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Close encounters of the third-body kind

1994; IOP Publishing; Volume: 424; Linguagem: Inglês

10.1086/173937

1538-4357

M. B. Davies, W. Benz, J. G. Hills,

Gamma-ray bursts and supernovae

view Abstract Citations (50) References (17) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Close Encounters of the Third-Body Kind Davies, M. B. ; Benz, W. ; Hills, J. G. Abstract We simulated encounters involving binaries of two eccentricities: e = 0 (i.e., circular binaries) and e = 0.5. In both cases the binary contained a point mass of 1.4 solar masses (i.e., a neutron star) and a 0.8 solar masses main-sequence star modeled as a polytrope. The semimajor axes of both binaries were set to 60 solar radii (0.28 AU). We considered intruders of three masses: 1.4 solar masses (a neutron star), 0.8 solar masses (a main-sequence star or a higher mass white dwarf), and 0.64 solar masses (a more typical mass white dwarf). Our strategy was to perform a large number (40,000) of encounters using a three-body code, then to rerun a small number of cases with a three-dimensional smoothed particle hydrodynamics (SPH) code to determine the importance of hydrodynamical effects. Using the results of the three-body runs, we computed the exchange across sections, sigmaex. From the results of the SPH runs, we computed the cross sections for clean exchange, denoted by sigmacx; the formation of a triple system, denoted by sigmatrp; and the formation of a merged binary with an object formed from the merger of two of the stars left in orbit around the third star, denoted by sigmamb. For encounters between either binary and a 1.4 solar masses neutron star, sigmacx approx. 0.7 sigmaex and sigmamb + sigmatrp approx. 0.3 sigmaex. For encounters between either binary and the 0.8 solar masses main-sequence star, sigmacx approx. 0.50 sigmaex and sigmamb + sigmatrp approx. 1.0 sigmaex. If the main sequence star is replaced by a main-sequence star of the same mass, we have sigmacx approx. 0.5 sigmaex and sigmamb + sigmatrp approx. 1.6 sigmaex. Although the exchange cross section is a sensitive function of intruder mass, we see that the cross section to produce merged binaries is roughly independent of intruder mass. The merged binaries produced have semi-major axes much larger than either those of the original binaries or those of binaries produced in clean exchanges. Coupled with their lower kick velocities, received from the encounters, their larger size will enhance their cross section, shortening the waiting time to a subsequent encounter with another single star. Publication: The Astrophysical Journal Pub Date: April 1994 DOI: 10.1086/173937 Bibcode: 1994ApJ...424..870D Keywords: Binary Stars; Celestial Mechanics; Encounters; Hydrodynamics; Stellar Mass; Three Body Problem; Computerized Simulation; Eccentricity; Main Sequence Stars; Neutron Stars; Numerical Analysis; Stellar Orbits; White Dwarf Stars; Astrophysics; STARS: BINARIES: CLOSE; CELESTIAL MECHANICS; STELLAR DYNAMICS; HYDRODYNAMICS; METHODS: NUMERICAL full text sources ADS |