2001/04/19 by E. B. Fomalont, B. J. Geldzahler, C. F. Bradshaw · 5 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Pulsars and Gravitational Waves Research #Radio Astronomy Observations and Technology #astro-ph
paper · pdf · doi:10.1086/320490
9 pages total, four figures. ApJ Letters, in press
arxiv created 2001/04/19 · openalex publication_date 2001/05/20 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
The evolution of the radio emission from Scorpius X-1 is determined from a 56 hr continuous VLBI observation and from shorter observations over a 4 yr period. The radio source consists of a variable core near the binary and two variable compact radio lobes, which form near the core, move diametrically outward, and then fade away. Subsequently, a new lobe pair form near the core and the behavior repeats. The differences in the radio properties of the two lobes are consistent with the delay and Doppler boosting associated with an average space velocity of 0.45 c at 44° to the line of sight. Four lobe speeds, between 0.32 c and 0.57 c , were measured for several lobe pairs on different days. The speed during each epoch remained constant over many hours. The direction of motion of the lobes over all epochs remained constant to a few degrees. Two core flares are contemporaneous with two lobe flares after removal of the delay associated with an energy burst moving with speed β j > 0.95 in a twin beam from the core to each lobe. This is the first direct measurement of the speed of energy flow within an astrophysical jet. The similarity of the core and lobe flares suggests that the twin-beam flow is symmetric and that the core is located near the base of the beam.