{
  "id": "nucl-th/9901090",
  "version": "v1",
  "published": "1999-01-27T17:43:57.000Z",
  "updated": "1999-01-27T17:43:57.000Z",
  "title": "Microscopic Calculations of Weak Interaction Rates of Nuclei in Stellar Environment for A = 18 to 100",
  "authors": [
    "J. -U. Nabi",
    "H. V. Klapdor-Kleingrothaus"
  ],
  "comment": "9 pages",
  "journal": "Eur.Phys.J.A5:337-339,1999",
  "doi": "10.1007/s100500050292",
  "categories": [
    "nucl-th",
    "astro-ph"
  ],
  "abstract": "We report here the microscopic calculation of weak interaction rates in stellar matter for 709 nuclei with A = 18 to 100 using a generalized form of proton-neutron quasiparticle RPA model with separable Gamow-Teller forces. This is the first ever extensive microscopic calculation of weak rates calculated over a wide temperature-density grid which includes 10^7 \\leq T(K) \\leq 30 \\times 10^9 and 10 \\leq \\rho Y_{e} (gcm^{-3}) \\leq 10^{11}, and over a larger mass range. Particle emission processes from excited states, previously ignored, are taken into account, and are found to significantly affect some $\\beta$ decay rates. The calculated capture and decay rates take into consideration the latest experimental energy levels and $ft$ value compilations. Our calculation of electron capture and $\\beta$-decay rates, in the $fp$-shell, show considerable differences with a recently reported shell model diagonalization approach calculation.",
  "revisions": [
    {
      "version": "v1",
      "updated": "1999-01-27T17:43:57.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "weak interaction rates",
      "microscopic calculation",
      "stellar environment",
      "decay rates",
      "shell model diagonalization approach calculation"
    ],
    "tags": [
      "journal article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 9,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 494577
    }
  }
}