Temporal variations in solar magnetic bright points intensity and plasma parameters

Eclipse on the Coral Sea: Cycle 24 Ascending

物理学;天文学

Jurák, J.^1 ; Utz, D.^2,3 ; Rubio, L. R. Bellot^2

Astronomical Institute, Academy of Sciences, Friova 298, 251 65, Ondejov, Czech Republic^1

Instituto de Astrofísica de Andalucía (CSIC), Apdo. de Correos 3004, E-18080 Granada, Spain^2

IGAM/Institute of Physics, University of Graz, Universitätsplatz 5, A-8010 Graz, Austria^3

关键词: Large amplitude;    Magnetic field strengths;    Maximum intensities;    Plasma parameter;    Selected examples;    Solar atmosphere;    Temporal resolution;    Temporal variation;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/440/1/012032/pdf
DOI  :  10.1088/1742-6596/440/1/012032

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

Magnetic bright points are one of the finest magnetic structures observed in the solar atmosphere. They possibly represent single flux tubes in quiet Sun regions. Their formation is described by the convective collapse model, while the decay phase of these structures is not well characterized yet. We attempt to follow the evolution of a few selected examples of MBPs and to study their changes in brightness and also the variations of plasma parameters during their lifetime. We use data from the Hinode satellite and the Sunrise mission. The G-band observations taken with a cadence of 30 seconds by the Hinode Solar Optical Telescope (SOT) show very fast changes of the maximum intensity of these structures. The complementary spectropolarimetric data, which are used to estimate the plasma parameters, were taken with a cadence of approximately two minutes. The variations of plasma parameters cannot be matched one to one to the changes in intensity due to the different temporal resolution. However, the slow changes of intensity with large amplitude are matched with variations of magnetic field strength and line-of-sight (LOS) velocity. The Sunrise/IMaX data have a temporal resolution of 32 seconds and show fast variations in the line wing intensity. These variations are associated with changes in the magnetic field strength and LOS velocity.