Ion velocity distributions in the form of bunches of gyrating particles traveling along helical paths have been observed moving sunward immediately upstream from quasi-parallel parts of the earth's bow shock specular reflection at the shock of a portion of the incident solar wind ions. In particular, the guiding center motion and the gyrospeeds of the gyrating ions are quantitatively consistent with simple geometrical consideration for specular reflection. These considerations reveal that specularly reflected ions can escape upstream for &THgr;Bn⟨45¿ but not for &THgr;Bn⟩45¿ (where &THgr;Bn is the angle between the upstream magnetic field, B and the local shock normal nˆ). These upstream gyrating ions are an important signature of one of the processes by which solar wind streaming energy is dissipated into other forms of energy at the shock.