{
  "abstract": "We report on the results of our XMM-Newton and NuSTAR campaign targeting V1674 Her in October 2023. These observations were timed to investigate the post-nova quiescent state 28 months after the 2021 outburst, although the optical luminosity was still slowly declining. The X-ray spectra are well-modeled by a multi-temperature thermal plasma. While in the best fit temperature we find that the highest plasma temperature is indicative of a massive white dwarf ($M_{\\text{WD}} \\approx 1.35 M_\\odot$), we caution that there is a degeneracy between the plasma temperature and the metallicity in the spectral fit, hindering a definitive constraint. Alternatively, the continuum can be phenomenologically described by a Comptonized component, although this model neglects the thermal bremsstrahlung component. Timing analysis reveals a stable 501.31 $\\pm$ 0.19 s modulation in the post-quiescent phase, whose amplitude diminishes with increasing energy; this is quite typical in intermediate polars (IP). The phase alignment between the quiescent and early post-outburst Chandra spin-folded light curves suggests that the soft X-ray emission originates from the same polar regions, which quickly re-established accretion following the eruption. V1674 Her belongs to a growing class of novae that are also IPs, and is one of four in which the modulation with rotation was observed during the outburst supersoft X-ray phase. We propose that the fast rise in outburst was due to a fast or centrifugal magnetic rotator wind, causing rapid mass loss instead of the commonly assumed radiation pressure wind.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2610.42132",
  "author_total": 4,
  "authors": [
    {
      "name": "G. J. M. Luna"
    },
    {
      "name": "M. Orio"
    },
    {
      "name": "A. Dobrotka"
    },
    {
      "name": "J. Magdolen"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/5cqkt6fz5j1sd.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2610.42132",
  "fulltext_url": null,
  "id": "5cqkt6fz5j1sd",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2610.42132",
  "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.HE"
    ],
    [
      "arxiv",
      "astro-ph.SR"
    ]
  ],
  "openalex": null,
  "pdf_url": "https://arxiv.org/pdf/2610.42132",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-30",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/5cqkt6fz5j1sd.ris",
  "sources": [
    {
      "first_seen": "2026-11-02T12:21:15Z",
      "native_id": "2610.42132",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2610.42132"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    },
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.SR",
      "subfield": "stellar"
    }
  ],
  "title": "Nova V1674 Her as a fast magnetic rotator",
  "title_text": "Nova V1674 Her as a fast magnetic rotator",
  "type": "preprint",
  "updated_at": "2026-11-04T15:20:51Z",
  "url": "https://research.draconitic.com/paper/5cqkt6fz5j1sd",
  "venue": "arXiv",
  "versions": [
    {
      "doi": "10.3847/1538-4357/aeba8a",
      "pid": null,
      "relation": "published-as",
      "title": null,
      "venue": null
    }
  ]
}