Discovery of Two High Magnetic Field Radio Pulsars

By F. Camilo, Victoria Kaspi, Andrew G. Lyne, R. Manchester, J. Bell, N. D'Amico, N. McKay, F. University, Mit, J. Bank and 2 more. 2000

208 citations recorded by the source corpus.

We report the discovery of two young isolated radio pulsars with very high inferred magnetic fields. PSR J1119-6127 has period P = 0.407 s, and the largest period derivative known among radio pulsars, Ṗ = 4.0 × 10-12. Under standard assumptions these parameters imply a characteristic spin-down age of only τc = 1.6 kyr and a surface dipole magnetic field strength of B = 4.1 × 1013 G. We have measured a stationary period second derivative for this pulsar, resulting in a braking index of n = 2.91 ± 0.05. We have also observed a glitch in the rotation of the pulsar, with fractional period change ΔP/P = -4.4 × 10-9. Archival radio imaging data suggest the presence of a previously uncataloged supernova remnant centered on the pulsar. The second pulsar, PSR J1814-1744, has P = 3.975 s and Ṗ = 7.4 × 10-13. These parameters imply τc = 85 kyr, and B = 5.5 × 1013 G, the largest of any known radio pulsar. Both PSR J1119-6127 and PSR J1814-1744 show apparently normal radio emission in a regime of magnetic field strength where some models predict that no emission should occur. Also, PSR J1814-1744 has spin parameters similar to the anomalous X-ray pulsar (AXP) 1E 2259+586, but shows no discernible X-ray emission. If AXPs are isolated, high magnetic field neutron stars ("magnetars"), these results suggest that their unusual attributes are unlikely to be merely a consequence of their very high inferred magnetic fields.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7310cd961d384f9e11ec67b022b429f06ca52d87

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Citations in the corpus

A study of 315 glitches in the rotation of 102 pulsars (2011, unknown): “…by guest on 30 July 2018 Table 1 – continued Name J name No. of MJD ν/ν ν̇/ν̇ Referencesa Glitches (d) (10−9) (10−3) J1105−6107 1105−6107 1 50417(16) 279.7(2) 4.63(4) Wang et al. (2000) J1105−6107 1105−6107 2 50610(3) 2(3) 0.19(1) Wang et al. (2000)…”
Avalanche Dynamics of Radio Pulsar Glitches (2007, unknown): “…(12) Downs 1981; (13) Wang et al. 2000; (14) Dodson et al. 2002; (15) Dodson et al. 2004; (16) Flanagan & Buchner 2006; (17) Hobbs et al. 2004b; (18) Camilo et al. 2000; (19) Camilo et al. 2004; (20) Torii et al. 2000; (21) Kaspi et al. 2000; (22) Kaspi & Gavriil 2003; (23) Shemar & Lyne 1996;…”
Detection of 107 glitches in 36 southern pulsars (2012, unknown): “The first is small c© 0000 RAS, MNRAS 000, 000–000 Glitches in 36 southern pulsars 11 with ∆νg/ν ∼ 4 × 10 −9 as was reported by Camilo et al. (2000).”
A UNIFIED MODEL OF THE MAGNETAR AND RADIO PULSAR BURSTING PHENOMENOLOGY (2011, background): “…any bursting behaviour, has raised another obvious quetion: why some “high-B” pulsars (PSR J1119-6127 and PSR J1814-1744) do not display any discernable X-ray emission nor outburst (Camilo et al. 2000), while at least one case of “low-B” NS does, if the magnetic field is their driving force ?”
The glitch-induced identity changes of PSR J1119−6127 (2010, methodology): “The pulse profile of PSR J1119–6127 is well known to be single-peaked (see e.g. Camilo et al. 2000; Johnston & Weisberg 2006).”
NEUTRINO EMISSION FROM COOPER PAIRS AND MINIMAL COOLING OF NEUTRON STARS (2009, methodology): “As the measured braking index n = 2.9 (Camilo et al. 2000) is compatible with magneto-dipolar breaking, and the characteristics of the associated SNR and the Pulsar Wind Nebula (PWN) are compatible with an age close to tsd (Safi-Harb & Kumar 2008), we adopt an age estimate of (0.5 − 2) × tsd. PSR…”
Young Core-Collapse Supernova Remnants and Their Supernovae (2004, unknown): “2 0.5 (Camilo et al. 2000), and 1:4 0:2 for the Vela pulsar (Lyne et al. 1996).”
The Parkes multi-beam pulsar survey - I. Observing and data analysis systems, discovery and timing of 100 pulsars (2001, background): “Camilo et al. (2000b) report the discovery of two young pulsars, J1119–6127 and J1814–1744, which have the highest surface dipole magnetic field strengths among known radio pulsars.”
The Parkes Multibeam Pulsar Survey – II. Discovery and timing of 120 pulsars (2002, background): “Camilo et al. (2000) discuss PSR J1814−1744, the inferred surface magnetic field strength of which, Bs = 5.5 × 1013 G, is the largest of any known radio pulsar.”
The Parkes Multibeam Pulsar Survey - III. Young Pulsars and the Discovery and Timing of 200 Pulsars (2003, methodology): “It has found a large number of young (e.g. Camilo et al. 2000, D’Amico et al. 2001), distant (this work), exotic (Lyne et al. 2000, Kaspi et al. 2000b, Stairs et al. 2001, Camilo et al. 2001b) and glitching pulsars (Hobbs et al. 2002) buried in the inner Galactic plane (|b| < 5◦,-100◦ < l < 50◦).”