偏心互轨主带双星系统
Main Belt Binary Asteroidal Systems With Eccentric Mutual Orbits
摘要：
利用8米至10米级望远镜及其自适应光学（AO）系统，我们于2003年启动了一项长期的自适应光学活动，重点关注四个双星小行星系统：（130）Elektra，（283）Emma，（379）Huenna和（3749）Balam。对这些数据的分析证实了他们的小行星卫星的存在。我们没有在这些系统周围检测到任何额外的卫星，尽管我们有能力检测到一个松散结合的碎片（位于1/4 x RHill），直径比主要的小40倍。其卫星的轨道显示出显著的偏心率，从0.1到0.9不等，表明起源不同。根据AO的大小估计，我们发现（130）Elektra和（283）Emma分别是G型和P型小行星，它们具有显著的孔隙度（30-60%，以CI-CO陨石为类似物），它们的卫星偏心率（e~0.1）可能是由于潮汐效应的激发。(379)Huenna和（3749）Balam是两个松散结合的双星系统，很可能是由相互俘获形成的。（3749）Balam可能有很高的体积密度，类似于（433）Eros，另一颗S-型小行星，而且应该也是破碎不良。(379)Huenna似乎显示了这两个特征：小卫星的轨道在稳定性方面远离主星（20% x RHill），但主星的孔隙率很大（30-60%）。
英文摘要：
Using 8m-10m class telescopes and their Adaptive Optics (AO) systems, we conducted a long-term adaptive optics campaign initiated in 2003 focusing on four binary asteroid systems: (130) Elektra, (283) Emma, (379) Huenna, and (3749) Balam. The analysis of these data confirms the presence of their asteroidal satellite. We did not detect any additional satellite around these systems even though we have the capability of detecting a loosely-bound fragment (located at 1/4 x RHill) ~40 times smaller in diameter than the primary. The orbits derived for their satellites display significant eccentricity, ranging from 0.1 to 0.9, suggesting a different origin. Based on AO size estimate, we show that (130) Elektra and (283) Emma, G-type and P-type asteroids respectively, have a significant porosity (30-60% considering CI-CO meteorites as analogs) and their satellite's eccentricities (e~0.1) are possibly due to excitation by tidal effects. (379) Huenna and (3749) Balam, two loosely bound binary systems, are most likely formed by mutual capture. (3749) Balam's possible high bulk density is similar to (433) Eros, another S-type asteroid, and should be poorly fractured as well. (379) Huenna seems to display both characteristics: the moonlet orbits far away from the primary in term of stability (20% x RHill), but the primary's porosity is significant (30-60%).
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
