A Tale of Two Long Tails: the Bow Shock Nebulae Associated with Pulsars J1747-2958 and J1509-5850

Details A Tale of Two Long Tails: the Bow Shock Nebulae Associated with Pulsars J1747-2958 and J1509-5850 A Tale of Two Long Tails: the Bow Shock Nebulae Associated with Pulsars J1747-2958 and J1509-5850

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21343605n&link_type=abstract

American Astronomical Society, AAS Meeting #213, #436.05; Bulletin of the American Astronomical Society, Vol. 41, p.307

Astronomy and Astrophysics

Astronomy

Scientific paper

Pulsars typically move supersonically through the interstellar medium. The ram pressure confinement of the resultant pulsar wind nebula (PWN) produces a bow shock with a tail behind the pulsar. Using new radio and X-ray observations, we present a detailed study of two such systems with the longest tails: the PWNe surrounding pulsars J1747-2958 and J1509-5850.
New Chandra HRC observation of the PWN associated with PSR J1747-2958, known as the Mouse, hints at the existence of small scale features near the backward termination shock region. Timing analysis shows no X-ray pulsation from the central pulsar. For PSR J1509-5850, polarimetric imaging at 3 and 6cm reveals a helical magnetic field along the 10pc long tail, providing an evidence of a pulsar magnetotail. The average equipartition field strength in the radio tail is 20\mu G, a few times lower than that of the X-ray emitting region. The different magnetic field structure in these two bow shock systems could be the result of different flow speeds, or differing degrees of alignment between the pulsar spin axes and the corresponding proper motion vectors.

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