The Formation of Close Binary Stellar Systems

Details The Formation of Close Binary Stellar Systems The Formation of Close Binary Stellar Systems

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.1004b&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #10.04; Bulletin of the American Astronomical Society, Vol. 32, p.1413

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Scientific paper

The formation of close binary systems is an unsolved problem. Whereas binaries with intermediate and wide separations can be explained by fragmentation during the isothermal collapse phase of a molecular cloud core, when the central part of the cloud becomes optically-thick and begins to heat up, fragmentation is inhibited. A second chance for fragmentation occurs inside the optically-thick region when molecular hydrogen dissociates, initiating the second collapse phase. We present results from three-dimensional hydrodynamic calculations which follow the collapse of a molecular cloud core ( ~ 10-18 g cm-3) to stellar densities (> 0.01 g cm-3). The calculations resolve structures over 7 orders of magnitude in spatial extent ( ~ 5000 AU - 0.1 Rsun), and over 17 orders of magnitude in density contrast. With these calculations, we consider whether fragmentation to form a close binary stellar system (separation <1 AU) can occur during the second collapse phase.

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