Advertisement

Solar Physics

, Volume 226, Issue 1, pp 143–151 | Cite as

Callisto – A New Concept for Solar Radio Spectrometers

  • Arnold O. Benz
  • Christian Monstein
  • Hansueli Meyer
Article

Abstract

A new radio spectrometer, CALLISTO, is presented. It is a dual-channel frequency-agile receiver based on commercially available consumer electronics. Its major characteristic is the low price for hardware and software, and the short assembly time, both two or more orders of magnitude below existing spectrometers. The instrument is sensitive at the physical limit and extremely stable. The total bandwidth is 825 MHz, and the width of individual channel is 300 kHz. A total of 1000 measurements can be made per second. The spectrometer is well suited for solar low-frequency radio observations pertinent to space weather research. Five instruments of the type were constructed until now and put into operation at several sites, including Bleien (Zurich) and NRAO (USA). First results in the 45–870 MHz range are presented. Some of them were recorded in a preliminary setup during the time of high solar activity in October and November 2003.

Keywords

Solar Activity Physical Limit Assembly Time Space Weather Solar Radio 
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. Bastian, T. S.: 2004, in D. E. Gary and C. U. Keller (eds.), Solar and Space Weather Radiophysics, Kluwer ASSL, p. 47.Google Scholar
  2. Benz, A. O., Messmer, P. and Monstein, C.: 2001, Astr. Astrophys. 366, 326.CrossRefGoogle Scholar
  3. Benz, A. O., Güdel, M., Isliker, H., Miszkowicz, S. and Stehling, W.: 1991, Solar Phys. 133, 385.CrossRefGoogle Scholar
  4. Cole, T. W., Stewart, R. T. and Milne, D. K.: 1978, Astr. Astrophys. 67, 277.Google Scholar
  5. Dumas, G., Caroubalos, C. and Bougeret, J. L.: 1982, Solar Phys. 81, 383.CrossRefGoogle Scholar
  6. Güdel, M. and Benz, A. O.: 1988, Astr. Astrophys. Sup. 75, 243.Google Scholar
  7. Isliker, H. and Benz, A. O.: 1994, Astr. Astrophys. Sup. 104, 145.Google Scholar
  8. Jiřička, K., Karlický, M., Kepka, O. and Tlamicha, A.: 1993, Solar Phys. 147, 203.CrossRefGoogle Scholar
  9. Kondo, T., Isobe, T., Igi, S., Watari, S. and Tokumaru, M.: 1995, J. Communications Res. Lab. 42, 111.Google Scholar
  10. Lecacheux, A., Rosolen, C., Davis, M., Bookbinder, J., Bastian, T. S. and Dulk, G. A.: 1993, Astr. Astrophys. 275, 670.Google Scholar
  11. Mann, G., Aurass, H., Voigt, W. and Paschke, J.: 1992, in ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition, 129.Google Scholar
  12. McLean, D. J. and Labrum, N. R.: 1985. Solar Radiophysics, Cambridge University Press, Cambridge, p. 516.Google Scholar
  13. Messmer, P., Benz, A. O. and Monstein, C.: 1999, Solar Phys. 187, 335.CrossRefGoogle Scholar
  14. Perrenoud, M. R.: 1982, Solar Phys. 81, 197.CrossRefGoogle Scholar
  15. Sawant, H. S., et al.: 2001, Solar Phys. 200, 167.CrossRefGoogle Scholar
  16. Smith, D. F. and Benz, A. O.: 1991, Solar Phys. 131, 351.CrossRefGoogle Scholar
  17. Wild, J. P. and McCready, L. L.: 1950, Australian J. Sci. Res. A 3, 541.Google Scholar
  18. Xu, F.-Y., Xu, Z.-C., Huang, G.-I. Yao, Q.-J., Meng, X. and Wu, H.-A.: 2003, Solar Phys. 216, 273.CrossRefGoogle Scholar

Copyright information

© Springer Science + Business Media, Inc. 2005

Authors and Affiliations

  • Arnold O. Benz
    • 1
  • Christian Monstein
    • 1
  • Hansueli Meyer
    • 1
  1. 1.Institute of AstronomyETH ZürichZurichSwitzerland

Personalised recommendations