Statistics – Computation
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.3610s&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #36.10; Bulletin of the American Astronomical Society, Vol. 24, p.1176
Statistics
Computation
3
Scientific paper
The Eggleton, Faulkner, and Flannery (EFF) equation of state (EOS) is widely used in stellar evolution codes throughout the world. This popularity is due primarily to its being analytical and thereby possessing a number of advantages over tabulated EOSs. Foremost is its flexibility -- varying compositions are routinely dealt with and new physics can be easily introduced and investigated. A number of shortcomings in the original EFF EOS have been known for some time; however, their significance may not have been thoroughly explored. Some physical improvements have recently been implemented by other researchers (Christensen-Dalsgaard 1990, Proffitt & Michaud 1991). We compare the Eggleton, Faulkner, and Flannery equation of state with the much more sophisticated and computationally expensive OPAL EOS developed at Livermore. We compute relevant thermodynamic quantities for a variety of representative stellar conditions with both EOSs. We show that results from the two EOSs differ significantly even under commonly encountered conditions. We identify the physical causes of the differences and address a number of them by modifying the original EFF equation of state while maintaining the analytical spirit of the EFF EOS. We compare results obtained using this modified EFF EOS with those from the OPAL EOS.
Rogers Forrest J.
Swenson Fritz J.
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