Diffusion of magnetic elements in a supergranular cell

Abstract

Small scale magnetic fields (magnetic elements) are ubiquitous in the solar photosphere. Their interaction can provide energy to the upper atmospheric layers, and contribute to heat the solar corona. In this work, the dynamic properties of magnetic elements in the quiet Sun are investigated. The high number of magnetic elements detected in a supegranular cell allowed us to compute their displacement spectrum $⟨(\Delta r{)}^2⟩\propto {\tau }^{\gamma }$ (being $\gamma >0$, and $\tau$ the time since the first detection), separating the contribution of the network (NW) and the internetwork (IN) regions. In particular, we found $\gamma =1.27\pm 0.05$ and $\gamma =1.08\pm 0.11$ in NW (at smaller and larger scales, respectively), and $\gamma =1.44\pm 0.08$ in IN. These results are discussed in light of the literature on the topic, as well as the implications for the build up of the magnetic network.

References in corpus (5)

• Emergence of Small-Scale Magnetic Loops in the Quiet Sun Internetwork
• Hinode Observations of Magnetic Elements in Internetwork Areas
• Identifying Potential Markers of the Sun's Giant Convective Scale
• Pervasive Linear Polarization Signals in the Quiet Sun
• 3D photospheric velocity field of a Supergranular cell

Cited by in corpus (7)

• Characterising motion types of G-band bright points in the quiet Sun
• Non-linear propagation of kink waves to the solar chromosphere
• Observational evidence for buffeting induced kink waves in solar magnetic elements
• Pair separation of magnetic elements in the quiet Sun
• Super-diffusion versus competitive advection: a simulation
• Magnetic pattern at supergranulation scale: the Void Size Distribution
• Chromospheric Rapid Blueshifted Excursions Observed with IBIS and Their Association with Photospheric Magnetic Field Evolution