Modeling the Crab Synchrotron Nebula by Including Radiative Losses in Flow Dynamics

Details Modeling the Crab Synchrotron Nebula by Including Radiative Losses in Flow Dynamics Modeling the Crab Synchrotron Nebula by Including Radiative Losses in Flow Dynamics

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20915612f&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #156.12; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

Scientific paper

Models of the Crab synchrotron nebula include energy losses by radiative and adiabatic expansion, but neglect the effect of radiative losses on the flow itself. The standard model of Kennel and Coroniti (1984), for example, calculates a post-shocked flow and modifies only the energy equation while assuming steady state flow dynamics. Recent efforts at simulating the synchrotron emission from the Crab also take this approach (Shibata et al. 2003 MNRAS, 346, 841, and Del Zanna et al. 2006, A&A, 453, 621). Typically, these authors argue that since the radiated power is only about 10 percent of the pulsar's spin down luminosity, radiative losses should have only negligible effects on flow dynamics. This argument implicitly assumes a spherically symmetric nebula: the estimate can be as high as 20 30 percent for a wedge geometry, for example.
In previous work we have revisited the problem of a steady state adiabatic flow, replacing the semi-analytic treatment of KC with a numerical calculation (Foy & Hester 2005). We present a preliminary time-dependent model that incorporates synchrotron radiative losses into the dynamics of the flow and discuss how such a treatment may reveal dynamical instabilities associated with the observed 'wisps' in the Crab nebula.
J.P.F. acknowledges support from the Arizona State University NASA Space Grant Program.

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