@Article{LImaPCNSCGSRABH:2024:Ev3XJ1,
               author = "LIma, Rafael C. R. de and Pereira, Jonas P. and Coelho, Jaziel G. 
                         and Nunes, Rafael da Costa and Stecchini, Paulo Eduardo Freire and 
                         Castro, Manuel and Gomes, Pierre and Silva, Rodrigo Reinert da and 
                         Rodrigues, Cl{\'a}udia Vilega and Ara{\'u}jo, Jos{\'e} Carlos 
                         Neves de and Bejger, Michal and Haensel, Pawel",
          affiliation = "{Universidade do Estado de Santa Catarina (UDESC)} and {Polish 
                         Academy of Sciences} and {Universidade Federal do 
                         Esp{\'{\i}}rito Santo (UFES)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)} and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)} and {Universidade Estadual de Campinas 
                         (UNICAMP)} and {Universidade do Estado de Santa Catarina (UDESC)} 
                         and {Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Polish Academy of 
                         Sciences} and {Polish Academy of Sciences}",
                title = "Evidence for 3XMM J185246.6+003317 as a massive magnetar with a 
                         low magnetic field",
              journal = "Journal of High Energy Astrophysics",
                 year = "2024",
               volume = "42",
                pages = "52--62",
                month = "June",
             abstract = "3XMM J185246.6+003317 is a transient magnetar located in the 
                         vicinity of the supernova remnant Kes 79. So far, observations 
                         have only set upper limits to its surface magnetic field and 
                         spindown, and there is no estimate for its mass and radius. Using 
                         ray-tracing modelling and Bayesian inference for the analysis of 
                         several light curves spanning a period of around three weeks, we 
                         have found that it may be one of the most massive neutron stars to 
                         date. In addition, our analysis suggests a multipolar magnetic 
                         field structure with a subcritical field strength and a carbon 
                         atmosphere composition. Due to the time-resolution limitation of 
                         the available light curves, we estimate the surface magnetic field 
                         and the mass to be log10\⁡(B/G)=11.89\−0.93+0.19 and 
                         M=2.09\−0.09+0.16 M\⊙ at 1\σ confidence level, 
                         while the radius is estimated to be R=12.02\−1.42+1.44 km 
                         at 2\σ confidence level. They were verified by simulations, 
                         i.e., data injections with known model parameters, and their 
                         subsequent recovery. The best-fitting model has three small hot 
                         spots, two of them in the southern hemisphere. These are, however, 
                         just first estimates and conclusions, based on a simple 
                         ray-tracing model with anisotropic emission; we also estimate the 
                         impact of modelling on the parameter uncertainties and the 
                         relevant phenomena on which to focus in more precise analyses. We 
                         interpret the above best-fitting results as due to accretion of 
                         supernova layers/interstellar medium onto 3XMM J185246.6+003317 
                         leading to burying and a subsequent re-emergence of the magnetic 
                         field, and a carbon atmosphere being formed possibly due to 
                         hydrogen/helium diffusive nuclear burning. Finally, we briefly 
                         discuss some consequences of our findings for superdense matter 
                         constraints.",
                  doi = "10.1016/j.jheap.2024.04.001",
                  url = "http://dx.doi.org/10.1016/j.jheap.2024.04.001",
                 issn = "2214-4048",
             language = "en",
           targetfile = "1-s2.0-S2214404824000235-main.pdf",
        urlaccessdate = "01 maio 2024"
}