Exploring magnetic field properties at the boundary of solar pores: A comparative study based on SDO-HMI observations

Abstract

The Sun's magnetic fields play an important role in various solar phenomena. Solar pores are regions of intensified magnetic field strength compared to the surrounding photospheric environment, and their study can help us better understand the properties and behaviour of magnetic fields in the Sun. Up to now, there exists only a single study on magnetic field properties at the boundary region of a pore. Therefore, the main goal of this work is to increase the statistics of magnetic properties determining the pore boundary region. We analyse six solar pores using data from the Helioseismic and Magnetic Imager instrument on board the Solar Dynamics Observatory. We apply image processing techniques to extract the relevant features of the solar pores and determine the boundary conditions of the magnetic fields. We find the maximal vertical magnetic field values on the boundaries of the studied solar pores to range from 1400~G to 1600~G, with a standard deviation between 7.8\% and 14.8\%. These values are lower than those reported in the mentioned preceding study. However, this can be explained by differences in spatial resolution as well as the type of data we used. The vertical magnetic field is an important factor in determining the boundary of solar pores, and it plays a more relevant role than the intensity gradient. The obtained information will be useful for future studies on the formation and evolution of magnetic structures of the Sun. Additionally, this study highlights the importance of high spatial resolution data for the purpose of accurately characterising the magnetic properties of solar pores.

arXiv comment9 pages, 7 figures. Accepted for publication in Astronomy and Astrophysics (A&A)

References in corpus (17)

• The Solar Orbiter mission -- Science overview
• The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance
• VFISV: Very Fast Inversion of the Stokes Vector for the Helioseismic and Magnetic Imager
• Flare-productive active regions
• The origin, early evolution and predictability of solar eruptions
• Penumbral structure and outflows in simulated sunspots
• Observables Processing for the Helioseismic and Magnetic Imager Instrument on the Solar Dynamics Observatory
• SunPy - Python for Solar Physics
• The formation of sunspot penumbra. I. Magnetic field properties
• The magnetic nature of umbra-penumbra boundary in sunspots
• Characterization of horizontal flows around solar pores from high-resolution time series of images
• Magnetic properties of a long-lived sunspot - Vertical magnetic field at the umbral boundary
• Could switchbacks originate in the lower solar atmosphere? I. Formation mechanisms of switchbacks
• Magnetic properties on the boundary of an evolving pore
• Magnetic topology of a naked sunspot: Is it really naked?
• Plasma flows and magnetic field interplay during the formation of a pore
• Photospheric plasma and magnetic field dynamics during the formation of solar AR 11190

Cited by in corpus (1)

• Determining the Magnetic Field in the Atmosphere of a Solar Active Region Observed by the CLASP2.1 Sounding Rocket Experiment