  In this paper, we present the analysis of the stellar system HIP 101227 to
determine the actual number of components in the system, and their properties.
We use dynamical modeling and complex spectrophotometric (involving atmospheric
modeling) techniques with recent data, to determine the physical properties and
orbital solution for the system, respectively, with better accuracy than past
studies. Based on our analysis, we found that the system is more consistent
with being a quadruple rather than a binary, or a triple system as that
suggested by previous studies. The total mass of the system determined from our
SED analysis is 3.42 $\pm$ 0.20 $M_{\odot}$, which are distributed almost
equally between the four stars. The stars are found to be zero-age main
sequence stars; i.e., at the last stage of pre-main sequence,with age less than
200 Myr and spectral types K0. All four stars have very similar physical
characteristics, suggesting that fragmentation process is the most likely
theory for the formation and evolution of the system.
