  We present new Keck II NIRSPEC high-spectral resolution 2 um echelle
observations of the young eruptive variable star V1647 Orionis. This star went
into outburst in late 2003 and faded to its pre-outburst brightness after
approximately 26 months. V1647 Orionis is the illuminating star of McNeil's
Nebula and is located near M 78 in the Lynds 1630 dark cloud. Our spectra have
a resolving power of approximately 18,000 and allow us to study in detail the
weak absorption features present on the strong near-IR veiled continuum. An
analysis of the echelle orders containing Mg I (2.1066 um) and Al I (2.1099
um), Br-gamma (2.1661 um), the Na I doublet (2.206 and 2.209 um), and the CO
overtone bandhead (2.2935 um) gives us considerable information on the physical
and geometric characteristics of the regions producing these spectral features.
We find that, at high-spectral resolution, V1647 Orionis in quiescence
resembles a significant number of FU Orionis type eruptive variables and does
not appear similar to the quiescent EX Lupi variables observed. This
correspondence is discussed and implications for the evolutionary state of the
star are considered.
