{
  "id": "2101.11480",
  "version": "v1",
  "published": "2021-01-27T15:14:18.000Z",
  "updated": "2021-01-27T15:14:18.000Z",
  "title": "X-ray observations of the nova shell IPHASX J210204.7+471015",
  "authors": [
    "J. A. Toalá",
    "G. Rubio",
    "E. Santamaría",
    "M. A. Guerrero",
    "S. Estrada-Dorado",
    "G. Ramos-Larios",
    "L. Sabin"
  ],
  "comment": "6 pages and 5 Figures; Accepted to MNRAS",
  "categories": [
    "astro-ph.SR",
    "astro-ph.HE"
  ],
  "abstract": "We present the analysis of XMM-Newton European Photon Imaging Camera (EPIC) observations of the nova shell IPHASX J210204.7$+$471015. We detect X-ray emission from the progenitor binary star with properties that resemble those of underluminous intermediate polars such as DQ Her: an X-ray-emitting plasma with temperature of $T_\\mathrm{X}=(6.4\\pm3.1)\\times10^{6}$ K, a non-thermal X-ray component, and an estimated X-ray luminosity of $L_\\mathrm{X}=10^{30}$ erg s$^{-1}$. Time series analyses unveil the presence of two periods, the dominant with a period of $2.9\\pm0.2$ hr, which might be attributed to the spin of the white dwarf, and a secondary of $4.5\\pm0.6$ hr that is in line with the orbital period of the binary system derived from optical observations. We do not detect extended X-ray emission as in other nova shells probably due to its relatively old age (130-170 yr) or to its asymmetric disrupted morphology which is suggestive of explosion scenarios different to the symmetric ones assumed in available numerical simulations of nova explosions.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2021-01-27T15:14:18.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "x-ray observations",
      "xmm-newton european photon imaging camera",
      "nova shell iphasx j210204",
      "time series analyses unveil",
      "detect x-ray emission"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}