Chandra observation of the interaction between the plasma nebula RCW89 and the pulsar jet of PSR B1509–58 |
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| Institution: | 1. Department of Physics, Tokyo Institute of Technology, 2-12-1 Ohokayama Meguro, Tokyo 152-8551, Japan;2. Nagoya University, Furo-cho, Chikusa, Nagoya 464-8602, Japan;3. Max-Planck-Institut für Extraterrestrische Physik, Postfach 1603, 85740 Garching, Germany;1. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS-70, Cambridge, MA 02138, USA;2. Jansky Fellow, National Radio Astronomy Observatory, and Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS-70, Cambridge, MA 02138, USA |
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| Abstract: | We present a Chandra observation of the H II region RCW89. The nebula lies 10′ north from the central pulsar PSR B1509–58, and it has been suggested that the nebula is irradiated by the pulsar jet. We performed a spectral analysis of the seven brightest emitting regions aligned in a horse-shoe like shape, and found that the temperature of the knots increases along the horse-shoe in the clockwise direction, while, in contrast, the ionization parameter net decreases. This result implies that RCW89 was heated in sequence. We examined the energy budget assuming that RCW89 is powered by the pulsar jet. The rate of energy injection into RCW89 by the jet was estimated from the synchrotron radiation flux. We obtained a heating time-scale of 1400 yr, which is consistent with the pulsar characteristic age of 1700 yr. To explain the temperature gradient, we discuss the cooling process for plasma clouds in RCW89. We argue that the plasma clumps can be cooled down by the adiabatic expansion within 250 yr, and form the temperature gradient reflecting the sequential heating by the precessing pulsar jet. |
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