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      Permanent link:
      https://www.ias.ac.in/article/fulltext/joaa/026/04/0435-0445

    • Keywords

       

      Sun; magnetic fluxtubes; kG magnetic fields

    • Abstract

       

      We analyse different observational data related to the problem of intrinsic magnetic field strength in small-scale fluxtubes outside sunspots. We conclude that the kG range of fluxtube fields follows from not only classical line ratio method, but also from other old and new techniques. For the quiet regions on the Sun, the most probable mode of such fields has a magnetic field strength of 1.2–1.5 kG assuming the rectangular field profile. To best interpret the observations, a weak background field between fluxtubes should be assumed, and its magnetic field strength is expected to increase with the filling factor of fluxtubes. The alternative point of view about subkilogauss fluxtube fields is critically examined, and possible sources of different conclusions are presented.

    • Author Affiliations

       

      D. N. Rachkovsky1 T. T. Tsap1 V. G. Lozitsky2

      1. Crimean Astrophysical Observatory, Nauchny, Crimea - UA-98409, Ukraine
      2. Kyiv University Astronomical Observatory, Observatorna St. 3, Kyiv - UA-04053, Ukraine

    • Dates

       
      Published
      December 2005
      Manuscript received
      28 December 2004
      Accepted
      28 November 2005

  • Journal of Astrophysics and Astronomy | News

    • Continuous Article Publication

      Posted on January 27, 2016

      Since January 2016, the Journal of Astrophysics and Astronomy has moved to Continuous Article Publishing (CAP) mode. This means that each accepted article is being published immediately online with DOI and article citation ID with starting page number 1. Articles are also visible in Web of Science immediately. All these have helped shorten the publication time and have improved the visibility of the articles.

    • Editorial Note on Continuous Article Publication

      Posted on July 25, 2019

      Click here for Editorial Note on CAP Mode

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