@InProceedings{BorgesRodCoeMalCas:2022:WhDwAc,
               author = "Borges, Sarah Vilanova and Rodrigues, Cl{\'a}udia Vilega and 
                         Coelho, Jaziel G. and Malheiro, Manuel and Castro, Manuel",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Universidade 
                         Tecnol{\'o}gica Federal do Paran{\'a} (UTFPR)} and {Instituto 
                         Tecnol{\'o}gico de Aeron{\'a}utica (ITA)} and {Instituto 
                         Tecnol{\'o}gico de Aeron{\'a}utica (ITA)}",
                title = "A white dwarf accretion model for the anomalous X-ray pulsar 4U 
                         0142+61",
            booktitle = "Proceedings...",
                 year = "2022",
                pages = "2105--2110",
         organization = "MG15. Meeting on General Relativity",
            publisher = "World Scientific",
             keywords = "Accretion, magnetic field, rotation, white dwarfs.",
             abstract = "The persistent emission of the anomalous X-ray pulsar 4U 0142+61 
                         extends over a broad range of energy, from mid-infrared up to hard 
                         X-rays. In particular, this object is unique among soft gamma-ray 
                         repeaters (SGRs) and anomalous X-ray pulsars (AXPs) in presenting 
                         simultaneously mid-infrared emission and also pulsed optical 
                         emission. In spite of having many propositions to explain this 
                         wide range of emission, it is still lacking one that reproduces 
                         simultaneously all the observations. Filling this gap, we present 
                         a model that is able, for the first time, to reproduce 
                         simultaneously the entire spectral energy distribution of 4U 
                         0142+61 using plausible physical components and parameters. We 
                         propose that the persistent emission comes from an accreting white 
                         dwarf (WD) surrounded by a debris disk. This model is thoroughly 
                         discussed at Ref. 2 and assumes that: (i) the hard X-rays are due 
                         to the bremsstrahlung emission from the post-shock region of the 
                         accretion column; (ii) the soft X-rays are originated by hot spots 
                         on the WD surface; and (iii) the optical and infrared emissions 
                         are caused by an optically thick dusty disk, the WD photosphere, 
                         and the tail of the post-shock region emission. In this scenario, 
                         4U 0142+61 harbors a fast-rotator near-Chandrasekhar WD, which is 
                         highly magnetized. Such a WD can be formed by a merger of two less 
                         massive WDs.",
  conference-location = "University of Rome La Sapienza",
      conference-year = "2020",
                  doi = "10.1142/9789811258251_0316",
                  url = "http://dx.doi.org/10.1142/9789811258251_0316",
                 isbn = "9789811258251",
                label = "lattes: 9527193250756102 2 BorgesRodCoeMalCas:2022:WhDwAc",
             language = "en",
           targetfile = "9789811258251_0316.pdf",
                  url = "https://www.worldscientific.com/doi/abs/10.1142/9789811258251_0316",
        urlaccessdate = "02 maio 2024"
}