通过MOLA廓线的共同登记对火星极地季节性CO2雪/冰帽的时间高度变化绘图的前景
Prospects for Mapping Temporal Height Variations of the Seasonal CO2 Snow/Ice Caps at the Martian Poles by Co-registration of MOLA Profiles
摘要：
我们研究的可行性和证明的优点，使用火星轨道器激光高度计（MOLA）的配置文件，以检索季节性的高度变化的CO2雪/冰帽在火星的极地地区，通过应用一个共同注册策略。本文对位于残留南极帽上的研究区[85.75°S，86.25°S，300°E，330°E]进行了原型分析。我们的方法包括重新计算MOLA足迹坐标与更新的火星全球勘测者（MGS）星历和修订后的火星旋转模型。再处理后的火星南极MOLA数据集（南纬78°），然后自我注册，形成一个连贯的参考数字地形模型（DTM）。我们共同注册的重新处理的MOLA配置文件的片段的自我注册的MOLA参考DTM，以获得时间的高度差异，无论是足迹或交叉。随后，两步区域伪交叉调整（RPCA）的过程中提出并应用于后校正上述时间的系统偏差和其他残留误差的时间高度差。这些伪交叉由纵断面对形成，纵断面对不一定相交，但通过下层DTM连接。最后，CO2雪/冰的时间高度变化是通过中值滤波这些后校正的时间高度差。推导的高度变化时间序列的精度为~4.9 cm。峰间高度变化估计约为2 m。此外，在南方春季还观测到一个以Ls=210°为中心的约0.5m量级的“坑”（瞬时高度积累）。所提出的方法开辟了在整个火星北极和南极地区绘制季节性二氧化碳雪/冰高度变化的可能性。
英文摘要：
We investigate the feasibility and demonstrate the merits of using Mars Orbiter Laser Altimeter (MOLA) profiles to retrieve seasonal height variations of CO2 snow/ice cap in Mars' polar areas by applying a co-registration strategy. We present a prototype analysis on the research region of [85.75°S, 86.25°S, 300°E, 330°E] that is located on the residual south polar cap. Our method comprises the recomputation of MOLA footprint coordinates with an updated Mars Global Surveyor (MGS) ephemeris and a revised Mars rotation model. The reprocessed MOLA dataset at the South Pole of Mars (poleward of 78°S) is then self-registered to form a coherent reference digital terrain model (DTM). We co-register segments of reprocessed MOLA profiles to the self-registered MOLA reference DTM to obtain the temporal height differences at either footprints or cross-overs. Subsequently, a two-step Regional Pseudo Cross-over Adjustment (RPCA) procedure is proposed and applied to post-correct the aforementioned temporal height differences for a temporal systematic bias and other residual errors. These pseudo cross-overs are formed by profile pairs that do not necessarily intersect, but are connected through the underlaying DTM. Finally, CO2 snow/ice temporal height variation is obtained by median-filtering those post-corrected temporal height differences. The precision of the derived height change time series is ~4.9 cm. The peak-to-peak height variation is estimated to be ~2 m. In addition, a pronounced "pit" (transient height accumulation) of ~0.5 m in magnitude centered at Ls=210° in southern spring is observed. The proposed method opens the possibility to map the seasonal CO2 snow/ice height variations at the entire North and South polar regions of Mars.
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