We further tested the effect of the initial eccentricity of the orbit , varying it from e = 0 to e = 0.9 . Up to an eccentricity of ∼ 0.6 , the results did not appreciably change , but higher eccentricities suppress the ripples at larger distance from the star . This is because the stars spend most of the time near apocenter . In the high - resolution simulations some appreciable deviations from the spiral structure is noticeable when viewed directly from pericenter as respect to other viewing angles , but the effect is much smaller than the    Montes et al . ( 2000 ) to the radio data of Weiler et al . ( 1991 ) . As indicated in the topright corner of the figure , we vary the companion mass of 1 M , 6 M and 15 M and for circular orbits as well as for one with an eccentricity of e = 0.75 . All simulated binaries had an orbital period of 2000 yr , were perfomed at a resolution of 10 −5 M per SPH particle and adopted a viewing angel in the plane of motion and along the binary 's long axis ( from apocenter ) .