Recent release, passed through Ned Wright's Cosmology site: http://www.astro.ucla.edu/~wright/cosmolog.htm#04Dec03 "A Double Radio Pulsar. 9 Jan 2004 - Lyne et al. (2004, Science in press) gives the details about PSR J0737-3039 A&B, the double radio pulsar binary with a relativistic orbit, previously reported as a single pulsar in a binary system on 4 Dec 2003. The mass of the 23 millisecond pulsar (A) is 1.337+/-0.005 M(sun) while the mass of the 2.8 second pulsar (B) is 1.250+/-0.005 M(sun). There are now 6 measured constraints on (MA,MB) and the values given above are consistent with all 6 constraints, providing a stringent test of General Relativity which GR passes with flying colors". And: "An amazing binary pulsar. 4 Dec 03 - Nature today published a paper (Burgay et al. 2003, Nature, 426, 531-533) about a newly announced millisecond pulsar, PSR J0737-3039, in a relativistic binary system. Radio pulsars are neutron stars (NS) which have a mass of about 1.4 solar masses and a radius of 10 km, magnetic fields billions to trillions of times larger than the Earth's magnetic field, and spin periods from 1.6 milliseconds to several seconds. PSR J0737-3039 is orbiting another neutron star every 2.4 hours and the two stars will merge in 85 Myr due to gravitational radiation. Hence LIGO will have many more detectable NS+NS merger events based on the statistics of two objects instead of the previous estimate based solely on the one merging binary pulsar PSR B1913+16 known earlier. There is currently a program on the GBT radiotelescope schedule entitled "RRS Observations of the Double Binary Pulsar PSR J0737-3039" indicating that this is more than just a pulsar in orbit around a neutron star. And there is a Director's Discretionary Time Chandra observing proposal that says that both neutron stars in this system are pulsars, the previously announced pulsar with 22 millisecond period and a 2.7 second period for the companion. The millisecond pulsar (A) is eclipsed for 22 seconds as it passes behind the slow pulsar (the B component). Since the relative motion of the two stars is 14,000 km in 22 seconds, this eclipse must be caused by a wind coming from the B component instead of the disk of the neutron star which is tiny".