The Solar Magnetic Hump, Heliopause, and the Very Local Interstellar Medium
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Burlaga, L. F., J. Park, D. B. Berdichevsky, L. K. Jian, and A. Szabo. “The Solar Magnetic Hump, Heliopause, and the Very Local Interstellar Medium.” The Astrophysical Journal Letters 971, no. 1 (August 2024): L17. https://doi.org/10.3847/2041-8213/ad6397.
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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract
The magnetic hump was observed from 2020.4 to ~2022 by Burlaga et al. who offered the hypothesis that it originated at the Sun during the declining phase of the solar cycle. Voyager 1 observed intermittency of 1 hr increments of the magnetic field from 2013 through 2019, as well as in the magnetic hump that began at the jump pf2 at 2020.4 and ended at ~2022. Throughout this interval, the intermittency in the components of B and the magnitude B was described by the Tsallis distribution (q-Gaussian distribution). The q-Gaussian distributions have been observed throughout the solar wind and heliosheath. However, there was little or no intermittency in the 1 hr increments of the magnetic field observed by Voyager 1 from ~2022.0 through day 270, 2023. During this interval Voyager 1 observed intermittency with a Gaussian distribution, which is associated with Boltzmann–Gibbs statistics. The boundary between these two regions, at ~2022.0, coincides with the heliopause predicted by Fisk & Gloeckler. Alternatively, the Voyager 1 observations might be a solar cycle effect.