{
  "abstract": "The source PSR J0901-4046 shows a very long rotational period, of $\\approx 75.88$ s. In fact, its long period suggests that it could be a white dwarf. We examine the properties of the source and compare the outcomes under the hypotheses of the source being a highly magnetized white dwarf (B-WD) and neutron star. We find that assuming it to be a B-WD with a surface field $\\sim 10^{10}$ G explains many properties, including its storage/rotational energy, explaining luminosity. On the contrary, the neutron star-based idea, particularly if examined under the conventional spin down mechanism, requires an unusually high surface magnetic field $\\gtrsim 10^{14}$ G, even exceeding $10^{16}$ G, depending on the obliquity angle and emission mechanism. The source also sits very close to AR Sco, a white dwarf pulsar, in the period and period-derivative plane. We suggest that the source is a B-WD. Along with AR Sco, it being a B-WD constrains the death line model. B-WD hypothesis alleviates the necessity of an unusually high magnetic field hindering pair production for PSR J0901-4046 under the neutron star hypothesis. We argue that some rotation-powered pulsars with extreme properties may possibly be white dwarfs rather than neutron stars.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2610.28741",
  "author_total": 5,
  "authors": [
    {
      "name": "Banibrata Mukhopadhyay"
    },
    {
      "name": "Nirupam Roy"
    },
    {
      "name": "Zenia Zuraiq"
    },
    {
      "name": "Chandrachur Chakraborty"
    },
    {
      "name": "A R Rao"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/09hqqaxvy09ch.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2610.28741",
  "fulltext_url": null,
  "id": "09hqqaxvy09ch",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2610.28741",
  "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",
      "astro-ph.HE"
    ],
    [
      "arxiv",
      "astro-ph.SR"
    ],
    [
      "arxiv",
      "gr-qc"
    ],
    [
      "openalex",
      "3103|Pulsars and Gravitational Waves Research"
    ]
  ],
  "openalex": "W7223220853",
  "pdf_url": "https://arxiv.org/pdf/2610.28741",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-20",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/09hqqaxvy09ch.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:34:34Z",
      "native_id": "2610.28741",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2610.28741"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    },
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.SR",
      "subfield": "stellar"
    },
    {
      "field": "physics",
      "origin": "arxiv:gr-qc",
      "subfield": "gravitation"
    }
  ],
  "title": "Exploring PSR J0901-4046 as an ultra-slowly rotating neutron star versus a white dwarf",
  "title_text": "Exploring PSR J0901-4046 as an ultra-slowly rotating neutron star versus a white dwarf",
  "type": "preprint",
  "updated_at": "2026-10-30T12:34:34Z",
  "url": "https://research.draconitic.com/paper/09hqqaxvy09ch",
  "venue": "arXiv",
  "versions": []
}