@InProceedings{SodréSantWrasFern:2018:AnPhMa,
               author = "Sodr{\'e}, Z. A. L. and Santos, J. C. and Wrasse, Cristiano Max 
                         and Fernandes, F. C. R.",
          affiliation = "{} and {} and {Instituto Nacional de Pesquisas Espaciais (INPE)}",
                title = "Analysis of photospheric magnetic fields reorganization and metric 
                         noise storm recorded in august 12, 2012",
                 year = "2018",
         organization = "Latin American Conference on Space Geophysics, 11. (COLAGE)",
             abstract = "Radio Noise Storms (RNS), also named as type I emissions, last 
                         from a few hours to several days. They are associated to the 
                         evolution of active regions (AR), as well as the occurrence of 
                         solar flares. However, recent studies show that RNS are not 
                         connect directly to flares, but mostly to reorganization of the 
                         magnetic fields of active regions. Considering that type I 
                         emissions is generated by the fundamental plasma emission, the 
                         reorganization of the scales in active region magnetic 
                         configuration was investigated as the possible process for 
                         maintenance of the RNS. On August 12, 2012, the BLEN7M 
                         (Switzerland) spectrograph of e-CALLISTO network, registered a RNS 
                         (14:08 - 15:35 UT); and the NOAA 11542 was in the centre of the 
                         solar disc, without the occurrence of intense flare (admitting 
                         only flares A and B Classes). The time evolution of the magnetic 
                         power spectra was used for identify in which length scales the 
                         reorganization of the photospheric magnetic fields occurs. The 481 
                         line-ofsight (LOS) magnetograms recorded by HMI instrument 
                         (Helioseismic and Magnetic Imager) on board of the SDO (Solar 
                         Dynamics Observatory) were analysed to study the power spectra and 
                         the energy spectra. Here, we present the preliminar results of 
                         this analysis. The spectrum index, \α;, was -2.29, greater 
                         than -5/3 (the Kolmogorovs index), indicating the possibility of 
                         energy transfer from small to large structures. Furthermore, 
                         increasing the value of the power law index causes a 
                         redistribution of energy along the power spectra. The 
                         reorganization of the photospheric magnetic fields occurred at 
                         values corresponding to scales greater than \∼ 20.9 Mm 
                         (\∼ 0.03 Rs), above the photosphere, beginning soon after 
                         the beginning of RNS (\∼ 10 min) and continuing after the 
                         end of that (\∼ 1h30min.). The time evolution of the 
                         dissipation spectra revealed that the power increased before the 
                         starting of the RNS for a wide range of wave numbers. These 
                         results will be presented.",
  conference-location = "Buenos Aires, Argentina",
      conference-year = "16-20 abr.",
             language = "en",
        urlaccessdate = "27 abr. 2024"
}