  Precision radial velocity (RV) measurements of the Sun-like dwarf
  14 Herculis published by Naef et. al (2004), Butler et. al (2006) and
  Wittenmyer et al (2007) reveal a Jovian planet in a 1760 day orbit and a
trend indicating the second distant object. On the grounds of dynamical
considerations, we test a hypothesis that the trend can be explained by the
presence of an additional giant planet. We derive dynamical limits to th
orbital parameters of the putative outer Jovian companion in an orbit within
~13 AU. In this case, the mutual interactions between the Jovian planets are
important for the long-term stability of the system. The best self-consistent
and stable Newtonian fit to an edge-on configuration of Jovian planets has the
outer planet in 9 AU orbit with a moderate eccentricity ~0.2 and confined to a
zone spanned by the low-order mean motion resonances 5:1 and 6:1. This solution
lies in a shallow minimum of \Chi and persists over a wide range of the system
inclination. Other stable configurations within 1\sigma confidence interval of
the best fit are possible for the semi-major axis of the outer planet in the
range of (6,13) AU and the eccentricity in the range of (0,0.3). The orbital
inclination cannot yet be determined but when it decreases, both planetary
masses approach ~10 Jupiter masses and for ~30 deg the hierarchy of the masses
is reversed.
