VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis
VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis
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最大主带小行星的 VLT/SPHERE 成像调查：最终结果和综合
DOI：
10.1051/0004-6361/202141781
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发表时间：
2021
影响因子：
6.5
通讯作者：
Marchis, F.
中科院分区：
文献类型：
--
作者：
Vernazza, P.;Ferrais, M.;Jorda, L.;Hanuš, J.;Carry, B.;Marsset, M.;Brož, M.;Fetick, R.;Viikinkoski, M.;Marchis, F.
直到最近，绝大多数最大的（D≥ 100公里）主带小行星的三维形状，因此密度（将体积估计与现有质量估计相结合时）和表面地形仍然没有受到很好的约束。SPHERE/ZIMPOL仪器性能的提高为地面小行星探测打开了新的大门。目的为了限制大型小行星代表性样本的形成和演化，我们用VLT/SPHERE/ZIMPOL对42颗大型主带小行星进行了高角分辨率成像调查。我们的小行星样本包括39个D ≥ 100 km的天体，特别是大多数D ≥ 200 km的主带小行星（20/23）。此外，它很好地反映了成分的多样性存在于主带的采样机构属于以下分类类：A，B，C，Ch/Cgh，E/M/X，K，P/T，S，和V。MethodsThe SPHERE/ZIMPOL图像首先被用来重建所有目标的三维形状与ADAM和MPCD重建方法。随后，我们进行了详细的形状分析和约束的密度，每个目标使用现有的质量估计，包括我们自己的质量估计的情况下，多system.ResultsThe重建的形状分析，使我们能够确定两个家庭的对象作为其直径的函数，即“球形”和“细长”机构。旋转周期的差异似乎是这种双峰性的主要来源。此外，除了一个天体（216 Kleopatra）外，所有天体都位于沿着麦克劳林层序，大型富挥发性天体最接近麦克劳林层序。我们的结果进一步揭示了大多数多重系统的原色具有短于6小时的旋转周期和细长的形状（cscina ≤ 0.65）。在我们的样本中，密度范围从~1.3 g cm−3（87 Sylvia）到~4.3 g cm−3（22 Kalliope）。此外，密度分布似乎是强烈的双峰与挥发物贫（ρ≥ 2.7 g cm−3）和挥发物丰富（ρ≤ 2.2 g cm−3）的机构。最后，我们的调查沿着与以前的观测提供的证据支持的可能性，一些C-复合体可能是内在相关的IDP类P-和D-型小行星，代表不同层的同一个机构（C：核心; P/D：外壳）。因此，我们建议，P/D型和一些C型可能有相同的起源在原始trans-Neptunian盘。
ContextUntil recently, the 3D shape, and therefore density (when combining the volume estimate with available mass estimates), and surface topography of the vast majority of the largest (D≥ 100 km) main-belt asteroids have remained poorly constrained. The improved capabilities of the SPHERE/ZIMPOL instrument have opened new doors into ground-based asteroid exploration.AimsTo constrain the formation and evolution of a representative sample of large asteroids, we conducted a high-angular-resolution imaging survey of 42 large main-belt asteroids with VLT/SPHERE/ZIMPOL. Our asteroid sample comprises 39 bodies withD≥ 100 km and in particular mostD≥ 200 km main-belt asteroids (20/23). Furthermore, it nicely reflects the compositional diversity present in the main belt as the sampled bodies belong to the following taxonomic classes: A, B, C, Ch/Cgh, E/M/X, K, P/T, S, and V.MethodsThe SPHERE/ZIMPOL images were first used to reconstruct the 3D shape of all targets with both the ADAM and MPCD reconstruction methods. We subsequently performed a detailed shape analysis and constrained the density of each target using available mass estimates including our own mass estimates in the case of multiple systems.ResultsThe analysis of the reconstructed shapes allowed us to identify two families of objects as a function of their diameters, namely “spherical” and “elongated” bodies. A difference in rotation period appears to be the main origin of this bimodality. In addition, all but one object (216 Kleopatra) are located along the Maclaurin sequence with large volatile-rich bodies being the closest to the latter. Our results further reveal that the primaries of most multiple systems possess a rotation period of shorter than 6 h and an elongated shape (c∕a≤ 0.65). Densities in our sample range from ~1.3 g cm−3(87 Sylvia) to ~4.3 g cm−3(22 Kalliope). Furthermore, the density distribution appears to be strongly bimodal with volatile-poor (ρ≥ 2.7 g cm−3) and volatile-rich (ρ≤ 2.2 g cm−3) bodies. Finally, our survey along with previous observations provides evidence in support of the possibility that some C-complex bodies could be intrinsically related to IDP-like P- and D-type asteroids, representing different layers of a same body (C: core; P/D: outer shell). We therefore propose that P/ D-types and some C-types may have the same origin in the primordial trans-Neptunian disk.
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影响因子：
3.2
作者：
M. Shepard;J. Richardson;P. Taylor;L. A. Rodriguez-Ford;A. Conrad;I. Pater;M. Ádámkovics;K. Kleer;J. Males;K. Morzinski;L. Close;M. Kaasalainen;M. Viikinkoski;B. Timerson;V. Reddy;C. Magri;M. Nolan;E. Howell;L. Benner;J. Giorgini;B. Warner;A. Harris
通讯作者：
M. Shepard;J. Richardson;P. Taylor;L. A. Rodriguez-Ford;A. Conrad;I. Pater;M. Ádámkovics;K. Kleer;J. Males;K. Morzinski;L. Close;M. Kaasalainen;M. Viikinkoski;B. Timerson;V. Reddy;C. Magri;M. Nolan;E. Howell;L. Benner;J. Giorgini;B. Warner;A. Harris
影响因子：
6.5
作者：
R. F'etick;L. Jorda;P. Vernazza;M. Marsset;A. Drouard;Thierry Fusco;B. Carry;F. Marchis;J. Hanuš;M. Viikinkoski;M. Birlan;P. Bartczak;J. Berthier;J. Castillo-Rogez;F. Cipriani;F. Colas;G. Dudziński;C. Dumas;M. Ferrais;E. Jehin;M. Kaasalainen;A. Kryszczyńska;P. Lamy;H. Coroller;A. Marciniak;T. Michałowski;P. Michel;L. Mugnier;B. Neichel;M. Pajuelo;E. Podlewska-Gaca;T. Santana-Ros;P. Tanga;F. Vachier;A. Vigan;O. Witasse;Bin Yang
通讯作者：
R. F'etick;L. Jorda;P. Vernazza;M. Marsset;A. Drouard;Thierry Fusco;B. Carry;F. Marchis;J. Hanuš;M. Viikinkoski;M. Birlan;P. Bartczak;J. Berthier;J. Castillo-Rogez;F. Cipriani;F. Colas;G. Dudziński;C. Dumas;M. Ferrais;E. Jehin;M. Kaasalainen;A. Kryszczyńska;P. Lamy;H. Coroller;A. Marciniak;T. Michałowski;P. Michel;L. Mugnier;B. Neichel;M. Pajuelo;E. Podlewska-Gaca;T. Santana-Ros;P. Tanga;F. Vachier;A. Vigan;O. Witasse;Bin Yang
CM类小行星的均质内部结构（41）Daphne
影响因子：
6.5
作者：
Carry, B.;Vachier, F.;Berthier, J.;Marsset, M.;Vernazza, P.;Grice, J.;Merline, W. J.;Lagadec, E.;Fienga, A.;Conrad, A.
通讯作者：
Conrad, A.
未分组和稀有陨石的可见红外光谱进一步限制了陨石与小行星的联系
影响因子：
3.2
作者：
L. K. Ruggiu;P. Beck;J. Gattacceca;J. Eschrig
通讯作者：
J. Eschrig
顽辉石球粒陨石密度、磁化率和孔隙率
DOI：
--
发表时间：
2010
期刊：
影响因子：
--
作者：
R. Macke;G. Consolmagno;D. Britt;M. Hutson
通讯作者：
M. Hutson