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We performed time resolved spectroscopy of the old-nova intermediate-polar DQ Her during an eclipse of its WD primary. The eclipse of the Hαand HeIλ6678 emission lines is reminiscent of that of an accretion disk. However, Hαshows a triple-peaked profile and is only partially eclipsed. The three stationary peaks shown by Hαcould be produced by the accretion stream overflowing the disk, some material near the barycenter of the binary system, the surface of the secondary facing the WD, a wind and/or a jet from the disk. Some contamination by the nova ejecta is also possible. The presence of stationary components in the emission line profiles is reminiscent of other CVs like the dwarf nova IP Peg. The broad component of the Hαemission seems to be produced by the accretion disk as this component is the only one to show radial velocity variations modulated by the orbital motion of the WD. The O–C value derived from the eclipse of the continuum confirms the cyclical behavior of the O–C vs. JD diagram and suggests a main secular periodicity slightly longer than ~22 yr, possibly due to magnetic activity cycles of the secondary.