“…Before going to the discussion, it should be mentioned here that our model is focused on quantum dusty plasmas of ultradense astrophysical objects (Ali and Shukla 2006;El-Taibany and Wadati 2007;El-Labany et al 2009b), in which the mass density is of order 10 6 g/cm 3 or more, like the case of white dwarfs or neutron stars, giving rise to k m ≈ 4 × 10 6 or more. Therefore, within the following numerical investigations, we will use (Ali and Shukla 2006;El-Taibany and Wadati 2007;El-Labany et al 2009b) r min = 10 −4 cm, k = 10 −6 , k z = 10 7 , k m = 4 × 10 6 , σ e ≈ 2, σ i ≈ 0.01, Fig. 1 Variation of phase shift with R for different values of the power law index β and r m = 10 −4 , k = 10 −6 , k z = 10 7 , k m = 4 × 10 6 n e0 = 5 × 10 23 cm −3 , n i0 = 2 × 10 24 cm −3 , H e ≈ 10 −1 , H i ≈ 10 −3 , and H d ≈ 10 −8 .…”