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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

A Magnetic White Dwarf Accretion Model for the Anomalous X-Ray Pulsar 4U 0142+61

Texto completo
Autor(es):
Borges, V, Sarah ; Rodrigues, V, Claudia ; Coelho, Jaziel G. [1, 2] ; Malheiro, Manuel [3] ; Castro, Manuel [1]
Número total de Autores: 5
Afiliação do(s) autor(es):
[1] Rodrigues, Claudia, V, Borges, Sarah, V, Inst Nacl Pesquisas Espaciais INPE, Div Astrofis, Av Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP - Brazil
[2] Univ Tecnol Fed Parana UTFPR, Dept Fis, BR-85884000 Medianeira, PR - Brazil
[3] Borges, Sarah, V, Inst Tecnol Aeronalut ITA, Dept Fis, BR-12228900 Sao Jose Dos Campos, SP - Brazil
Número total de Afiliações: 3
Tipo de documento: Artigo Científico
Fonte: ASTROPHYSICAL JOURNAL; v. 895, n. 1 MAY 2020.
Citações Web of Science: 0
Resumo

The quiescent emission of the anomalous X-ray pulsar (AXP) 4U 0142+61 extends over a broad range of energy, from radio up to hard X-rays. In particular, this object is unique among soft gamma-ray repeaters (SGRs) and AXPs in presenting simultaneously mid-infrared emission and pulsed optical emission. In spite of the many propositions to explain this wide range of emission, it still lacks one that reproduces all of the observations. Filling this gap, we present a model to reproduce the quiescent spectral energy distribution of 4U 0142+61 from mid-infrared up to hard X-rays using plausible physical components and parameters. We propose that the persistent emission comes from a magnetic accreting white dwarf (WD) surrounded by a debris disk. This model assumes that (i) the hard X-rays are due to the bremsstrahlung emission from the postshock 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 postshock region emission. In this scenario, the fitted model parameters indicate that 4U 0142+61 harbors a fast-rotator magnetic near-Chandrasekhar WD, which is very hot and hence young. Such a WD can be the recent outcome of a merger of two less massive WDs. In this case, 4U 0142+61 can evolve into a supernova Ia and hence give hints of the origin of these important astrophysical events. Additionally, we also present a new estimate of 4U 0142+61's distance, 3.78(-0.18)(+0.12) kpc, based on the measured hydrogen column density and new interstellar extinction 3D maps. (AU)

Processo FAPESP: 15/25972-0 - Desenvolvimento e caracterização do sistema de detectores do experimento MIRAX
Beneficiário:Manuel Antonio Castro Ávila
Linha de fomento: Bolsas no Brasil - Pós-Doutorado
Processo FAPESP: 13/26258-4 - Matéria superdensa no universo
Beneficiário:Manuel Máximo Bastos Malheiro de Oliveira
Linha de fomento: Auxílio à Pesquisa - Temático
Processo FAPESP: 13/15088-0 - Magnetares e os pulsares de anãs brancas magnetizadas, muito rápidas, massivas e estranhas e a geração de ondas gravitacionais
Beneficiário:Jaziel Goulart Coelho
Linha de fomento: Bolsas no Brasil - Pós-Doutorado