  HD 95086 is a young early-type star that hosts (1) a 5 MJ planet at the
projected distance of 56 AU revealed by direct imaging, and (2) a prominent
debris disk. Here we report the detection of 69 um crystalline olivine feature
from the disk using the Spitzer/MIPS-SED data covering 55-95 um. Due to the low
resolution of MIPS-SED mode, this feature is not spectrally resolved, but is
consistent with the emission from crystalline forsterite contributing 5% of the
total dust mass. We also present detailed analysis of the disk SED and
re-analysis of resolved images obtained by Herschel. Our results suggest that
the debris structure around HD 95086 consists of a warm (175 K) belt, a cold
(55 K) disk, and an extended disk halo (up to 800 AU), and is very similar to
that of HR 8799. We compare the properties of the three debris components, and
suggest that HD 95086 is a young analog of HR 8799. We further investigate and
constrain single-planet, two-planet, three-planet and four-planet architectures
that can account for the observed debris structure and are compatible with
dynamical stability constraints. We find that equal-mass four-planet
configurations of geometrically spaced orbits, with each planet of mass 5 MJ,
could maintain the gap between the warm and cold debris belts, and also be just
marginally stable for timescales comparable to the age of the system.
