Exploring Magnetic Island Morphology through 2D MHD and Synthetic Fields

In this project, we are exploring a few aspects of low frequency and wavenumber magnetic field energy spectra in the context of space physics, following observations of 1/f behavior (e.g. [1]-[4]). The origin of this phenomena is still debated;  however studies have suggested that these processes could be generated from scale-invariant processes in the corona or further within the dynamo of the Sun. One of the paradigms that has been discussed ([5],[6]) for achieving scale invariant structure is the merger of two dimensional or quasi-two dimensional magnetic flux tubes or flux ropes. This may be particularly relevant in the corona. To further explore this connection, it becomes necessary to understand the distributions of size and magnetic flux content, as well as the morphology of magnetic structures/”islands” in two dimensional turbulence representations. These features of the magnetic field will be explored using methods described herein [7]. These will be implemented using magnetic fields obtained from synthetic construction and 2D simulation. 

[1]Burlaga, L. F., & Ness, N. F. 1998, JGR, 103, 29 719

[2]Matthaeus, W. H., & Goldstein, M. L. 1986, PhRvL, 57, 495

[3]Wang, J., Matthaeus, W. H., Chhiber, R., et al. 2024, SoPh, 299, 169

[4]Pradata, R. A., Roy, S., Matthaeus, W. H., et al. 2025, ApJL, 984, L23

[5]Matthaeus, W. H., & Goldstein, M. L. 1982, JGR, 87, 6011

[6]Mullan, D.J.: 1990, Astron. Astrophys. 232, 520.

[7]Servidio, S., Matthaeus, W., Shay, M., et al. 2010, Physics of Plasmas, 17