{
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  "authors": [
    {
      "raw_name": "Pierce Giffin", 
      "affiliations": [
        {
          "country": "USA", 
          "value": "Department of Physics, University of California, Santa Cruz, California 95064, USA"
        }, 
        {
          "country": "USA", 
          "value": "Santa Cruz Institute for Particle Physics, Santa Cruz, California 95064, USA"
        }
      ], 
      "surname": "Giffin", 
      "given_names": "Pierce", 
      "full_name": "Giffin, Pierce"
    }, 
    {
      "raw_name": "John Lloyd", 
      "affiliations": [
        {
          "country": "USA", 
          "value": "Department of Physics, University of California, Santa Cruz, California 95064, USA"
        }
      ], 
      "surname": "Lloyd", 
      "given_names": "John", 
      "full_name": "Lloyd, John"
    }, 
    {
      "raw_name": "Samuel D. McDermott", 
      "affiliations": [
        {
          "country": "USA", 
          "value": "Fermi National Accelerator Laboratory, Batavia, Illinois 60510 USA"
        }
      ], 
      "surname": "McDermott", 
      "given_names": "Samuel D.", 
      "full_name": "McDermott, Samuel D."
    }, 
    {
      "raw_name": "Stefano Profumo", 
      "affiliations": [
        {
          "country": "USA", 
          "value": "Department of Physics, University of California, Santa Cruz, California 95064, USA"
        }, 
        {
          "country": "USA", 
          "value": "Santa Cruz Institute for Particle Physics, Santa Cruz, California 95064, USA"
        }
      ], 
      "surname": "Profumo", 
      "given_names": "Stefano", 
      "full_name": "Profumo, Stefano"
    }
  ], 
  "titles": [
    {
      "source": "APS", 
      "title": "Neutron star quantum death by small black holes"
    }
  ], 
  "dois": [
    {
      "value": "10.1103/PhysRevD.105.123030"
    }
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  "publication_info": [
    {
      "journal_volume": "105", 
      "journal_title": "Physical Review D", 
      "material": "article", 
      "journal_issue": "12", 
      "year": 2022
    }
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    "method": "APS", 
    "submission_number": "f27893d8f41d11eca1a1661ec451a4e4"
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  "page_nr": [
    7
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      "url": "https://creativecommons.org/licenses/by/4.0/", 
      "license": "CC-BY-4.0"
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  "copyright": [
    {
      "statement": "Published by the American Physical Society", 
      "year": "2022"
    }
  ], 
  "control_number": "70986", 
  "record_creation_date": "2022-06-24T14:30:03.812289", 
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      "primary": "HEP"
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      "primary": "Citeable"
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      "categories": [
        "hep-ph", 
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        "astro-ph.SR", 
        "gr-qc"
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      "value": "2105.06504"
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  ], 
  "abstracts": [
    {
      "source": "APS", 
      "value": "Neutron stars can be destroyed by black holes at their center accreting material and eventually by swallowing the entire star. Here we note that the accretion model adopted in the literature, based on Bondi accretion or variations thereof, is inadequate for small black holes\u2014black holes whose Schwarzschild radius is comparable to, or smaller than, the neutron\u2019s de Broglie wavelength. In this case, quantum mechanical aspects of the accretion process cannot be neglected, and give rise to a completely different accretion rate. We show that for the case of black holes seeded by the collapse of bosonic dark matter, this is the case for electroweak-scale dark matter particles. In the case of fermionic dark matter, typically the black holes that would form at the center of a neutron star are more massive, unless the dark matter particle mass is very large, larger than about <math><mrow><msup><mrow><mn>10</mn></mrow><mrow><mn>10</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>GeV</mi></mrow></math>. We calculate the lifetime of neutron stars harboring a \u201csmall\u201d black hole, and find that black holes lighter than <math><mo>\u223c</mo><msup><mn>10</mn><mn>11</mn></msup><mtext> </mtext><mtext> </mtext><mi>kg</mi></math> quickly evaporate, leaving no trace. More massive black holes destroy neutron stars via quantum accretion on timescales much shorter than the age of observed neutron stars. We find that the range where seed black holes inside neutron stars are massive enough that they do not quickly evaporate away, but not so massive that a fluid accretion picture is warranted is limited to between <math><mo>\u223c</mo><msup><mn>10</mn><mn>11</mn></msup></math> and <math><msup><mn>10</mn><mn>12</mn></msup><mtext> </mtext><mtext> </mtext><mi>kg</mi></math>, but our results are key to accurately determine the actual critical black hole mass corresponding to the onset of neutron star destruction."
    }
  ], 
  "imprints": [
    {
      "date": "2022-06-24", 
      "publisher": "APS"
    }
  ]
}