{
  "id": "1910.08317",
  "version": "v1",
  "published": "2019-10-18T09:25:43.000Z",
  "updated": "2019-10-18T09:25:43.000Z",
  "title": "Investigation of the Millisecond Pulsar Origins by their Spin Periods at the Wavebands of Radio, X-Ray, and γ-Ray",
  "authors": [
    "De-Hua Wang",
    "Cheng-Min Zhang",
    "Shuang-Qiang Wang"
  ],
  "comment": "9 pages, 2 figures, 6 tables",
  "journal": "2019PASP..131b4201W (Publications of the Astronomical Society of the Pacific, Volume 131, Issue 996, pp. 024201 (2019))",
  "doi": "10.1088/1538-3873/aaecc7",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "To track the formation and evolution links of the millisecond pulsars (MSPs) powered by accretion and rotation in the Galactic field, we investigate the spin period (P) and spin-down power (Edot) distributions of the MSPs observed at the wavebands of radio, X-ray, and {\\gamma}-ray. We find that all but one (119/120) of the {\\gamma}-ray MSPs have been detected with the radio signals (radio+{\\gamma} MSPs); on the contrary, nearly half of the radio MSPs (118/237) have not been detected with {\\gamma}-rays (radio-only MSPs). In addition, the radio+{\\gamma} MSPs are shown to be the relative faster and more energetic objects (<P> ~ 3.28 ms and <Edot> ~ 4.5 * 10^34 erg s^-1) compared with the radio-only MSPs (<P> ~ 4.70 ms and <Edot> ~ 1.0 * 10^34 erg s^-1), while the spin periods of these two MSP populations are compatible with the log-normal distributions by the statistical tests. Most rotation-powered MSPs (RMSPs) with the radio eclipsing (31/34) exhibit the radio+{\\gamma} signals, which share the faster spin (<P> ~ 2.78 ms) and larger spin-down power (<Edot> ~ 4.1 * 10^34 erg s^-1) distributions than the non-eclipsing ones (<P> ~ 4.19 ms, <Edot> ~ 2.4 * 10^34 erg s^-1), implying the radio+{\\gamma} MSPs to be younger than the radio-only MSPs. It is noticed that the spin distribution of the accretion-powered X-ray MSPs shows a clustering phenomenon around ~ 1.6-2.0 ms, which is not observed in RMSPs, hinting that the RMSPs may experience the multiple possible origins. Particularly, all the three super-fast spinning RMSPs with P ~ 1.4-1.6 ms exhibit the non-eclipsing, and we argue that they may be the distinctive sources formed by the accretion induced collapse (AIC) of white dwarfs.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2019-10-18T09:25:43.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "spin period",
      "millisecond pulsar origins",
      "radio-only msps",
      "investigation",
      "larger spin-down power"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "publisher": "IOP"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 9,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}