  V934 Her = 4U1700+24 is an M giant-neutron star (NS) X-ray symbiotic (SyXB)
system. Employing optical and infrared radial velocities spanning 29 years
combined with the extensive velocities in the literature, we compute the
spectroscopic orbit of the M giant in that system. We determine an orbital
period of 4391 days or 12.0 yr, the longest for any SyXB, and far longer than
the 404 day orbit commonly cited for this system in the literature. In addition
to the 12.0 yr orbital period we find a shorter period of 420 days, similar to
the one previously found. Instead of orbital motion, we attribute this much
shorter period to long secondary pulsation of the M3 III SRb variable. Our new
orbit supports earlier work that concluded that the orbit is seen nearly pole
on, which is why X-ray pulsations associated with the NS have not been
detected. We estimate an orbital inclination of 11.3$^\circ$ $\pm$ 0.4$^\circ$.
Arguments are made that this low inclination supports a pulsation origin for
the 420 day long secondary period. We also measure CNO and Fe peak abundances
of the M giant and find it to be slightly metal poor compared to the Sun with
no trace of the NS forming SN event. Basic properties of the M giant and NS are
derived. We discuss the possible evolutionary paths that this system has taken
to get to its current state.
