% IMPORTANT: The following is UTF-8 encoded.  This means that in the presence
% of non-ASCII characters, it will not work with BibTeX 0.99 or older.
% Instead, you should use an up-to-date BibTeX implementation like “bibtex8” or
% “biber”.

@ARTICLE{Stiele:1033995,
      author       = {Stiele, H. and Kong, A. K. H.},
      title        = {{NICER} and {S}wift /{XRT} monitoring of the 2023 outburst
                      of {S}wift {J}1727.7–1613},
      journal      = {Astronomy and astrophysics},
      volume       = {691},
      issn         = {0004-6361},
      address      = {Les Ulis},
      publisher    = {EDP Sciences},
      reportid     = {FZJ-2024-06828},
      pages        = {A268 -},
      year         = {2024},
      abstract     = {Aims. The X-ray transient Swift J1727.7–1613 was first
                      detected on August 24 2023 by Swift/BAT and INTEGRAL. We
                      investigated data from the Neutron star Interior Composition
                      Explorer (NICER) and the Neil GehrelsSwift Observatory taken
                      between August and October 2023.<br><br>Methods. We studied
                      diagnostic diagrams, energy spectra, and short term
                      variability. The observations cover the initial rise of the
                      outburst in the hard state and the transition to the soft
                      state. We focused on the evolution of quasi-periodic
                      oscillations (QPOs) using power-density spectra and on the
                      evolution of the spectral parameters.<br><br>Results. The
                      overall evolution of Swift J1727.7–1613 is consistent with
                      this source being a low-mass black hole X-ray binary. Based
                      on the Lense-Thirring precession interpretation of type-C
                      QPOs, we obtained outer radii for the hot inner flow and
                      found that the overall evolution of these radii agrees well
                      with the evolution of the inner disc radii obtained from
                      fits to the energy spectra. This result holds on all
                      timescales tested in this study and supports the
                      Lense-Thirring precession interpretation of type-C QPOs.},
      cin          = {JSC},
      ddc          = {520},
      cid          = {I:(DE-Juel1)JSC-20090406},
      pnm          = {5111 - Domain-Specific Simulation $\&$ Data Life Cycle Labs
                      (SDLs) and Research Groups (POF4-511) / Big Bang to Big Data
                      - B3D [NRW-Cluster für datenintensive Radioastronomie]
                      (PROFILNRW-2020-038B)},
      pid          = {G:(DE-HGF)POF4-5111 / G:(DE-Juel-1)PROFILNRW-2020-038B},
      typ          = {PUB:(DE-HGF)16},
      UT           = {WOS:001360344100008},
      doi          = {10.1051/0004-6361/202450657},
      url          = {https://juser.fz-juelich.de/record/1033995},
}