Double-core evolution. 5: Three-dimensional effects in the merger of a red giant with a dwarf companion

Details Double-core evolution. 5: Three-dimensional effects in the merger of a red giant with a dwarf companion Double-core evolution. 5: Three-dimensional effects in the merger of a red giant with a dwarf companion

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422..729t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 2, p. 729-736

Astronomy and Astrophysics

Astrophysics

36

Astronomical Models, Binary Stars, Computerized Simulation, Hydrodynamics, Late Stars, Mathematical Models, Red Giant Stars, Stellar Evolution, Stellar Mass Ejection, White Dwarf Stars, Angular Momentum, Center Of Mass, Circular Orbits, Eccentric Orbits, Gravitational Fields, Orbital Mechanics

Scientific paper

The evolution of the common envelope phase of a binary system consisting of a 4.67 solar mass red giant and a 0.94 solar mass dwarf is studied using smoothed particle hydrodynamics. We demonstrate that the three-dimensional effects associated with the gravitational tidal torques lead to a rapid decay of the orbit on timescales approximately less than 1 yr. The relative orbit of the two cores in the common envelope is initally eccentric and tends to circularize as the orbital separation of the two cores decreases. The angular momentum lost from the orbital motion is distributed throughout the common envelope, and the double core does not evolve to a state of co-rotation for the evolutionary time followed. The energy dissipated from the relative orbit and deposited in the common envelope results in the ejection of approximately 13% of the mass of the envelope. The mass is ejected in all directions, but there is a preference for mass ejection in the orbital plane of the binary system. For example, approximately 80% of the ejected mass lies within 30 deg of the binary orbital plane. Because gravitational forces are long range, most of the energy and angular momentum is imparted to a small fraction of the common envelope resulting in an efficiency of the mass ejection process of approximately 15%. The core of the red giant executes significant displacement with respect to the center of mass of the system and contributes nearly equally to the total energy dissipation rate during the latter phases of the evolution. The degree of departure from synchronism of the initial binary system can be an important property of the system which can affect the outcome of the common envelope phase.

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