Excitation Conditions and Line Ratios from X-wind Jets

Details Excitation Conditions and Line Ratios from X-wind Jets Excitation Conditions and Line Ratios from X-wind Jets

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19713209s&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #132.09; Bulletin of the American Astronomical Society, Vol. 33, p.718

Astronomy and Astrophysics

Astronomy

Scientific paper

Thermal structures of the X-wind proves to be a necessary yet very important foundation for realistic modeling of the jet phenomena. X-rays and magnetic disturbances emanating from the central source, are identified as the self-sustaining energy generators in the x-wind star-disk interacting system. Following the demonstration of density structure and kinematic information in X-winds in Shang et al. (1998) with the assumption of uniform ionization conditions to calculate the emissions in the [S II]λ 6716/6731 and [O I]λ 6300/6364 lines, we investigate the self-consistent excitation conditions powered by the energy sources in the X-wind system. We perform streamline-by-streamline integrations of the rate and heat equations on the steady-state x-wind. Results show that X-rays are capable of providing typical ionization fractions inferred from the optical jets. We model the external heating mechanism as he averaging of mechanical energies deposited by shocks and/or MHD turbulence cascades. Shockwaves or turbulence cascades of magnetic origins are needed to provide the sufficiently high temperatures in enough emitting areas of the jets observed in the forbidden lines at thousands of AU from the stars to maintain the excitation. A good demonstration of such diagnostics would be line ratios from the optical forbidden lines. We will report in this presentation that the electron densities and temperatures achieved in the overall self-consistent model yield line ratios similar to those observed in a large set of YSO jet sources.

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