The discovery of the first double pulsar

PSR J0737-3039A, a millisecond pulsar with a spin period of 22.7 ms, was discovered in April 2003 27 . The original discovery record showed a strongly varying Doppler shift, corresponding an acceleration of 99 m s2 suggesting a binary period of just few hours for a companion of 1 M (as a comparison, the typical observed binary pulsars having a 0.2 0.3 M white dwarf companion display acceleration < 50 m s2). Follow-up observations performed in May 2003 confirmed that the orbit was indeed very...

J P Ap E fo

Here, nbin is the number of pulsars in a period bin of width AP, pi is the 'scale factor' and fi is the beaming fraction of the ith pulsar. As discussed earlier, fi is based on some beaming model. For a given pulsar, its scale factor pi represents the number of pulsars with similar parameters in the Galaxy and is computed using a Monte Carlo simulation of N pulsars with identical periods and luminosities. Using accurate models for the various pulsar surveys, it is relatively straightforward to...

List of participants speakers and guests

Akg n, Taner (akgun astro.cornell.edu) Cornell University, USA Aksaker, Nazim (aknazim yahoo.com) Qukurova niversitesi, Turkey Aky z, Aysun (aakyuz cu.edu.tr) Qukurova niversitesi, Turkey Alpar, M. Ali (alpar sabanciuniv.edu) Sabanci University, Turkey Altamirano, Diego (diego science.uva.nl) University of Amsterdam, The Netherlands Ankay, Askin (askin gursey.gov.tr) T BITAK Feza G rsey Institute, Turkey Asian, Zeki (aslan tug.tug.tubitak.gov.tr) TUG, Turkey Balman, S len (solen...