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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.)

Relating braking indices of young pulsars to the dynamics of superfluid cores

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Autor(es):
Oliveira, H. O. [1] ; Magalhaes, N. S. [1, 2] ; Marinho, Jr., R. M. [1] ; Carvalho, G. A. [3, 4, 5, 1] ; Frajuca, C. [6]
Número total de Autores: 5
Afiliação do(s) autor(es):
[1] Technol Inst Aeronaut, Grad Program Phys, Praca Marechal Eduardo Gomes 50, BR-12228900 Sao Jose Dos Campos, SP - Brazil
[2] Univ Fed Sao Paulo, Dept Phys, Rua Sao Nicolau 210, BR-09913030 Diadema, SP - Brazil
[3] Sapienza Univ Roma, Dipartimento Fis, Ple Aldo Moro 5, I-00185 Rome - Italy
[4] Sapienza Univ Roma, ICRA, Ple Aldo Moro 5, I-00185 Rome - Italy
[5] ICRANet, Pzza Repubbl 10, I-65122 Pescara - Italy
[6] Fed Inst Educ Sci & Technol Sao Paulo, R Pedro Vicente 625, BR-01109010 Sao Paulo, SP - Brazil
Número total de Afiliações: 6
Tipo de documento: Artigo Científico
Fonte: Journal of Cosmology and Astroparticle Physics; n. 11 NOV 2018.
Citações Web of Science: 0
Resumo

Pulsars are stars that emit electromagnetic radiation in well-defined time intervals. The frequency of such pulses decays with time as is quantified by the braking index (n). In the canonical model n = 3 for all pulsars, but observational data show that n not equal 3, indicating a limitation of the model. In this work we present a new approach to study the frequency decay of the rotation of a pulsar, based on an adaptation of the canonical one. We consider the pulsar a star that rotates in vacuum and has a strong magnetic field but, differently from the canonical model, we assume that its moment of inertia changes in time due to a uniform variation of a displacement parameter in time. We found that the braking index results smaller than the canonical value as a consequence of an increase in the star's displacement parameter, whose variation is small enough to allow plausible physical considerations that can be applied to a more complex model for pulsars in the future. In particular, this variation is of the order of neutron vortices' creep in rotating superfluids. When applied to pulsar data our model yielded values for the stars' braking indices close to the observational ones. The application of this approach to a more complex star model, where pulsars are assumed to have superfluid interiors, is the next step in probing it. We hypothesize that the slow expansion of the displacement parameter might mimic the motion of core superfluid neutron vortices in realistic models. (AU)

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: 08/57807-5 - Instituto Nacional Avançado de Astrofísica
Beneficiário:João Evangelista Steiner
Linha de fomento: Auxílio à Pesquisa - Temático