The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission has been orbiting Mars since 2014 and now has tens of thousands of 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 angle in the X, Y MSO plane. 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 propagates 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.

翻译：火星大气与挥发物演化（MAVEN）探测器自2014年起环绕火星运行，现已积累数万条轨道数据，可用于表征火星动态空间环境。通过基于MAVEN磁场数据的全球场线追踪，我们发现火星上方垂直方向（$\hat Z$火星太阳状态坐标系，MSO）的弯曲形态呈现高度依赖性，且与感应磁层经典预期存在差异。我们利用贝叶斯多元线性回归模型，从经典感应磁层图像中量化了这一差异，该模型将弯曲场描述为上流行星际磁场（IMF）、残余地壳磁场以及此前被低估的感应效应的函数。根据模型结论，日侧高层弯曲（>800 km）中非预期扭转是由IMF在X-Y MSO平面中的角度所致。我们认为这属于感应磁层现有理论的自然结果，但因过去常将IMF近似为纯$\pm \hat Y$方向而被低估。此外，我们估算出沿$\hat Z$方向的日侧低层弯曲（<800 km）畸变与残余地壳磁场直接相关。研究表明，日侧弯曲会向尾向传播，此前报道的内磁尾扭转很可能由火星地壳磁场引起，而外磁尾形态则受IMF方向主导的感应响应调控。最终我们提出感应磁层的更新认知：详细描述了多方向入射IMF下的日侧弯曲特征，并探讨了该弯曲对磁尾形态的影响。