SOLARNET Conference: The Many Scales of the Magnetic Sun

Solar pores are penumbra-lacking magnetic features that mark two important transitions in the spectrum of magnetohydrodynamic processes: (1) the magnetic field becomes sufficiently strong to suppress the convective energy transport and (2) at some critical point some pores develop a penumbra and become sunspots. Pores are rarely encountered in quiet-Sun images (Verma & Denker 2014, Astron. Astrophys. 563, A112) and only about 10% of pores exist in isolation. In general, pores do not exhibit a circular shape. Smaller pores tend to be more circular, and their boundaries are less corrugated. Several scientific questions related to pores need answers such as: Are different mechanisms responsible for the formation of isolated, quiet-Sun pores and pores, which are part of active regions? Do isolated pores ever aggregate sufficient flux to form a penumbra? I present the high-spatial and temporal resolution observations of two pores taken at the GREGOR solar telescope using the High-resolution Fast Imager (HiFI) and Integral Field Unit (IFU) of the GREGOR Infrared Spectrograph (GRIS). One is isolated and the other is part of a decaying active region. HiFI images are taken in G-band and blue continuum, whereas the GRIS IFU data are in the 1083.0 nm spectral range containing photospheric and chromospheric spectral lines. For the isolated pore, we have 20 mosaics whereas 30 mosaics are available for the other pore. The aim is to compare the difference in the 3-dimensional velocity and magnetic field structure of these two pores. Furthermore, the application of the machine learning algorithm t-SNE will reveal if there are any unique Stokes profiles associated with either of these pores.