1 Ocak 2018 Dergi makalesi Açık Erişim

Meshcheryakov, Alexander V.; Tsygankov, Sergey S.; Khamitov, Irek M.; Shakura, Nikolay I.; Bikmaev, Ilfan F.; Eselevich, Maxim V.; Vlasyuk, Valeriy V.; Pavlinsky, Mikhail N.

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  <identifier identifierType="URL">https://aperta.ulakbim.gov.tr/record/89777</identifier>
  <creators>
    <creator>
      <creatorName>Meshcheryakov, Alexander V.</creatorName>
      <givenName>Alexander V.</givenName>
      <familyName>Meshcheryakov</familyName>
    </creator>
    <creator>
      <creatorName>Tsygankov, Sergey S.</creatorName>
      <givenName>Sergey S.</givenName>
      <familyName>Tsygankov</familyName>
    </creator>
    <creator>
      <creatorName>Khamitov, Irek M.</creatorName>
      <givenName>Irek M.</givenName>
      <familyName>Khamitov</familyName>
    </creator>
    <creator>
      <creatorName>Shakura, Nikolay I.</creatorName>
      <givenName>Nikolay I.</givenName>
      <familyName>Shakura</familyName>
      <affiliation>Kazan Fed Univ, Kremlevskaya 18, Kazan 420008, Russia</affiliation>
    </creator>
    <creator>
      <creatorName>Bikmaev, Ilfan F.</creatorName>
      <givenName>Ilfan F.</givenName>
      <familyName>Bikmaev</familyName>
    </creator>
    <creator>
      <creatorName>Eselevich, Maxim V.</creatorName>
      <givenName>Maxim V.</givenName>
      <familyName>Eselevich</familyName>
      <affiliation>RAS, SB, ISTP, Lermontov Str 126A, Irkutsk 664033, Russia</affiliation>
    </creator>
    <creator>
      <creatorName>Vlasyuk, Valeriy V.</creatorName>
      <givenName>Valeriy V.</givenName>
      <familyName>Vlasyuk</familyName>
      <affiliation>RAS, SAO, Nizhnii Arkhyz 369167, Russia</affiliation>
    </creator>
    <creator>
      <creatorName>Pavlinsky, Mikhail N.</creatorName>
      <givenName>Mikhail N.</givenName>
      <familyName>Pavlinsky</familyName>
      <affiliation>Russian Acad Sci IKI, Space Res Inst, 84-32 Profsoyuznaya Str, Moscow 117997, Russia</affiliation>
    </creator>
  </creators>
  <titles>
    <title>Evolution Of Broad-Band Sed During Outburst Rise In Ns X-Ray Nova Aql X-1</title>
  </titles>
  <publisher>Aperta</publisher>
  <publicationYear>2018</publicationYear>
  <dates>
    <date dateType="Issued">2018-01-01</date>
  </dates>
  <resourceType resourceTypeGeneral="Text">Journal article</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://aperta.ulakbim.gov.tr/record/89777</alternateIdentifier>
  </alternateIdentifiers>
  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsIdenticalTo">10.1093/mnras/stx2565</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">The observed evolution of the broad-band spectral energy distribution (SED) in NS X-ray Nova Aql X-1 during the rise phase of a bright Fast-Rise-Exponential-Decay-type outburst in 2013 can be understood in the framework of thermal emission from non-stationary accretion disc with radial temperature distribution transforming from a single-temperature blackbody emitting ring into the multicolour irradiated accretion disc. SED evolution during the hard to soft X-ray state transition looks unusual, as it cannot be reproduced by the standard disc irradiation model with a single irradiation parameter for NUV, Optical and NIR spectral bands. NIR (NUV) band is correlated with soft (hard) X-ray flux changes during the state transition interval, respectively. In our interpretation, at the moment of X-ray state transition UV-emitting parts of the accretion disc are screened from direct X-ray illumination from the central source and are heated primarily by hard X-rays (E &amp;gt; 10 keV), scattered in the hot corona or wind possibly formed above the optically thick outer accretion flow; the outer edge of multicolour disc, which emits in Optical-NIR, can be heated primarily by direct X-ray illumination. We point out that future simultaneous multiwavelength observations of X-ray Nova systems during the fast X-ray state transition interval are of great importance, as it can serve as 'X-ray tomograph' to study physical conditions in outer regions of accretion flow. This can provide an effective tool to directly test the energy-dependent X-ray heating efficiency, vertical structure and accretion flow geometry in transient low-mass X-ray binaries.</description>
  </descriptions>
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