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@Article{OliveiraRoPaDiBeSi:2019:OpObCY,
               author = "Oliveira, Alexandre S. and Rodrigues, Cl{\'a}udia Vilega and 
                         Palhares, Matheus S. and Diaz, Marcos P. and Belloni, Diogo 
                         Teixeira and Silva, Karleyne M. G.",
          affiliation = "{Universidade do Vale do Para{\'{\i}}ba (UNIVAP)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Universidade do Vale 
                         do Para{\'{\i}}ba (UNIVAP)} and {Universidade de S{\~a}o Paulo 
                         (USP)} and {Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {European Southern Observatory}",
                title = "Optical observations and CYCLOPS post-shock region modelling of 
                         the polar V348 Pav",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2019",
               volume = "489",
               number = "3",
                pages = "4032--4042",
                month = "Nov.",
             keywords = "polarization, radiative transfer, stars: individual: V348 Pav, 
                         stars: magnetic field, novae, cataclysmic variables, white 
                         dwarfs.",
             abstract = "Post-shock regions (PSR) of polar cataclysmic variables (CVs) 
                         produce most of their luminosity and give rise to high circular 
                         polarization in optical wavelengths and strong variability on the 
                         white dwarf (WD) rotation period, which are distinctive features 
                         of these systems. To investigate the polar candidate V348 Pav, we 
                         obtained a comprehensive observational set including photometric, 
                         polarimetric, and spectroscopic data, which was used to constrain 
                         the post-shock properties of the system. The object presents high 
                         circular polarization (similar to 30 per cent) and high He II 4686 
                         angstrom to H beta line ratio, confirming it is a polar. From both 
                         radial velocities and light curves, we determined an orbital 
                         period of 79.98 min, close to the orbital period minimum of CVs. 
                         The H beta radial velocity curve has a semi-amplitude of 141.4 +/- 
                         1.5 km s(-1). Doppler tomography showed that most of the spectral 
                         line emission in this system is originated in the region of the 
                         companion star facing the WD, possibly irradiated by the emission 
                         related to the PSR. We modelled the PSR using the CYCLOPS code. 
                         The PSR density and temperature profiles, obtained by a proper 
                         solution of the hydrothermodynamic equations, were used in a 3D 
                         radiative transfer solution that takes into account the system 
                         geometry. We could reproduce the V348 Pav B, V, R, and I 
                         photometric and polarimetric data using a model with a WD magnetic 
                         field of similar to 28 MG, a WD mass of similar to 0.85M(circle 
                         dot), and a low (similar to 25 degrees) orbital inclination. These 
                         values for the WD mass and orbital inclination are consistent with 
                         the measured radial velocities.",
                  doi = "10.1093/mnras/stz2445",
                  url = "http://dx.doi.org/10.1093/mnras/stz2445",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "oliveira_optical.pdf",
        urlaccessdate = "17 abr. 2021"
}


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