Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...20925405z&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #254.05; Bulletin of the American Astronomical Society,
Astronomy and Astrophysics
Astronomy
Scientific paper
The young, high dE/dt pulsars B1951+32 and B1757-24 were observed over 14.5 yr and 6.5 yr, respectively, with the Very Large Array in L-band spectral-line mode. Both pulsars have been associated with complex supernova remnants: B1951+32 lies in the plerionic core of CTB 80 (G69.0+2.7) and B1757-24 leads the beak of the Duck (G5.27-0.90, G5.4-1.2) and lies near the galactic center. Long time-baseline astrometry has been used to understand better the births and evolution of both pulsars.
The observed proper motion of B1951+32 is $-28.8±0.9 mas yr-1 R.A. and -14.5±0.9 mas yr-1 Dec; for B1757-24, a proper motion of -4.0±4.1 mas yr-1 R.A. and -6.8±9.0 mas yr-1 Dec. was observed. Both measurements are presented without accounting for differential galactic rotation. The measurements agree with previous observations but place tighter constraints on evolutionary models. Observations give the true age of B1951+32 at 58±1 kyr if it is associated with the infrared and H I shells of CTB 80, significantly less than the characteristic spin-down age of 107 kyr. Observations of B1757-24 cannot provide significant evidence of motion, but 2-σ proper motion indicates an upper age limit of 11.2 kyr if it is associated with the head of the Duck remnant and 135 kyr if it is associated with the body; the characteristic age of B1747-24 is 15.5 kyr. If both pulsars are much younger than their characteristic ages, these results indicate that braking mechanisms or evolutionary processes of the pulsars are not well approximated by the characteristic approximation.
Brisken Walter
Chatterjee Saikat
Zeiger Benjamin
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