Acceleration of pulsars by asymmetric radiation

Harrison, Edward; Tademaru, E.

doi:10.1086/153907

Cited by 174 publications

(146 citation statements)

References 0 publications

Supporting

Mentioning

142

Contrasting

Order By: Relevance

“…Lai, Cherno †, & Cordes 2001). We also note that alignment of the spin axis and proper motion is a natural consequence of the Harrison & Tademaru (1975) photon rocket acceleration mechanism. With the recent revision of Lai et al (2001), an initial spin period as long as 6 ms suffices to account for the measured transverse component of the velocity in the maximum acceleration case.…”

Section: Implications Of the Proper Motionmentioning

confidence: 62%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

288

305

View full text Add to dashboard Cite

We present high-resolution Chandra X-ray observations of PSR B0833[45, the 89 ms pulsar associated with the Vela supernova remnant. We have acquired two observations separated by 1 month to search for changes in the pulsar and its environment following an extreme glitch in its rotation frequency. We Ðnd a well-resolved nebula with a toroidal morphology remarkably similar to that observed in the Crab Nebula, along with an axial Crab-like jet. Between the two observations, taken D3 ] 105 s and D3 ] 106 s after the glitch, the Ñux from the pulsar is found to be steady to within 0.75% ; the 3 p limit on the fractional increase in the pulsarÏs X-ray Ñux is of the inferred glitch energy. We use [10~5 this limit to constrain parameters of glitch models and neutron star structure. We do Ðnd a signiÐcant increase in the Ñux of the nebulaÏs outer arc ; if associated with the glitch, the inferred propagation velocity is similar to that seen in the brightening of the Crab Nebula wisps. We propose an explana-Z0.7c, tion for the X-ray structure of the Vela synchrotron nebula based on a model originally developed for the Crab Nebula. In this model, the bright X-ray arcs are the shocked termination of a relativistic equatorial pulsar wind that is contained within the surrounding kidney-bean shaped synchrotron nebula comprising the postshock, but still relativistic, Ñow. In a departure from the Crab model, the magnetization parameter p of the Vela pulsar wind is allowed to be of order unity ; this is consistent with the simplest MHD transport of magnetic Ðeld from the pulsar to the nebula, where B ¹ 4 ] 10~4 G. The inclination angle of the axis of the equatorial torus with respect to the line of sight is identical to that of the rotation axis of the pulsar as previously measured from the polarization of the radio pulse. The projection of the rotation axis on the sky may also be close to the direction of proper motion of the pulsar if previous radio measurements were confused by orthogonal-mode polarized components. We review e †ects that may enhance the probability of alignment between the spin axis and space velocity of a pulsar, and speculate that short-period, slowly moving pulsars are just the ones best-suited to producing synchrotron nebulae with such aligned structures. Previous interpretations of the compact Vela nebula as a bow-shock in a very weakly magnetized wind su †ered from data of inadequate spatial resolution and less plausible physical assumptions.

show abstract

Section: Implications Of the Proper Motionmentioning

confidence: 62%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

288

305

View full text Add to dashboard Cite

show abstract

“…The general assumption for explaining the high velocities is that, during a certain time period in their evolution, neutron stars experience an accelerating kick, a so-called pulsar kick. This could be induced by a hydrodynamic mechanism (Burrows et al 2006;Janka et al 2007), based on an asymmetric supernova explosion, disruption of binary systems (Gott et al 1970) or asymmetric low-frequency electromagnetic radiation due to an off-centred rotating dipole (Harrison & Tademaru 1975; for an overview see e.g. Wang et al 2006;Lai et al 2001).…”

Section: Pulsar Kicksmentioning

confidence: 99%

Pulsar kicks by anisotropic neutrino emission from quark matter in strong magnetic fields

Sagert¹,

Schaffner-Bielich²

2008

A&A

View full text Add to dashboard Cite

Aims. We critically discuss a pulsar acceleration mechanism based on asymmetric neutrino emission from the direct quark Urca process in the interior of proto neutron stars. Methods. The neutrinos are emitted by the cooling strange quark matter core with an anisotropy caused by a strong magnetic field. We calculate the kick velocity of the proto neutron star in dependence of the temperature and radius of the quark phase. The results are compared with the necessary magnetic field strength, as well as the neutrino mean free path. Results. We find that within a quark phase radius of 10 km and temperatures higher than 5 MeV kick velocities of 1000 km s −1 can be reached only when neutrino quark scattering is ignored. When taking the neutrino mean free paths in quark matter into account kick velocities higher than 100 km s −1 cannot be reached. The same holds even when effects from colour superconductivity are included. For pulsar kicks powered by quark phase transitions from an ungapped quark phase to the CFL phase the final velocity depends crucially on the pairing gap and the quark chemical potential and reaches 1000 km s −1 only in marginal cases. Conclusions. We find that the phenomenon of pulsar kick velocities higher than 100 km s −1 cannot be explained by asymmetric neutrino emission from either cooling normal strange quark or colour superconducting quark matter due to the small neutrino mean free paths. If neutrinos are produced by a phase transition to colour-superconducting quark matter, high kick velocities can only be reached for temperatures below 1 MeV.

show abstract

“…Lyne & Lorimer (1994) and Hobbs et al (2005) analysed a large number of pulsar proper motions and demonstrated that their transverse velocities are typically several hundred km s −1 . Various explanations have been proposed for these high velocities, including a postnatal electromagnetic rocket mechanism (Harrison & Tademaru 1975), asymmetric neutrino emission in the presence of super-strong magnetic fields (Lai & Qian 1998), hydrodynamical instabilities in the collapsed supernova core (Lai & Goldreich 2000) and the asymmetric explosion of γ-ray bursts (Cui et al 2007). Knowledge of pulsar proper motions and velocities is essential for many aspects of pulsar and neutron star astrophysics including determinations of the birth rate of pulsars, associations with supernova remnants and the Galactic distribution of the progenitor population.…”

Section: Introductionmentioning

confidence: 99%

Proper motions of 15 pulsars: a comparison between Bayesian and frequentist algorithms

Wang

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present proper motions for 15 pulsars which are observed regularly by the Nanshan 25-m radio telescope. Two methods, the frequentist method (Coles et al. 2011) and the Bayesian (Lentati et al. 2014) method, are used and the results are compared. We demonstrate that the two methods can be applied to young pulsar data sets that exhibit large amounts of timing noise with steep spectral exponents and give consistent results. The measured positions also agree with very-long-baseline interferometric positions. Proper motions for four pulsars are obtained for the first time, and improved values are obtained for five pulsars.

show abstract

Acceleration of pulsars by asymmetric radiation

Cited by 174 publications

References 0 publications

Vela Pulsar and Its Synchrotron Nebula

Vela Pulsar and Its Synchrotron Nebula

Pulsar kicks by anisotropic neutrino emission from quark matter in strong magnetic fields

Proper motions of 15 pulsars: a comparison between Bayesian and frequentist algorithms

Contact Info

Product

Resources

About