  The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission has been orbiting
Mars since 2014 and now has over 10,000 orbits which we use to characterize
Mars' dynamic space environment. Through global field line tracing with MAVEN
magnetic field data we find an altitude dependent draping morphology that
differs from expectations of induced magnetospheres in the vertical ($\hat Z$
Mars Sun-state, MSO) direction. We quantify this difference from the classical
picture of induced magnetospheres with a Bayesian multiple linear regression
model to predict the draped field as a function of the upstream interplanetary
magnetic field (IMF), remanent crustal fields, and a previously underestimated
induced effect. From our model we conclude that unexpected twists in high
altitude dayside draping ($>$800 km) are a result of the IMF component in the
$\pm \hat X$ MSO direction. We propose that this is a natural outcome of
current theories of induced magnetospheres but has been underestimated due to
approximations of the IMF as solely $\pm \hat Y$ directed. We additionally
estimate that distortions in low altitude ($<$800 km) dayside draping along
$\hat Z$ are directly related to remanent crustal fields. We show dayside
draping traces down tail and previously reported inner magnetotail twists are
likely caused by the crustal field of Mars, while the outer tail morphology is
governed by an induced response to the IMF direction. We conclude with an
updated understanding of induced magnetospheres which details dayside draping
for multiple directions of the incoming IMF and discuss the repercussions of
this draping for magnetotail morphology.
