1 Ocak 2022 Dergi makalesi Açık Erişim

Allak, S.; Akyuz, A.; Oralhan, I. Akkaya; Avdan, S.; Aksaker, N.; Vinokurov, A.; Soydugan, F.; Sonbas, E.; Dhuga, K. S.

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  <identifier identifierType="URL">https://aperta.ulakbim.gov.tr/record/256679</identifier>
  <creators>
    <creator>
      <creatorName>Allak, S.</creatorName>
      <givenName>S.</givenName>
      <familyName>Allak</familyName>
    </creator>
    <creator>
      <creatorName>Akyuz, A.</creatorName>
      <givenName>A.</givenName>
      <familyName>Akyuz</familyName>
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    <creator>
      <creatorName>Oralhan, I. Akkaya</creatorName>
      <givenName>I. Akkaya</givenName>
      <familyName>Oralhan</familyName>
      <affiliation>Erciyes Univ, Dept Astron &amp; Space Sci, TR-38039 Kayseri, Turkey</affiliation>
    </creator>
    <creator>
      <creatorName>Avdan, S.</creatorName>
      <givenName>S.</givenName>
      <familyName>Avdan</familyName>
      <affiliation>Univ Cukurova, Space Sci &amp; Solar Energy Res &amp; Applicat Ctr UZAYM, TR-01330 Adana, Turkey</affiliation>
    </creator>
    <creator>
      <creatorName>Aksaker, N.</creatorName>
      <givenName>N.</givenName>
      <familyName>Aksaker</familyName>
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    <creator>
      <creatorName>Vinokurov, A.</creatorName>
      <givenName>A.</givenName>
      <familyName>Vinokurov</familyName>
      <affiliation>Special Astrophys Observ Russian AS, Nizhnii Arkhyz 399167, Russia</affiliation>
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    <creator>
      <creatorName>Soydugan, F.</creatorName>
      <givenName>F.</givenName>
      <familyName>Soydugan</familyName>
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    <creator>
      <creatorName>Sonbas, E.</creatorName>
      <givenName>E.</givenName>
      <familyName>Sonbas</familyName>
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    <creator>
      <creatorName>Dhuga, K. S.</creatorName>
      <givenName>K. S.</givenName>
      <familyName>Dhuga</familyName>
      <affiliation>George Washington Univ, Dept Phys, Washington, DC 20052 USA</affiliation>
    </creator>
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  <titles>
    <title>The Transient Ultraluminous X-Ray Source, Ulx-4, In M51</title>
  </titles>
  <publisher>Aperta</publisher>
  <publicationYear>2022</publicationYear>
  <dates>
    <date dateType="Issued">2022-01-01</date>
  </dates>
  <resourceType resourceTypeGeneral="Text">Journal article</resourceType>
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    <alternateIdentifier alternateIdentifierType="url">https://aperta.ulakbim.gov.tr/record/256679</alternateIdentifier>
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  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsIdenticalTo">10.1093/mnras/stab3693</relatedIdentifier>
  </relatedIdentifiers>
  <rightsList>
    <rights rightsURI="http://www.opendefinition.org/licenses/cc-by">Creative Commons Attribution</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">We present the results of a temporal and spectral analysis of the transient source ULX-4 in the galaxy M51. The data used were drawn from Chandra, XMM-Newton, and Swift-XRT archives, spanning the years 2000-2019.. The X-ray flux of the source is seen to vary by two orders of magnitudes within a month but a short-term variability was not observed over the time intervals of 100-2000 s in the 0.3-10 keV energy band. We find some evidence for the existence of bi-modality feature in the flux distribution of ULX-4. We identified two optical sources as possible counterparts within an error radius of 0.'' 18 at 95 per cent confidence level for ULX-4 based on the archival Hubble Space Telescope (HST)/ACS and HST/WFC3 data. Blackbody fits of the spectral energy distributions (SEDs) indicate the spectral type to be B-type stars. One of these counterparts exhibits a low-amplitude optical periodicity of 264 +/- 37 d in the F606W filter; if we assume this apparent periodicity is associated with the orbital motion of the donor, then it is more likely that the donor is a red supergiant satisfying the long periodicity and accretion via Roche lobe overflow. Consequently, the SED would then have to be interpreted as a superposition of emissions from a cold donor and a hot flow component, most likely from an accretion disc. If, on the other hand, the periodicity is superorbital in nature i.e. due to possible interactions of the compact object with a circumstellar disc, the donor could then be a Be/X star hosting a neutron star.</description>
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