We present WSRT HI line observations, together with CCD-BVRI photometr
y, of NGC 7217, which is known to be an isolated galaxy with an inner
ring, an inner pseudoring and an outer ring, but for which no clear bi
-symmetric distortion is immeadiately apparent. Assuming, as is known
to be the case for barred galaxies, that the outer ring corresponds to
the outer Lindblad resonance, we have derived the expected locations
for the other resonances using a combined optical/H I rotation curve.
Our result is that the observed inner ring coincides with the inner Li
ndblad resonance and the inner pseudoring with the ultraharmonic (4:1)
resonance. The associated pattern speed is 86.0 km s(-1) kpc(-1) Howe
ver, it is less clear which feature is actually setting up this patter
n. The outer ring, which has a size of similar or equal to 6.3 x 5.9 k
pc, contains roughly two-thirds of the total H I mass, and has bluer c
olours and more intense Her emission than the main disk. A Fourier ana
lysis of the B - I colour along this ring suggests that it is composed
of 9 blobs, indicating the existence of a bead instability. This is i
n agreement with a simple calculation showing that the number of Jeans
lengths along the ring is also 9, and that self-gravity is probably i
mportant here. Clumps also exist in the inner pseudoring, but they are
less well defined, and there is no HI concentration along it. This ri
ng has redder colours than the outer ring. The blue inner ring is inco
mplete, coincides with a complete and intense Ha ring, and is surround
ed by a redder ring. A spiral-like structure extends from the inner ri
ng out to the inner pseudoring, with the same winding direction as the
outer flocculent arms. We have constructed a mass model, from which w
e obtain a mass-to-I-band luminosity ratio of 5.1 for the bulge, and 1
.8 for the disk. The core radius of the halo is 11.0 kpc, and its cent
ral density 0.062 Mo pc(-3). The ratio of halo core radius to optical
radius is thus of order unity.