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Title:
Constraining Binary Stellar Evolution With Pulsar Timing
Authors:
Ferdman, Robert D.; Stairs, I. H.; Backer, D. C.; Burgay, M.; Camilo, F.; D'Amico, N.; Demorest, P.; Faulkner, A.; Hobbs, G.; Kramer, M.; Lorimer, D. R.; Lyne, A. G.; Manchester, R.; McLaughlin, M.; Nice, D. J.; Possenti, A.
Affiliation:
AA(University of British Columbia, Canada), AB(University of British Columbia, Canada), AC(University of California, Berkeley), AD(Istituto Nazionale di Astrofisica, Italy), AE(Columbia University), AF(Istituto Nazionale di Astrofisica, Italy), AG(University of California, Berkeley), AH(Jodrell Bank Observatory, United Kingdom), AI(Australia Telescope National Facility, Australia), AJ(Jodrell Bank Observatory, United Kingdom), AK(Jodrell Bank Observatory, United Kingdom), AL(Jodrell Bank Observatory, United Kingdom), AM(Australia Telescope National Facility, Australia), AN(Jodrell Bank Observatory, United Kingdom), AO(Bryn Mawr College), AP(Istituto Nazionale di Astrofisica, Italy)
Publication:
American Astronomical Society Meeting 208, #4.08; Bulletin of the American Astronomical Society, Vol. 38, p.82
Publication Date:
06/2006
Origin:
AAS
Bibliographic Code:
2006AAS...208.0408F

Abstract

The Parkes Multibeam Pulsar Survey has yielded a significant number of very interesting binary and millisecond pulsars. Two of these objects are part of an ongoing timing study at the Green Bank Telescope (GBT). PSR J1756-2251 is a double-neutron star (DNS) binary system. It is similar to the original Hulse-Taylor binary pulsar system PSR B1913+16 in its orbital properties, thus providing another important opportunity to test the validity of General Relativity, as well as the evolutionary history of DNS systems through mass measurements. PSR J1802-2124 is part of the relatively new and unstudied "intermediate-mass" class of binary system, which typically have spin periods in the tens of milliseconds, and/or relatively massive (> 0.7 solar masses) white dwarf companions. With our GBT observations, we have detected the Shapiro delay in this system, allowing us to constrain the individual masses of the neutron star and white dwarf companion, and thus the mass-transfer history, in this unusual system.
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