@Article{SilvaRoOlAlCiCoJa:2015:NeEcPo,
               author = "Silva, Karleyne M. G. and Rodrigues, Cl{\'a}udia Vilega and 
                         Oliveira, A. S. and Almeida, L. A. and Cieslinski, 
                         Deon{\'{\i}}sio and Costa, Joaquim Eduardo Rezende and 
                         Jablonski, Francisco Jos{\'e}",
          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 do Vale do 
                         Para{\'{\i}}ba (UNIVAP)} and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)} and {Instituto Nacional de Pesquisas Espaciais 
                         (INPE)} and {Instituto Nacional de Pesquisas Espaciais (INPE)}",
                title = "MLS110213:022733+130617: a new eclipsing polar above the period 
                         gap",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2015",
               volume = "451",
                pages = "4183--4192",
             keywords = "Binaries: eclipsing, Magnetic fields, Novae, cataclysmic 
                         variables, Polarization, Radiative transfer, Stars: individual: 
                         MLS110213:022733+130617.",
             abstract = "This study confirms MLS110213:022733+130617 as a new eclipsing 
                         polar. We performed optical spectroscopic, polarimetric and 
                         photometric follow-up of this variable source identified by the 
                         Catalina Real Time Transient Survey. Using the mid-eclipse times, 
                         we estimated an orbital period of 3.787 h, which is above the 
                         orbital period gap of the cataclysmic variables (CVs). There are 
                         nine other known polars with longer orbital periods, and only two 
                         of them are eclipsing. We identified high- and low-brightness 
                         states and high polarization modulated with the orbital period. 
                         The spectra are typical of polars, with strong high ionization 
                         emission lines and inverted Balmer decrement. The He II 4686 Å 
                         line is as strong as H \β. We modelled the photometric and 
                         polarimetric bright-state light curves using the CYCLOPS code. Our 
                         modelling suggests an extended emitting region on the white dwarf 
                         (WD) surface, with a mean temperature of 9 keV and B in the range 
                         18-33, although the possibility that it could be a two-pole 
                         accretor cannot yet be ruled out. TheWDmass estimated from the 
                         shock temperature is 0.67 M\⊙. The derived parameters are 
                         consistent with the eclipse profile. The distance was estimated as 
                         406 ± 54 pc using the period-luminosity-colours method. MLS110213 
                         populates a rare sub-group of polars, near the upper limit of the 
                         period distribution, important to understand the evolution of 
                         mCVs.",
                  doi = "10.1093/mnras/stv1105",
                  url = "http://dx.doi.org/10.1093/mnras/stv1105",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
        urlaccessdate = "27 abr. 2024"
}