Long time trends of MBP characteristics
Abstract
The change of Magnetic Bright Points (MBPs) characteristics over time periods of the solar sunspot cycle is studied. MBPs are small-scale solar magnetic field features reaching well beyond kG magnetic field strength and visible in intergranular lines within the solar photosphere. They are very variable and dynamic on time scales of just a few minutes. Due to their strong magnetic field, which resembles in shape the ideal concept of vertical flux tubes, as well as their dynamic behaviour, they are of special interest for wave triggering and propagation processes. On the other hand these small-scale structures appear brighter on the solar photosphere and thus their long time behaviour in respect of number, size, and intensity is of great importance for the total solar irradiance variability and thus also for climate change studies. In the current contribution we want to have a detailed look on exactly these parameters over the time period from end of 2006 until spring 2017 when unfortunately the Hinode SOT/BFI and NFI CCD cameras failed and thus no more data could be taken by the Hinode spacecrafts BFI instrument. The key findings can be summarized as that the number at the disc centre is variable and correlated to the sunspot cycle but shifted in regards to it. Moreover the size distribution of MBPs varies with the cycle indicating that fundamental magneto-convective properties might change on the 11th-year solar-cycle time-period.
- Publication:
-
Central European Astrophysical Bulletin
- Pub Date:
- 2018
- Bibcode:
- 2018CEAB...42...13U
- Keywords:
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- Magnetic Bright Points;
- Solar Cycle;
- magnetic fields;
- Hinode synoptic data