2012ApJ...750...70T -
Astrophys. J., 750, 70 (2012/May-1)
Modeling high-energy light curves of the PSR B1259-63/LS 2883 binary based on 3D SPH simulations.
TAKATA J., OKAZAKI A.T., NAGATAKI S., NAITO T., KAWACHI A., LEE S.-H., MORI M., HAYASAKI K., YAMAGUCHI M.S. and OWOCKI S.P.
Abstract (from CDS):
Temporal changes of X-ray to very high energy gamma-ray emissions from the pulsar-Be-star binary PSR B1259-63/LS 2883 are studied based on three-dimensional smoothed particle hydrodynamic simulations of pulsar wind interaction with Be-disk and wind. We focus on the periastron passage of the binary and calculate the variation of the synchrotron and inverse-Compton emissions using the simulated shock geometry and pressure distribution of the pulsar wind. The characteristic double-peaked X-ray light curve from observations is reproduced by our simulation under a dense Be-disk condition (base density ∼10–9 g/cm3). We interpret the pre- and post-periastron peaks as being due to a significant increase in the conversion efficiency from pulsar spin-down power to the shock-accelerated particle energy at orbital phases when the pulsar crosses the disk before periastron passage, and when the pulsar wind creates a cavity in the disk gas after periastron passage, respectively. On the contrary, in the model TeV light curve, which also shows a double-peak feature, the first peak appears around the periastron phase. The possible effects of cooling processes on the TeV light curve are briefly discussed.
Abstract Copyright:
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Journal keyword(s):
hydrodynamics - pulsars: individual: PSR B1259-63 - radiation mechanisms: non-thermal - stars: individual: LS 2883
Simbad objects:
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