{
  "abstract": "Compact star cores reach extreme densities and may contain exotic dense-matter phases. Information about the exotic interiors of rapidly rotating pulsars can be inferred from r-mode oscillations, whose stability is governed by viscous dissipation. In this work, we model a compact star containing a possible mixed phase of hadronic and quark matter and employ a hybrid statistical framework based on Bayesian inference to infer the dissipation time scales associated with the hybrid phase. Using low-mass X-ray binaries (LMXB) timing observations together with mass-radius constraints from the Neutron Star Interior Composition Explorer (NICER) mission, we estimate the shear and bulk viscosity contributions to r-mode damping for a hybrid star of two layers. Our inference yields shear and bulk viscous dissipation time scales of $τ_s=(4.99^{+0.49}_{-0.52}) \\times 10^8 T^{\\frac{5}{3}}$s and $τ_B=(2.150^{+1.23}_{-0.60}) \\times 10^{19} (T^4 10^{-12}+T^2 10^{-6})^{-1}Ω^{-2}$s respectively. The timescales thus obtained can be implemented to obtain the minima of the star's rotation frequency at $Ω=451.87$ Hz at temperature $T=0.259$ MeV for a hybrid star of mass $1.5$ $M_{\\odot}$ and $Ω=517.47$ Hz at $T=0.234$ MeV for $M=1.75 M_{\\odot}$. We find that the instability window obtained through the inference framework effectively explains the observed stability of millisecond pulsars in both the radio and LMXB populations, particularly for XTE J0929-314 and XTE J1807-294, J0437-4715, J2124-3358, respectively. These results demonstrate that Bayesian inference combined with r-mode phenomenology provides a powerful and observationally consistent framework for constraining the transport properties of dense hybrid matter.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": "Journal reference: European Physical Journal C 86, 1064 (2026)",
  "arxiv": "2606.27465",
  "author_total": 2,
  "authors": [
    {
      "name": "Khushbu Zala"
    },
    {
      "name": "Sreemoyee Sarkar"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/a3vrhctxy8phw.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2606.27465",
  "fulltext_url": null,
  "id": "a3vrhctxy8phw",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2606.27465",
  "language": null,
  "licence": "CC-BY-NC-SA-4.0",
  "licence_label": "CC BY-NC-SA 4.0",
  "licence_source": "article",
  "licence_url": "http://creativecommons.org/licenses/by-nc-sa/4.0/",
  "metadata_licence": "CC0-1.0",
  "native_subjects": [
    [
      "arxiv",
      "astro-ph.HE"
    ],
    [
      "arxiv",
      "hep-ph"
    ],
    [
      "arxiv",
      "nucl-th"
    ]
  ],
  "openalex": null,
  "pdf_url": "https://arxiv.org/pdf/2606.27465",
  "pmcid": null,
  "pmid": null,
  "published": "2026-09-16",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/a3vrhctxy8phw.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:22:01Z",
      "native_id": "2606.27465",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2606.27465"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    },
    {
      "field": "physics",
      "origin": "arxiv:hep-ph",
      "subfield": "high-energy"
    },
    {
      "field": "physics",
      "origin": "arxiv:nucl-th",
      "subfield": "nuclear"
    }
  ],
  "title": "Modelling Dissipative Dynamics of r-mode Instability in Hybrid Stars",
  "title_text": "Modelling Dissipative Dynamics of r-mode Instability in Hybrid Stars",
  "type": "preprint",
  "updated_at": "2026-10-30T12:22:01Z",
  "url": "https://research.draconitic.com/paper/a3vrhctxy8phw",
  "venue": "arXiv",
  "versions": [
    {
      "doi": "10.1140/epjc/s10052-026-16199-6",
      "pid": null,
      "relation": "published-as",
      "title": null,
      "venue": null
    }
  ]
}