  Nussbaumer et al. (1989) proposed that broad H$\alpha$ wings can be formed
through Raman scattering of Ly$\beta$ photons, and in this Letter we argue that
the H$\alpha$ wings prevalently seen in symbiotic stars may be indeed formed in
this way. Assuming a flat incident UV radiation around Ly$\beta$, we generate
template wing profiles around H$\alpha$ that are formed through Raman
scattering in a plane-parallel H~I region. We perform profile fitting analyses
to show that the template wing profiles are in excellent agreement with the
observed ones that are provided by van Winckel et al. (1993) and Ivison et al.
(1994). The wing flux is determined by the scattering H~I column density and
the incident Ly$\beta$ flux strength and profile. From our profile analysis it
is proposed that the Raman scattering component may be identified with the
neutral envelope with a column density ranging $10^{18-20} {\rm cm^{-2}}$ that
surrounds the binary system. We briefly discuss alternative candidates for the
wing formation mechanism and observational implications of Raman scattering in
symbiotic stars and in other astronomical objects including planetary nebulae,
post AGB stars and active galactic nuclei.
