Events

Magnetic flux emergence and evolution through the photosphere provide the connection between subsurface magnetic fields and energy release in the low solar atmosphere. However, most vector magnetograms still provide boundary information on optical-depth surfaces, while the magnetic connectivity that underlies small-scale dynamics, like jets, is intrinsically three-dimensional.

In this talk, I will present DKIST ViSP/VBI observations of fine-scale solar jets analyzed with a newly constructed 3D vector magnetogram of the low solar atmosphere. I will briefly describe how the reconstruction resolves the 180-degree azimuth ambiguity and maps the inverted magnetic field from optical depth to geometric height using the divergence-free condition, but the focus will be on the physical structures revealed by the DKIST observations. Field-line tracing, electric-current mapping, and magnetic-connectivity diagnostics show that different jet sites are associated with distinct 3D magnetic environments, including canopy-like fields, bald-patch configurations, and hyperbolic-flux-tube-like connectivity.

These results demonstrate how DKIST spectropolarimetry can move beyond 2D boundary magnetograms toward observationally constrained 3D magnetic topology. The resulting measurements provide new constraints for models of fine-scale flux emergence, magnetic connectivity through the photosphere, and energy release in the low solar atmosphere.