{
  "abstract": "The solar wind plasma is modeled as a collection of discrete domains, each possessing local rotational symmetry about its domain-mean magnetic field. Based on this partial symmetry, we construct cascade models governed by the nonlinear and Alfvénic time scales. We introduce a stochastic renewal process with a bimodal waiting-time distribution determined by these two time scales. This process yields a two-branch renormalization solution for the total energy: a statistically robust branch with an Iroshnikov-Kraichnan-like $k^{-3/2}$ spectrum and a statistically marginal branch with a Kolmogorov-like $k^{-5/3}$ spectrum. Whenever energy-flux fluctuations become supercritical, the system selects the faster of the two available cascade rates, thereby preventing flux accumulation. During solar wind expansion, the system undergoes a dynamical first-order phase transition from the slow $k^{-3/2}$ cascade to the fast $k^{-5/3}$ cascade, with switchbacks accelerating the transition. The mixing of subcritical and supercritical domains in raw spacecraft measurements produces an apparent decoupling of the velocity and magnetic-field spectral indices. Incorporating a magnetic helicity cascade slaved to the energy cascade, we show that the large-scale spectra decouple into $k^{-3/4}$ magnetic and $k^{-3/2}$ kinetic spectra. For switchbacks inside the upper solar corona, the corresponding large-scale spectra instead decouple into $k^{-2/3}$ magnetic and $k^{-5/3}$ kinetic spectra. Data from Voyager, Ulysses, Helios, Wind, and PSP confirm the spectral signatures across heliospheric regions spanning heliocentric distances from 0.056 to 140 AU.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2609.10418",
  "author_total": 1,
  "authors": [
    {
      "name": "A. Bershadskii"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/1fcmj9eps9vd5.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2609.10418",
  "fulltext_url": null,
  "id": "1fcmj9eps9vd5",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2609.10418",
  "language": null,
  "licence": "LicenseRef-arXiv-nonexclusive-1.0",
  "licence_label": "arXiv licence",
  "licence_source": "article",
  "licence_url": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
  "metadata_licence": "CC0-1.0",
  "native_subjects": [
    [
      "arxiv",
      "physics.space-ph"
    ],
    [
      "openalex",
      "3103|Solar and Space Plasma Dynamics"
    ]
  ],
  "openalex": "W7212142796",
  "pdf_url": "https://arxiv.org/pdf/2609.10418",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-29",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/1fcmj9eps9vd5.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:36:28Z",
      "native_id": "2609.10418",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2609.10418"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:physics.space-ph",
      "subfield": "stellar"
    }
  ],
  "title": "Cascade models of anisotropic turbulence in magnetized plasma of solar wind",
  "title_text": "Cascade models of anisotropic turbulence in magnetized plasma of solar wind",
  "type": "preprint",
  "updated_at": "2026-11-01T12:20:47Z",
  "url": "https://research.draconitic.com/paper/1fcmj9eps9vd5",
  "venue": "arXiv",
  "versions": []
}