%0 Journal Article
%4 sid.inpe.br/mtc-m21d/2021/10.25.19.18
%2 sid.inpe.br/mtc-m21d/2021/10.25.19.18.17
%@doi 10.3847/1538-4357/ac1d41
%@issn 0004-637X
%@issn 1538-4357
%T Observational Constraints on the Pulsar Wind Model: The Cases of Crab and Vela
%D 2021
%8 Oct.
%9 journal article
%A Coelho, Jaziel G.,
%A Araújo, José Carlos Neves de,
%A Ladislau, Samantha Monaliza,
%A Nunes, Rafael da Costa,
%@affiliation Universidade Tecnológica Federal do Paraná (UTFPR)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@electronicmailaddress jazielcoelho@utfpr.edu.br
%@electronicmailaddress jcndearaujo@gmail.com
%@electronicmailaddress smladislau@gmail.com
%@electronicmailaddress rafadcnunes@gmail.com
%B Astrophysical Journal
%V 920
%N 1
%P e57
%X As is well known, pulsars are extremely stable rotators. However, although slowly, they spindown thanks to brake mechanisms, which are in fact still a subject of intense investigation in the literature. Since pulsars are usually modeled as highly magnetized neutron stars that emit beams of electromagnetic radiation out of their magnetic poles, it is reasonable to consider that the spindown has to do with a magnetic brake. Although an interesting and simple idea, a pure magnetic brake is not able to adequately account for the spindown rate. Thus, many alternative spindown mechanisms appear in the literature, among them the pulsar wind model, where the wind of particles coming from the pulsar itself can carry part of its rotational kinetic energy. Such a spindown mechanism depends critically on three parameters, namely, the dipole magnetic field (B), the angle between the magnetic and rotation axes (phi), and the density of primary particles (zeta) of the pulsar's magnetosphere. Differently from a series of articles in this subject, we consider for the first time in the literature a statistical modeling that includes a combination of a magnetic dipole and wind brakes. As a result, we are able to constrain the above referred parameters in particular for Crab and Vela pulsars.
%@language en
%3 coelho_observational.pdf