{
  "id": "2411.10256",
  "version": "v1",
  "published": "2024-11-15T15:03:52.000Z",
  "updated": "2024-11-15T15:03:52.000Z",
  "title": "Mass-loss, composition and observational signatures of stellar winds from X-ray bursts",
  "authors": [
    "Yago Herrera",
    "Daniel Muñoz Vela",
    "Glòria Sala",
    "Jordi José",
    "Yuri Cavecchi"
  ],
  "comment": "6 pages, 3 figures, part of 2024 XMM-Newton Science Conference Proceedings, Madrid",
  "categories": [
    "astro-ph.HE",
    "astro-ph.SR"
  ],
  "abstract": "X-Ray bursts (XRBs) are powerful thermonuclear events on the surface of accreting neutron stars (NSs), which can synthesize intermediate-mass elements. Although the high surface gravity prevents an explosive ejection, a small fraction of the envelope may be ejected by radiation-driven winds. In our previous works, we have developed a non-relativistic radiative wind model and coupled it to an XRB hydrodynamic simulation. We now apply this technique to another model featuring consecutive bursts. We determine the mass-loss and chemical composition of the wind ejecta. Results show that, for a representative XRB, about $0.1\\%$ of the envelope mass is ejected per burst, at an average rate of $3.9 \\times 10^{-12}\\,M_\\odot \\texttt{yr}^{-1}$. Between $66\\%$ and $76\\%$ of the ejecta composition is $^{60}$Ni, $^{64}$Zn, $^{68}$Ge, $^{4}$He and $^{58}$Ni. We also report on the evolution of observational quantities during the wind phase and simulate NICER observations that resemble those of 4U 1820-40.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2024-11-15T15:03:52.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "x-ray bursts",
      "observational signatures",
      "stellar winds",
      "high surface gravity prevents",
      "simulate nicer observations"
    ],
    "tags": [
      "conference paper"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}