Density (top) and temperature (bottom) profiles of the column at successive times across the oscillation (shown in the inset) for an accretion rate of ṁ = 10 g/cm2/s, a white dwarf of 0.8 M⊙, and a pure bremsstrahlung cooling. Starting after t = 6.35 s, a secondary shock clearly forms at the basis of the accretion column and propagates upstream while the main shock falls towards the white dwarf surface.
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