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      "year": "2022"
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  "authors": [
    {
      "affiliations": [
        {
          "country": "USA", 
          "value": "Department of Mathematics and Physics, North Carolina Central University, Durham, USA"
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      ], 
      "surname": "Eingorn", 
      "email": "maxim.eingorn@gmail.com", 
      "full_name": "Eingorn, Maxim", 
      "given_names": "Maxim"
    }, 
    {
      "orcid": "0000-0003-4554-1268", 
      "affiliations": [
        {
          "country": "Turkey", 
          "value": "Department of Physics, Istanbul Technical University, Istanbul, Turkey"
        }
      ], 
      "surname": "Y\u00fckselci", 
      "given_names": "A. Emrah", 
      "full_name": "Y\u00fckselci, A. Emrah"
    }, 
    {
      "orcid": "0000-0001-9107-5048", 
      "affiliations": [
        {
          "country": "Ukraine", 
          "value": "Astronomical Observatory, Odessa I.I. Mechnikov National University, Odessa, Ukraine"
        }
      ], 
      "surname": "Zhuk", 
      "given_names": "Alexander", 
      "full_name": "Zhuk, Alexander"
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  "titles": [
    {
      "source": "Elsevier", 
      "title": "Screening vs. gevolution: In chase of a perfect cosmological simulation code"
    }
  ], 
  "collections": [
    {
      "primary": "Physics Letters B"
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      "journal_volume": "826 C", 
      "journal_title": "Physics Letters B", 
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  "abstracts": [
    {
      "source": "Elsevier", 
      "value": "We compare two competing relativistic approaches to the N-body simulation of the Universe large-scale structure. To this end, employing the corresponding alternative computer codes (\u201cgevolution\u201d and \u201cscreening\u201d), we conduct a series of cosmological simulations in boxes of different sizes and calculate the power spectra of the scalar perturbation \u03a6, the frame-dragging vector potential B and the difference between scalar modes <math><mi>\u03c7</mi><mo>=</mo><mi>\u03a6</mi><mo>\u2212</mo><mi>\u03a8</mi></math>. We demonstrate that the corresponding power spectra are in very good agreement between the compared schemes. For example, the relative difference of the power spectra for \u03a6 is 0.04% maximum. Since the perturbed Einstein equations have much simpler form in the screening approach, the simulation with this code consumes less computational time, saving almost 40% of CPU hours."
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