Evidence for alignment of the rotation and velocity vectors in pulsars. II. Further data and emission heights

By Simon Johnston, G. Hobbs, S. Vigeland, Michael Kramer, J. Weisberg, Andrew G. Lyne. 2005

198 citations recorded by the source corpus.

We have conducted observations of 22 pulsars at frequencies of 0.7, 1.4 and 3.1 GHz and present their polarization profiles. The observations were carried out for two main purposes. First, we compare the orientation of the spin and velocity vectors to verify the proposed alignment of these vectors by Johnston et al. We find, for the 14 pulsars for which we were able to determine both vectors, that seven are plausibly aligned, a fraction which is lower than, but consistent with, earlier measurements. Secondly, we use profiles obtained simultaneously at widely spaced frequencies to compute the radio emission heights. We find, similar to other workers in the field, that radiation from the centre of the profile originates from lower in the magnetosphere than the radiation from the outer parts of the profile.

Subfields: Astronomy and Astrophysics, Oceanography, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/6d1f00b7e5131b481a7836ebdd94f159acbceed9

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Citations in the corpus

Massive runaway and walkaway stars (2018, background): “…direction is assumed to be isotropically distributed in the frame of the collapsing star (Wongwathanarat et al. 2013; Bear & Soker 2017), although Johnston et al. (2005) and Kaplan et al. (2008) suggest that there is weak evidence for kick-spin alignment in well observed pulsars such as the Crab…”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, background): “…that we do not find any correlation of spin and kick directions in our explosion models of nonrotating progenitor stars, and a possible spin-kick alignment suggested by observations (e.g., Johnston et al. 2005, 2007; Kaplan et al. 2008; also see Wang et al. 2006, 2007) remains unexplained.”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, result): “This seems to be compatible with recent studies of observational constraints on neutron star kicks for isolated pulsars and for neutron stars in binary systems (Wang et al. 2006), although the interpretation of observations is still ambiguous (Johnston et al. 2005).”
Science with the Murchison Widefield Array (2012, background): “Statistics derived from average pulse profiles may be among the best probes of complicated phenomena like corecollapse supernova (e.g., Johnston et al. 2005).”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “Observations have suggested a tendency towards spin-kick alignment in young pulsars (Johnston et al. 2005; Ng & Romani 2007; Noutsos et al. 2012, 2013; but see also Kaplan et al. 2008 for difficulties in determining the angle between the spin axis and the kick velocity).”