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首页> 外文期刊>Planetary and space science >Shape modeling technique KOALA validated by ESA Rosetta at (21) Lutetia
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Shape modeling technique KOALA validated by ESA Rosetta at (21) Lutetia

机译：ESA Rosetta在（21）Lutetia验证了形状建模技术KOALA

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摘要

We present here a comparison of our results from ground-based observations of asteroid (21) Lutetia with imaging data acquired during the flyby of the asteroid by the ESA Rosetta mission. This flyby provided a unique opportunity to evaluate and calibrate our method of determination of size, 3-D shape, and spin of an asteroid from ground-based observations. Knowledge of certain observable physical properties of small bodies (e.g., size, spin, 3-D shape, and density) have far-reaching implications in furthering our under-standing of these objects, such as composition, internal structure, and the effects of non-gravitational forces. We review the different observing techniques used to determine the above physical properties of asteroids and present our 3-D shape-modeling technique KOALA - Knitted Occultation, Adaptive-optics, and Lightcurve Analysis - which is based on multi-dataset inversion. We compare the results we obtained with KOALA, prior to the flyby, on asteroid (21) Lutetia with the high-spatial resolution images of the asteroid taken with the OSIRIS camera on-board the ESA Rosetta spacecraft, during its encounter with Lutetia on 2010July 10. The spin axis determined with KOALA was found to be accurate to within 2°, while the KOALA diameter determinations were within 2% of the Rosetta-derived values. The 3-D shape of the KOALA model is also confirmed by the spectacular visual agreement between both 3-D shape models (KOALA pre- and OSIRIS post-flyby). We found a typical deviation of only 2 km at local scales between the profiles from KOALA predictions and OSIRIS images, resulting in a volume uncertainty provided by KOALA better than 10%. Radiometric techniques for the interpretation of thermal infrared data also benefit greatly from the KOALA shape model: the absolute size and geometric albedo can be derived with high accuracy, and thermal properties, for example the thermal inertia, can be determined unambiguously. The corresponding Lutetia analysis leads to a geometric albedo of 0.19 ± 0.01 and a thermal inertia below 40 J m~(-2)s~(-0.5)K~(-1) both in excellent agreement with the Rosetta findings. We consider this to be a validation of the KOALA method. Because space exploration will remain limited to only a few objects, KOALA stands as a powerful technique to study a much larger set of small bodies using Earth-based observations.
机译：在这里，我们将对小行星（21）Lutetia的地面观测结果与ESA Rosetta任务飞越小行星期间获得的成像数据进行比较。飞越提供了独特的机会，可以评估和校准我们从地面观测中确定小行星的大小，3-D形状和旋转的方法。了解小物体某些可观察到的物理特性（例如大小，自旋，3-D形状和密度）对于促进我们对这些物体的理解（如成分，内部结构以及物体的影响）具有深远的影响。非引力。我们回顾了用于确定小行星的上述物理特性的不同观测技术，并提出了基于多数据集反演的3-D形状建模技术KOALA-针织掩星，自适应光学和光曲线分析。我们将飞越之前使用KOALA在小行星（21）Lutetia上获得的结果与ESA Rosetta航天飞机上的OSIRIS相机在2010年7月与Lutetia遭遇期间使用OSIRIS相机拍摄的小行星的高空间分辨率图像进行了比较10.发现使用KOALA确定的旋转轴精确到2°以内，而KOALA直径确定在Rosetta派生值的2％以内。两种3-D形状模型（KOALA飞行前和OSIRIS飞越后）之间惊人的视觉一致性也证实了KOALA模型的3-D形状。我们发现，从KOALA预测到OSIRIS图像的剖面之间在局部尺度上的典型偏差仅为2 km，导致KOALA提供的体积不确定性优于10％。用于解释热红外数据的辐射技术也从KOALA形状模型中受益匪浅：可以以高精度得出绝对尺寸和几何反照率，并且可以明确确定热特性，例如热惯性。相应的Lutetia分析导致几何反照率达到0.19±0.01，热惯性低于40 J m〜（-2）s〜（-0.5）K〜（-1），这与Rosetta的发现非常吻合。我们认为这是对KOALA方法的验证。由于太空探索将仍然仅限于少数几个物体，因此KOALA是一项强大的技术，可以使用基于地球的观测来研究更大的小型物体。

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  • 来源
    《Planetary and space science》 |2012年第1期|p.200-212|共13页
  • 作者

    B. Carry; M. Kaasalainen; W.J. Merline; T.G. Mueller; L Jorda; J.D. Drummond; J. Berthier; L ORourke; J. Durech; M. Kueppers; A. Conrad; P. Tamblyn; C. Dumas; H. Sierks;

  • 作者单位

    European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Canada Madrid, Spain;

    Tampere University of Technology, P.O. Box 553, 33101 Tampere, Finland;

    Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302, USA;

    Max-Planck-Institut filr extraterrestrische Physik (MPE), Ciessenbachstrasse, 85748 Garching, Germany;

    Laboratoire d'Astrophysique de Marseille, Universite de Provence, Marseille, France;

    Starflre Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, NM 87117-577, USA;

    Institut de Mecanique Celeste et de Calcul des Ephemerides, Observatoire de Paris, UMR8028 CNRS, 77 av. Denfert-Rochereau 75014 Paris, France;

    European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Canada Madrid, Spain;

    Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holesovickach 2, 18000 Prague, Czech Republic;

    European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Canada Madrid, Spain;

    Max Planck Institute fuer Astronomy (MPA), Konigstuhl 17,69117 Heidelberg, Germany;

    Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302, USA;

    European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Canada Madrid, Spain;

    European Space Astronomy Centre, ESA, P.O. Box 78, 28691 Villanueva de la Canada Madrid, Spain;

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  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类
  • 关键词

    asteroid; (21) lutetia; disk-resolved imaging; KOALA; rosetta;

    机译：小行星;（21）黄体;盘分辨成像;KOALA;rosetta;

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