The Structure and Signals of Neutron Stars, from Birth to Death

Session

Afternoon session - Parallel B

25 Mar 2014, 14:30

Conveners

Afternoon session - Parallel B

• Alice Harding (NASA, USA)

146. Origin and evolution of magnetars

Dr Sergei Popov (SAI Moscow)

25/03/2014, 14:30

Up to now it is unclear how magnetars obtain their large magnetic fields. In the standard model it is proposed that fields are enhanced via a dynamo mechanism. This scenario requires that the neutron star has very rapid initial rotation. Such assumption, on one hand, requires rapid rotation of the progenitor, and so a specific evolution; on another hand, this assumption leads us to...

82. Partially Screened Gap in Pulsars

Dr Andrzej Szary (Kepler Institute of Astronomy, Univ. Zielona Gora, Poland)

25/03/2014, 14:50

Coherent pulsar radio emission requires an existence of inner acceleration region above the polar cap. The most advanced implementation of the inner gap idea is the Partially Screened Gap (PSG) model, based on recent calculations of the surface binding energy and Hall drift induced surface magnetic field in neutron stars. The PSG model has a great predictive power and can be tested...

55. Clues to the formation and evolution of magnetars from X-ray observations of the associated supernova remnants

Toshio Nakano (University of tokyo)

25/03/2014, 15:10

Magnetars, i.e., neutron stars (NSs) with extremely strong magnetic fields, are thought to be produced by Type II supernovae (SNe), like other NSs. Indeed, several of them are located inside supernova remnants (SNRs). However, we do not know how the magnetar-producing SNe differ from those creating the other NSs. Observations of the SNRs associated with magnetars are expected to provide...

1. Effect of strong magnetic fields on the nuclear “pasta” phase structure

Dr Rafael C. R. de Lima (Universidade do Estado de Santa Catarina)

25/03/2014, 15:30

The effect of strong magnetic fields on the properties of the pasta structure is calculated within a Thomas-Fermi approach using relativistic mean-field models to modulate stellar matter. It is shown how quantities such as the size of the clusters and Wigner-Seitz cells, the surface tension, and the transition between configurations are affected. It is expected that these effects may give...

14. Stellar compact objects under strong magnetic fields

Dr Rudiney Casali (Institut de Physique Nucléaire de Lyon)

25/03/2014, 15:45

We apply magnetic fields of the order of 10^17 G and 10^18 G to nuclear matter, and study its influence on the symmetry energy and its slope. We also study the effects caused by the inclusion of anomalous magnetic moments to these quantities. Then, we investigate the effects caused by strong magnetic fields on the properties of compact objects, composed by hadronic matter in β-equilibrium,...

88. What makes magnetars (as well as normal pulsars) radio laud?

Prof. George Melikidze (J. Kepler Institute of Astronomy, University of Zielona Gora, Poland)

25/03/2014, 16:00

We present circumstances that should be fulfilled in the magnetosphere of the neutron stars to “switch” the mechanism for radio emission on. We claim that the curvature of magnetic field lines at the stellar surface is the most influential factor affecting the radio emission process. The most plausible mechanism for the radio emission which most probably is the coherent curvature radiation...

90. Azimuthally-structured radio beams of pulsars

Dr Jaroslaw Dyks (Nicolaus Copernicus Astronomical Center)

25/03/2014, 16:15

There is a growing evidence that radio beams of some pulsars are azimuthally-structured. When viewed down the dipole axis, the beam resembles spokes in a wheel, with narrow emission stripes spreading away from the dipole axis. I will present objects for which the spoke-like model describes their profiles more successfully than the traditional conal geometry. Further from the dipole...