{
  "license": [
    {
      "url": "http://creativecommons.org/licenses/by/3.0/", 
      "license": "CC-BY-3.0"
    }
  ], 
  "copyright": [
    {
      "holder": "The Author(s)", 
      "statement": "The Author(s)", 
      "year": "2023"
    }
  ], 
  "control_number": "79770", 
  "_oai": {
    "updated": "2023-09-26T15:31:23Z", 
    "id": "oai:repo.scoap3.org:79770", 
    "sets": [
      "PLB"
    ]
  }, 
  "authors": [
    {
      "surname": "Sui", 
      "given_names": "Tao-Tao", 
      "affiliations": [
        {
          "country": "China", 
          "value": "College of Physics, Nanjing University of Aeronautics and Astronautics, Nanjing, China"
        }
      ], 
      "full_name": "Sui, Tao-Tao", 
      "orcid": "0000-0003-3541-6842", 
      "email": "suitt14@lzu.edu.cn"
    }, 
    {
      "affiliations": [
        {
          "country": "China", 
          "value": "Institute of Physics, Shaanxi University of Technology, Hanzhong, China"
        }, 
        {
          "country": "China", 
          "value": "Department of Physics, College of Sciences, Northeastern University, Shenyang, China"
        }
      ], 
      "surname": "Fu", 
      "given_names": "Qi-Ming", 
      "full_name": "Fu, Qi-Ming"
    }, 
    {
      "affiliations": [
        {
          "country": "China", 
          "value": "Institute of Theoretical Physics & Research Center of Gravitation, Lanzhou University, Lanzhou, China"
        }
      ], 
      "surname": "Guo", 
      "email": "guowd@lzu.edu.cn", 
      "full_name": "Guo, Wen-Di", 
      "given_names": "Wen-Di"
    }
  ], 
  "_files": [
    {
      "checksum": "md5:633f61bb1e99c60f5442ed3fe8f53008", 
      "filetype": "xml", 
      "bucket": "08e401b2-bd05-493e-bf65-feace43b5777", 
      "version_id": "fe3389c1-faf9-4764-9304-48294afabaf8", 
      "key": "10.1016/j.physletb.2023.138135.xml", 
      "size": 232266
    }, 
    {
      "checksum": "md5:54ddb84a1076ec221439a74b936647b9", 
      "filetype": "pdf", 
      "bucket": "08e401b2-bd05-493e-bf65-feace43b5777", 
      "version_id": "699d74a3-9bf1-4fa2-a2c3-f054fbb6f200", 
      "key": "10.1016/j.physletb.2023.138135.pdf", 
      "size": 892381
    }, 
    {
      "checksum": "md5:d8738215fdc195410eb9c45c54b10cae", 
      "filetype": "pdf/a", 
      "bucket": "08e401b2-bd05-493e-bf65-feace43b5777", 
      "version_id": "f49adb26-d240-4537-a431-ead2f3f7f670", 
      "key": "10.1016/j.physletb.2023.138135_a.pdf", 
      "size": 931830
    }
  ], 
  "record_creation_date": "2023-08-23T12:30:44.570499", 
  "titles": [
    {
      "source": "Elsevier", 
      "title": "The shadows of accelerating Kerr-Newman black hole and constraints from M87*"
    }
  ], 
  "collections": [
    {
      "primary": "Physics Letters B"
    }
  ], 
  "dois": [
    {
      "value": "10.1016/j.physletb.2023.138135"
    }
  ], 
  "publication_info": [
    {
      "journal_volume": "845 C", 
      "journal_title": "Physics Letters B", 
      "material": "article", 
      "artid": "138135", 
      "year": 2023
    }
  ], 
  "$schema": "http://repo.scoap3.org/schemas/hep.json", 
  "abstracts": [
    {
      "source": "Elsevier", 
      "value": "In this paper, we study the influence of the parameters for the accelerating Kerr-Newman black hole on the shadows and the constraints, extensively. We find that the rotating parameter a, the charge parameter e, and the inclination angle <math><msub><mrow><mi>\u03b8</mi></mrow><mrow><mn>0</mn></mrow></msub></math> affect the shadow qualitatively similar to that of Kerr-Newman black holes. The result shows that the size of the shadow will scale down with the accelerating factor A. Besides, the factor A also can affect the best viewing angles, which make the observations maximum deviate from <math><msub><mrow><mi>\u03b8</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mfrac><mrow><mi>\u03c0</mi></mrow><mrow><mn>2</mn></mrow></mfrac></math>, and the degree of the deviations are less than 1%. Then, we assume the M87* as an accelerating Kerr-Newman black hole with the mass <math><mi>M</mi><mo>=</mo><mn>6.5</mn><mo>\u00d7</mo><msup><mrow><mn>10</mn></mrow><mrow><mn>9</mn></mrow></msup><msub><mrow><mi>M</mi></mrow><mrow><mo>\u2299</mo></mrow></msub></math> and the distance <math><msub><mrow><mi>r</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>16.8</mn><mi>M</mi><mi>p</mi><mi>c</mi></math>. Combining the EHT observations, we find that neither the observations, circularity deviation \u0394C or axial ratio <math><msub><mrow><mi>D</mi></mrow><mrow><mi>x</mi></mrow></msub></math> can distinguish the accelerating black hole or not. However, the characteristic areal-radius of the shadow curve <math><msub><mrow><mi>R</mi></mrow><mrow><mi>a</mi></mrow></msub></math> can give corresponding constraints on the parameters of the accelerating Kerr-Newman black hole. The result shows that the bigger accelerating factor A is, the stronger constraints on the rotating parameter a and charged parameter e. The maximum range of the accelerating factor is <math><mi>A</mi><msub><mrow><mi>r</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>\u2264</mo><mn>0.558</mn></math> for a accelerating Schwarzschild case with <math><mo>(</mo><mi>a</mi><mo>/</mo><mi>M</mi><mo>=</mo><mi>e</mi><mo>/</mo><mi>M</mi><mo>=</mo><mn>0</mn><mo>)</mo></math>, and for an extremely slow accelerating case <math><mo>(</mo><mi>A</mi><msub><mrow><mi>r</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>\u2264</mo><mn>0.01</mn><mo>)</mo></math>, the ranges of rotating parameter a and charged parameter e are <math><mi>a</mi><mo>/</mo><mi>M</mi><mo>\u2208</mo><mo>(</mo><mn>0</mn><mo>,</mo><mn>1</mn><mo>)</mo></math> and <math><mi>e</mi><mo>/</mo><mi>M</mi><mo>\u2208</mo><mo>(</mo><mn>0</mn><mo>,</mo><mn>0.9</mn><mo>)</mo></math>."
    }
  ], 
  "imprints": [
    {
      "date": "2023-09-26", 
      "publisher": "Elsevier"
    }
  ], 
  "acquisition_source": {
    "date": "2023-09-26T15:30:56.958075", 
    "source": "Elsevier", 
    "method": "Elsevier", 
    "submission_number": "8e2fc7985c8111ee9688729695cabdc8"
  }
}