Test of pulsar acceleration mechanisms

Morris, David J.; Radhakrishnan, V.; Shukre, C. S.

doi:10.1038/260124a0

Cited by 15 publications

(5 citation statements)

References 8 publications

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“…In this paper, we propose an alternative explanation of the age discrepancy because PSR J 0538+2817 could be the stellar remnant of the first supernova (SN) explosion in a massive binary system and therefore could be as old as indicated by its characteristic age (cf. Morris et al 1978). Our proposal implies that S 147 is the diffuse remnant of the second SN explosion (that disrupted the binary system) and that a much younger second NS (not necessarily manifesting itself as a radio pulsar) should be associated with S 147.…”

Section: Introductionmentioning

confidence: 80%

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Supernova remnant S 147 and its associated neutron star(s)

Gvaramadze

2006

A&A

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The supernova remnant S 147 harbors the pulsar PSR J 0538+2817 whose characteristic age is more than an order of magnitude greater than the kinematic age of the system (inferred from the angular offset of the pulsar from the geometric center of the supernova remnant and the pulsar proper motion). To reconcile this discrepancy we propose that PSR J 0538+2817 could be the stellar remnant of the first supernova explosion in a massive binary system and therefore could be as old as its characteristic age. Our proposal implies that S 147 is the diffuse remnant of the second supernova explosion (that disrupted the binary system) and that a much younger second neutron star (not necessarily manifesting itself as a radio pulsar) should be associated with S 147. We use the existing observational data on the system to suggest that the progenitor of the supernova that formed S 147 was a Wolf-Rayet star (so that the supernova explosion occurred within a wind bubble surrounded by a massive shell) and to constrain the parameters of the binary system. We also restrict the magnitude and direction of the kick velocity received by the young neutron star at birth and find that the kick vector should not strongly deviate from the orbital plane of the binary system.

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Section: Introductionmentioning

confidence: 80%

“…Morris et al 1978). Our proposal implies that S 147 is the diffuse remnant of the second SN explosion (that disrupted the binary system) and that a much younger second NS (not necessarily manifesting itself as a radio pulsar) should be associated with S 147.…”

Section: Introductionmentioning

confidence: 99%

Supernova remnant S 147 and its associated neutron star(s)

Gvaramadze

2006

A&A

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“…Tademaru & Harrison (1975) proposed the so‐called rocket mechanism whereby an offset of the magnetic dipole from the centre of the star causes the star to accelerate along its rotation axis. Observational tests of this mechanism by Morris, Radhakrishnan & Shukre (1976) and Tademaru (1977) reached opposing conclusions, with the former claiming no correlation between the velocity vector and the spin axis, and the latter claiming a good correlation. Following this, Anderson & Lyne (1983) revisited the issue with an updated data base of pulsar proper motions.…”

Section: Introductionmentioning

confidence: 99%

Evidence for alignment of the rotation and velocity vectors in pulsars

Johnston

Hobbs

Vigeland

et al. 2005

Monthly Notices of the Royal Astronomical Society

228

245

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We present strong observational evidence for a relationship between the direction of a pulsar's motion and its rotation axis. We show carefully calibrated polarization data for 25 pulsars, 20 of which display linearly polarized emission from the pulse longitude at closest approach to the magnetic pole. Such data allow determination of the position angle of the linear polarisation which in turn reflects the position angle of the rotation axis. Of these 20 pulsars, 10 show an offset between the velocity vector and the polarisation position angle which is either less than 10\degr or more than 80\degr, a fraction which is very unlikely by random chance. We believe that the bimodal nature of the distribution arises from the presence of orthogonal polarisation modes in the pulsar radio emission. In some cases this orthogonal ambiguity is resolved by observations at other wavelengths so that we conclude that the velocity vector and the rotation axis are aligned at birth. Strengthening the case is the fact that 4 of the 5 pulsars with ages less than 3 Myr show this relationship, including the Vela pulsar. We discuss the implications of these findings in the context of the Spruit & Phinney (1998)\nocite{sp98} model of pulsar birth-kicks. We point out that, contrary to claims in the literature, observations of double neutron star systems do not rule out aligned kick models and describe a possible observational test involving the double pulsar system.Comment: MNRAS, In Pres

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“…And in fact, most of the pulsars discovered (about 300) are related to various nebulas--the remains of different supernovas. [5][6][7][8] The youngest pulsars, such as PSR 0532 +21 and PSR 0833 -45, are located in the Crab nebula and in the remains of the supernova Vela X, respectively (following the letters PSR, which denote pulsar, the galactic coordinates of these objects are given--the first four figures denote declination in hours and minutes, the last two denote right ascension in degrees). It is suggested that the pulsar PSR 0531 +21 was born in 1054 A.D. when a "heavenly guest" (so called by the Japanese and Chinese astronomers who observed the phenomenon) appeared--a star which blazed up abruptly in the constellation Taurus and was seen even in the daytime.…”

Section: Introductionmentioning

confidence: 99%