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Characterizing dark mantle deposits in the lunar crater Alphonsus

机译：表征月球陨石坑Alphonsus中的暗幔沉积

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摘要

We analyze available remote-sensing data of the crater Alphonsus, focusing on the analysis of the crater's dark mantle deposits (DMDs), which includes images from NASA Clementine and Lunar Reconnaissance Orbiter (LRO), Japanese Selene (Kaguya), and Indian Chandrayaan-1 missions. The Alphonsus DMD5 are gentle-sloped flat hills with typical heights of several meters, which are presented with pyroclastic materials. Our determination of the absolute ages of the Alphonsus DMDs by the technique of crater size-frequency distributions shows that they are similar to 200-400 my. old. However, being geologically young, the Alphonsus DMDs are not seen in OMAT maps. The DMDs have noticeably lower content of TiO2 (2-3%) than the mare regions to the west (4%). The assessment of total pyroxene shows it has a higher abundance in the DMDs, although LRO Diviner measurements of the Chirstiansen feature suggest, rather, a high abundance of olivine. The DMDs pyroclastic material has no signs of OH/H2O compounds. We may suggest that this characteristic of the DMD5 either relates to their impact reworking and loss of the OH/H2O compounds or to the non-water volatiles as the driving agent of the pyroclastic activity. The compositional assessments of the DMDs may be flawed from contamination with the surrounding material due to horizontal and vertical transportation due to impacts. This effect probably can be observed in LROC NAC images of high resolution. A very dark material outcropping on the slopes of the vent depression is seen due to renovation of the regolith on the steep walls of the depression. Thus, at smaller phase angles, the pyroclastic material is dark and at larger phase angles it appears almost like the surrounding material. This means that the phase dependence of the outcropping dark material is shallow; i.e. the dark surface is smoother than its surroundings. This may suggest venting of gases resulting in fluidization of the granular pyroclastic material of the deposit.
机译：我们分析了陨石坑Alphonsus的可用遥感数据，重点分析了陨石坑的暗幔沉积物（DMD），其中包括来自NASA克莱门汀和月球侦察轨道卫星（LRO），日本Selene（Kaguya）和印度Chandrayaan- 1个任务。 Alphonsus DMD5是平缓倾斜的平坦山丘，典型高度为几米，并以火山碎屑材料出现。我们通过陨石坑大小-频率分布技术确定了Alphonsus DMD的绝对年龄，结果表明它们类似于200-400 my。旧。但是，由于地理年轻，Alphonsus DMD在OMAT地图中看不到。 DMD的TiO2含量（2-3％）明显低于西部的母马地区（> 4％）。对总辉石的评估表明它在DMD中具有较高的丰度，尽管对Chirstiansen特征的LRO Diviner测量表明，橄榄石的丰度较高。 DMDs火山碎屑材料没有OH / H2O化合物的迹象。我们可能会建议DMD5的这一特性与其影响重做和OH / H2O化合物的损失有关，或者与作为水热碎裂活动推动剂的非水挥发物有关。 DMD的成分评估可能会因撞击造成的水平和垂直运输而受到周围材料的污染，从而产生缺陷。在高分辨率的LROC NAC图像中可能会观察到这种效果。由于凹陷陡峭壁上的碎屑岩的翻新，在通风孔凹陷的斜坡上发现了非常暗的物质露头。因此，在较小的相角下，热碎裂材料是深色的，而在较大的相角下，它看起来几乎像周围的材料。这意味着露出的深色物质的相位依赖性很浅；即深色表面比其周围的表面光滑。这可能表明排出了气体，导致沉积物的粒状热碎屑材料流化。

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  • 来源
    《Planetary and space science》 |2018年第4期|22-38|共17页
  • 作者

    Shkuratov Y. G.; Ivanov M. A.; Korokhin V. V.; Kaydash V. G.; Basilevsky A. T.; Videen G.; Hradyska L. V.; Velikodsky Y. I.; Marchenko G. P.;

  • 作者单位

    Kharkov Natl Univ, Inst Astron, 35 Sumska St, UA-61022 Kharkov, Ukraine;

    GEOKHI RAS, Kosygin St 19, Moscow, Russia;

    Kharkov Natl Univ, Inst Astron, 35 Sumska St, UA-61022 Kharkov, Ukraine;

    Kharkov Natl Univ, Inst Astron, 35 Sumska St, UA-61022 Kharkov, Ukraine;

    GEOKHI RAS, Kosygin St 19, Moscow, Russia;

    Space Sci Inst, 4750 Walnut St Suite 205, Boulder, CO 80301 USA;

    Kharkov Natl Univ, Inst Astron, 35 Sumska St, UA-61022 Kharkov, Ukraine;

    Kharkov Natl Univ, Inst Astron, 35 Sumska St, UA-61022 Kharkov, Ukraine;

    Kharkov Natl Univ, Inst Astron, 35 Sumska St, UA-61022 Kharkov, Ukraine;

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