@Article{CoelhoAraúLadiNune:2021:CaCrVe,
               author = "Coelho, Jaziel G. and Ara{\'u}jo, Jos{\'e} Carlos Neves de and 
                         Ladislau, Samantha Monaliza and Nunes, Rafael da Costa",
          affiliation = "{Universidade Tecnol{\'o}gica Federal do Paran{\'a} (UTFPR)} and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)}",
                title = "Observational Constraints on the Pulsar Wind Model: The Cases of 
                         Crab and Vela",
              journal = "Astrophysical Journal",
                 year = "2021",
               volume = "920",
               number = "1",
                pages = "e57",
                month = "Oct.",
             abstract = "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.",
                  doi = "10.3847/1538-4357/ac1d41",
                  url = "http://dx.doi.org/10.3847/1538-4357/ac1d41",
                 issn = "0004-637X and 1538-4357",
             language = "en",
           targetfile = "coelho_observational.pdf",
        urlaccessdate = "05 maio 2024"
}