%0 Conference Proceedings
%4 sid.inpe.br/plutao/2022/12.12.17.52.32
%2 sid.inpe.br/plutao/2022/12.12.17.52.33
%@doi 10.1142/9789811258251_0316
%@isbn 9789811258251
%F lattes: 9527193250756102 2 BorgesRodCoeMalCas:2022:WhDwAc
%T A white dwarf accretion model for the anomalous X-ray pulsar 4U 0142+61
%D 2022
%A Borges, Sarah Vilanova,
%A Rodrigues, Cláudia Vilega,
%A Coelho, Jaziel G.,
%A Malheiro, Manuel,
%A Castro, Manuel,
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Universidade Tecnológica Federal do Paraná (UTFPR)
%@affiliation Instituto Tecnológico de Aeronáutica (ITA)
%@affiliation Instituto Tecnológico de Aeronáutica (ITA)
%@electronicmailaddress vilanovaborges@gmail.com
%@electronicmailaddress claudia.vilega@inpe.br
%B MG15 Meeting on General Relativity
%C University of Rome La Sapienza
%8 2020
%I World Scientific
%P 2105-2110
%S Proceedings
%K Accretion, magnetic field, rotation, white dwarfs.
%X 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.
%@language en
%3 9789811258251_0316.pdf
%U https://www.worldscientific.com/doi/abs/10.1142/9789811258251_0316