dc.date.accessioned | 2019-06-27T16:01:27Z | |
dc.date.accessioned | 2022-10-18T22:26:39Z | |
dc.date.available | 2019-06-27T16:01:27Z | |
dc.date.available | 2022-10-18T22:26:39Z | |
dc.date.created | 2019-06-27T16:01:27Z | |
dc.date.issued | 2018 | |
dc.identifier | http://hdl.handle.net/10533/236158 | |
dc.identifier | 1150411 | |
dc.identifier.uri | https://repositorioslatinoamericanos.uchile.cl/handle/2250/4467494 | |
dc.description.abstract | Millisecond pulsars are old, fast spinning neutron stars thought to have evolved from classical
pulsars in binary systems, where the rapid rotation is caused by the accretion of matter
and angular momentum from their companion. During this transition between classical and
millisecond pulsars, there is a magnetic field reduction of ∼ 4 orders of magnitude, which
is not well understood. According to the standard scenario, the magnetic field is reduced as
a consequence of accretion, either through ohmic dissipation or through screening by the
accreted matter. We explored an alternative hypothesis in which the magnetic field is reduced
through ambipolar diffusion before the accretion. This is particularly effective during the long
epoch in which the pulsar has cooled, but has not yet started accreting. This makes the final
magnetic field dependent on the evolution time of the companion star and thus its initial mass.
We use observed binary systems to constrain the time available for the magnetic field decay
based on the current pulsar companion: a helium white dwarf, a carbon-oxygen white dwarf,
or another neutron star. Based on a simplified model without baryon pairing, we show that the
proposed process agrees with the general distribution of observed magnetic field strengths in
binaries, but is not able to explain some mildly recycled pulsars where no significant decay
appears to have occurred. We discuss the possibility of other formation channels for these
systems and the conditions under which the magnetic field evolution would be set by the
neutron star crust rather than the core.
Key words: magnetic fields – stars: neutron – pulsars: general – stars: white dwarfs – X-rays:
binaries | |
dc.language | eng | |
dc.relation | https://arxiv.org/pdf/1906.06076.pdf | |
dc.relation | info:eu-repo/grantAgreement//1150411 | |
dc.relation | info:eu-repo/semantics/dataset/hdl.handle.net/10533/93482 | |
dc.relation | instname: Conicyt | |
dc.relation | reponame: Repositorio Digital RI2.0 | |
dc.rights | http://creativecommons.org/licenses/by-nc-nd/3.0/cl/ | |
dc.rights | info:eu-repo/semantics/openAccess | |
dc.rights | Attribution-NonCommercial-NoDerivs 3.0 Chile | |
dc.title | On the weak magnetic field of millisecond pulsars: Does it decay before accretion? | |
dc.type | Manuscrito | |