  Observations of SN 1987A by the Chandra High Energy Transmission Grating
(HETG) in 1999 and the XMM-Newton Reflection Grating Spectrometer (RGS) in 2003
show very broad (v-b) lines with a full-width at half-maximum (FWHM) of order
10^4 kms; at these times the blast wave was primarily interacting with the HII
region around the progenitor. Since then, the X-ray emission has been
increasingly dominated by narrower components as the blast wave encounters
dense equatorial ring (ER) material. Even so, continuing v-b emission is seen
in the grating spectra suggesting that interaction with HII region material is
on-going. Based on the deep HETG 2007 and 2011 data sets, and confirmed by RGS
and other HETG observations, the v-b component has a width of 9300 +/-2000 kms
FWHM and contributes of order 20% of the current 0.5--2 keV flux. Guided by
this result, SN 1987A's X-ray spectra are modeled as the weighted sum of the
non-equilibrium-ionization (NEI) emission from two simple 1D hydrodynamic
simulations, this "2x1D" model reproduces the observed radii, light curves, and
spectra with a minimum of free parameters. The interaction with the HII region
(rho_init \sim 130 amu/cc, +/- 15 degrees opening angle) produces the
very-broad emission lines and most of the 3-10 keV flux. Our ER hydrodynamics,
admittedly a crude approximation to the multi-D reality, gives ER densities of
order 10^4 amu/cc, requires dense clumps (x5.5 density enhancement in \sim 30%
of the volume), and it predicts that the 0.5-2 keV flux will drop at a rate of
\sim 17% per year once no new dense ER material is being shocked.
