Gamma-Ray Bursts (GRBs) are a high energy astrophysical transient phenomena that signal the
death of massive stars and the merging of compact objects. They provide us with the unique
opportunity to study fundamental physics at energy scales that cannot be created on Earth. The
afterglow of a GRB can be observed over a period of days up to many months within the X-ray
band. The flux time series, or light curve (LC), of the afterglow typically consists of a smooth
underlying continuum with sharply peaked pulses known as X-ray flares. While the underlying
continuum is well-described by a broken power-law, flaring components are often removed due
to their origins and mechanisms being less constrained. This results in missing power-law
breaks and reduced precision in characterizing the LC. To address this issue, we present a
complete parameterized forward model for GRB LCs. This modeling allows us to infer useful
characteristics of flares including start/end/peak times, flare widths, flare asymmetries, the
number of flares present within the LC and more. We also leverage the work started by Ioka et
al. (2005) and have used the flaring components to distinguish possible flaring mechanisms (e.g.
circumburst density fluctuations, patchy shell, etc.). Such an analysis has the potential to uncover
new features in the GRB population and discover correlations between GRB properties that
could help shed light on GRB progenitors and their environments.