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Albert is Still Looking Good.

  1. Jan 9, 2004 #1


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    Recent release, passed through Ned Wright's Cosmology site:

    "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
  2. jcsd
  3. Jan 9, 2004 #2


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    Dearly Missed

    great news Labguy, thanks for posting this!
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