skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Interstellar scintillation of the double pulsar J0737–3039

Journal Article · · Astrophysical Journal
; ;  [1];  [2];  [3];  [4]; ; ;  [5];  [6]
  1. ECE Dept., University of California San Diego, La Jolla, CA 92093-0407 (United States)
  2. West Virginia University, Morgantown, WV 26505 (United States)
  3. National Radio Astronomy Observatory, Charlottesville, VA 22903 (United States)
  4. National Astronomy and Ionosphere Center, Arecibo, PR 00612-8346 (United States)
  5. Jodrell Bank Center for Astrophysics, University of Manchester, M13 9PL (United Kingdom)
  6. Dept. of Physics, McGill University, Montréal, QC H3A 2T8 (Canada)

We report a series of observations of the interstellar scintillation (ISS) of the double pulsar J0737–3039 over the course of 18 months. As in earlier work, the basic phenomenon is the variation in the ISS caused by the changing transverse velocities of each pulsar, the ionized interstellar medium (IISM), and the Earth. The transverse velocity of the binary system can be determined both by very long baseline interferometry and timing observations. The orbital velocity and inclination is almost completely determined from timing observations, but the direction of the orbital angular momentum is not known. Since the Earth's velocity is known, and can be compared with the orbital velocity by its effect on the timescale of the ISS, we can determine the orientation Ω of the pulsar orbit with respect to equatorial coordinates (Ω = 65 ± 2°). We also resolve the ambiguity (i = 88.°7 or 91.°3) in the inclination of the orbit deduced from the measured Shapiro delay by our estimate i = 88.°1 ± 0.°5. This relies on the analysis of the ISS over both frequency and time, and provides a model for the location, anisotropy, turbulence level, and transverse phase gradient of the IISM. We find that the IISM can be well-modeled during each observation, typically of a few orbital periods, but its turbulence level and mean velocity vary significantly over the 18 months.

OSTI ID:
22356729
Journal Information:
Astrophysical Journal, Vol. 787, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
Country of Publication:
United States
Language:
English

Similar Records

Formation and progenitor of PSR J0737-3039: New constraints on the supernova explosion forming pulsar B
Journal Article · Tue Aug 15 00:00:00 EDT 2006 · Physical Review. D, Particles Fields · OSTI ID:22356729

Effects of gravitational lensing and companion motion on the binary pulsar timing
Journal Article · Wed Mar 15 00:00:00 EST 2006 · Physical Review. D, Particles Fields · OSTI ID:22356729

Similarity of PSR J1906+0746 to PSR J0737–3039: a Candidate of a New Double Pulsar System?
Journal Article · Wed Feb 01 00:00:00 EST 2017 · Astrophysical Journal · OSTI ID:22356729