Astronomical School’s Report, 2013, Volume 9, Issue 1, Pages 15–19

https://doi.org/10.18372/2411-6602.09.1015
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UDC 523.982+52-337

To the problem of temporal changes of magnetic fields in small-scale magnetic fluxtubes during 11-years cycle of solar activity

Lozitsky V.G.

Astronomical Observatory, Kyiv Shevchenko National University, Ukraine

Abstract

We critical analyze paper by V.A.Kotov [1], what contains the important results of observations of total magnetic field of the Sun observed in Crimea astrophysical observatory in FeI 5247.1 and 5250.2Å lines during 2001–2011. A conclusion is argued that obtained observational data indicate the true magnetic field changes in small-scale flux tubes. Likely, magnetic field strengths in such fluxtubes change with solar cycle phase in the following way: maximum field values arise nearly the minimum of sunspots number, whereas minimum one – 2–4 years after peak of solar cycle. From comparison of named changes with visual measurements of magnetic fields in sunspots [2, 3] follows that magnetic field strength in large sunspots (22–44 Mm) and spatially unresolved fluxtubes change in opposite phase with difference no more than one year.

Keywords: Sun; magnetic fields; sunspots; fluxtubes

References

  1. Kotov V.A. (2012). Zagadka izmereny obschego magnitnogo polya Solntsa. Izvestiya Krym. Astrofiz. Observatorii., 108(1), 35–47.
  2. Lozitskaya N.I. (2010). Vekovye variatsii magnitnykh poley solnechnykh pyaten: sopostavlenie razlichnykh indeksov. Kosmіchna nauka і tekhnologіya, 16(4), 30–36. https://doi.org/10.15407/knit2010.04.030
  3. Lozitskaya N.I., Malaschuk V.F., Stepanyan N.N. (2011). Nachalo 24-go tsikla solnechnoy aktivnosti po dannym izmereny magnitnykh poley solnechnykh pyaten. Izvestiya Krym. astrofiz. observatorii., 107(1. –– S.244–245).
  4. Lozitsky V.G., Tsap T.T. (1989). Empiricheskaya model’ melkomasshtabnogo magnitnogo elementa spokoynoy oblasti Solntsa. Kinematika i fizika nebes. tel., 5(1), 50–58.
  5. Lozyts’kyy V.H., Tsap T.T., Osyka O.B. (2007). Porivnial’na di’ahnostyka tonkostrukturnykh mahnitnykh poliv u soniachnomu spalakhu ta spokiynykh oblastiakh na Sontsi. Visnyk Kyyivs’koho universytetu imeni Tarasa Shevchenka. Astronomiya., 17–20.
  6. Rachkovsky D.N., Tsap T.T. (1985). Izuchenie magnitnykh poley metodom otnosheniya izmerennykh napryazhennostey v liniyakh vne aktivnykh oblastey. Izv. Krym. astrofiz. observatorii., 71, 79–87.
  7. Lozitska N., Lozitskij V. (1994). Small-scale magnetic fluxtube diagnostics in a solar flare. Solar Physics, 151(2), 319–331. https://doi.org/10.1007/bf00679078
  8. Rachkovsky D.N., Tsap T.T., Lozitsky V.G. (2005). Small-scale magnetic field diagnostics outside sunspots: comparison of different methods. Journ. of Astrophys. and Astronomy., 26(4), 435–445. https://doi.org/10.1007/bf02702449
  9. Stenflo J.O. (1973). Magnetic-field structure of the photospheric network. Solar Physics, 32(1), 41–63. https://doi.org/10.1007/bf00152728
  10. Stenflo J.O. (1989). Small-scale magnetic structures on the Sun. Astron. Astrophys. Rev., 1, 3–48.
  11. Wiehr E. (1978). A unique magnetic field range for non-spot solar magnetic regions. Astron. and Astrophys., 69(2), 279–284.

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