{
  "abstract": "Cosmic transients can enhance the local radiation field on timescales of days to months. Using the time-domain \\TransRAT\\ framework, which self-consistently follows grain heating, alignment, rotational disruption, and switching of the alignment axis between the magnetic field ({\\bf B}) and the radiation direction ({\\bf k}), we predict the time-dependent dust polarization of a dense cloud, represented by a homogeneous one-zone model, illuminated by a Type~IIP supernova over a range of source--cloud distances. We identify four key signatures. First, for $D\\lesssim1$~pc, a \\emph{polarization flare} develops within days to weeks, marked by sharp increases in both thermal dust polarization and extinction-polarization efficiency; this is followed by a \\emph{polarization dip} as radiative torque disruption (RAT-D) destroys the large aligned grains. Second, the peak wavelength of extinction polarization, $λ_{\\rm max}$, shifts blueward as the minimum aligned-grain size decreases. Third, the transition from B-RAT to k-RAT produces an abrupt \\emph{polarization-angle rotation} of up to $45^{\\circ}$ in our fiducial geometry. Fourth, as the transient fades, the return to B-RAT generates a \\emph{polarization-angle reverberation} governed by Larmor precession. At $D>1$~pc, SN-induced polarization properties can persist long after the radiation has faded. These {\\it fossil imprints} offer the most practical near-term observational test: clouds near supernova remnants younger than the relaxation timescale of $\\sim10\\,t_{\\rm gas}$ with $t_{\\rm gas}$ gas damping time, should exhibit elevated polarization and blueshifted $λ_{\\max}$ today. Time-dependent dust polarization can therefore probe dust physics, dust properties, and pristine pre-shock magnetic fields in real time, while fossil imprints preserve a record of past explosions.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2607.24517",
  "author_total": 1,
  "authors": [
    {
      "name": "Thiem Hoang"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/1df5njewqzw5q.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2607.24517",
  "fulltext_url": null,
  "id": "1df5njewqzw5q",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2607.24517",
  "language": null,
  "licence": "CC-BY-4.0",
  "licence_label": "CC BY 4.0",
  "licence_source": "article",
  "licence_url": "http://creativecommons.org/licenses/by/4.0/",
  "metadata_licence": "CC0-1.0",
  "native_subjects": [
    [
      "arxiv",
      "astro-ph.GA"
    ],
    [
      "arxiv",
      "astro-ph.HE"
    ],
    [
      "openalex",
      "3103|Astrophysics and Star Formation Studies"
    ]
  ],
  "openalex": "W7171541093",
  "pdf_url": "https://arxiv.org/pdf/2607.24517",
  "pmcid": null,
  "pmid": null,
  "published": "2026-09-11",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/1df5njewqzw5q.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:21:07Z",
      "native_id": "2607.24517",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2607.24517"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.GA",
      "subfield": "galaxies"
    },
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    }
  ],
  "title": "Time-Domain Dust Astrophysics. I. Polarization Flares, Polarization-Angle Reverberation, and Fossil Imprints in Supernova-Illuminated Clouds",
  "title_text": "Time-Domain Dust Astrophysics. I. Polarization Flares, Polarization-Angle Reverberation, and Fossil Imprints in Supernova-Illuminated Clouds",
  "type": "preprint",
  "updated_at": "2026-10-30T12:21:07Z",
  "url": "https://research.draconitic.com/paper/1df5njewqzw5q",
  "venue": "arXiv",
  "versions": []
}