, M. R.: 1992,Solar Phys. 138, 163.

    Google Scholar 

  • Zheleznyakov, V. V.: 1970,Radio Emission of the Sun and Planets, Pergamon Press, Oxford.

    Google Scholar 

  • Zheleznyakov, V. V.: 1977,Electromagnetic Waves in Cosmic Plasmas-Generation and Propagation, Nauka, Moscow (in Russian).

  • Zheleznyakov, V. V. and Zlotnik, E. Ya.: 1988,Soviet Astron. Letters 14, 195.

    Google Scholar 

  • Zlobec, P., Li, H. W., Messerotti, M., Comari, M., and Barry, M. B.: 1987,Solar Phys. 114, 375.

    Google Scholar 

  • Zlotnik, E. Ya.: 1977,Soviet Astron. 21, 744.

    Google Scholar 

Download references

Author information

Authors and Affiliations

  1. IZMIRAN, 142092, Troitsk, Moscow Region, Russia

    G. P. Chernov

  2. Trieste Astronomical Observatory, 34131, Trieste, Italy

    P. Zlobec

Authors
  1. G. P. Chernov
    View author publications

    You can also search for this author in PubMed Google Scholar

  2. P. Zlobec
    View author publications

    You can also search for this author in PubMed Google Scholar

Rights and permissions

Reprints and permissions

About this article

Cite this article

Chernov, G.P., Zlobec, P. Delay between the circularly polarized components in fine structures during solar type IV events. Sol Phys 160, 79–96 (1995). https://doi.org/10.1007/BF00679097

Download citation

  • Received:

  • Revised:

  • Issue Date:

  • DOI: https://doi.org/10.1007/BF00679097

Keywords

Search

Navigation