2002/04/16 by Slavko Bogdanov, Malgorzata Pruszynska, Małgorzata Pruszyńska +3 · 2 citations
Physics and Astronomy · #Astronomy #Astrophysics #Binary pulsar #Cosmology and Gravitation Theories #Detector #Interstellar medium #Longitude #Millisecond pulsar #Optics #Physics #Proper motion #Pulsar #Pulsars and Gravitational Waves Research #Radial velocity #Radio telescope #Scattering #Scintillation #Solar and Space Plasma Dynamics #Stars #astro-ph
paper · pdf · doi:10.1086/344169
16 pages, 3 PostScript figures, submitted to the Astrophysical Journal
arxiv created 2002/04/16 · openalex publication_date 2002/12/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present interstellar scintillation (ISS) velocity measurements for four millisecond pulsars, obtained from long-term monitoring observations with the Arecibo radio telescope at 430 MHz. We also derive explicit expressions, valid for a thin scattering screen, that relate the measured scintillation velocity to the effective transverse velocity responsible for the motion of the diffraction pattern for both binary and solitary pulsars. For PSR B1257+12, PSR B1534+12, PSR J1640+2224, and PSR J1713+0747 we derive ISS velocity estimates of 197 ± 57, 192 ± 63, 38 ± 8, and 82 ± 16 km s -1 , respectively. These values are in good agreement with proper-motion measurements for the four pulsars. For the relativistic binary pulsar PSR B1534+12, we use the ISS velocity dependence on orbital phase to determine the longitude of the ascending node Ω of the pulsar's orbit and to derive an estimate of the effective scattering screen location. The two possible values of Ω are 70° ± 20° and 290° ± 20°, and the approximate screen location is 630 ± 200 pc, with the assumed pulsar distance of 1.1 kpc.