Constraints on the viscosity parameter in the thick disk from X-ray and gamma-ray observations in SS 433

Details Constraints on the viscosity parameter in the thick disk from X-ray and gamma-ray observations in SS 433 Constraints on the viscosity parameter in the thick disk from X-ray and gamma-ray observations in SS 433

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324..391c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 1, 1988, p. 391-404.

Statistics

Computation

7

Accretion Disks, Doppler Effect, Gamma Rays, X Rays, Computational Astrophysics, Line Spectra

Scientific paper

We show that if the ratios [He]/[H] and [Fe]/[H] observed in the jet in SS 433 are very similar to the solar abundance, then the viscosity parameter α near the center of the disk must be larger than a few times 10-5, independent of any particular mechanism for SS 433. This assumes that the abundances of the elements in the jet reflect the average abundance of the accreting matter during the final moments of its journey toward the central hole. We follow matter as it is accreted and calculate the changes in composition on the way. Several models are studied with αranging from 10-4 to 10-6and the accretion rate from 10 to 100 (in units of the critical rate). It is observed that for α <10-5 the mass averaged ratios [He]/[H] and [Fe]/[H] go up dramatically from their normal values. This happens because for such parameter ranges the time scales involved in the HCNO cycle and the proton and neutron capture rates of iron become comparable to the residence time of matter in the disk. Since the requirement on viscosity is limited only to regions near the center of the disk, this does not violate any conditions on the residence time for the present models of SS 433. We also suggest that if the absence of the 1.2 and 1.5 MeV γ-ray lines is due to changes in the viscous mechanism in the disk, then α near the center lies much above 10-4.

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