NEA大型超快速旋转器（436724）2011 UW158的物理表征
Physical characterization of NEA Large Super-Fast Rotator (436724) 2011 UW158
摘要：
尺寸大于0.15公里的小行星通常不会有小于2.2小时的周期，这是一个被称为无凝聚力自旋势垒的极限。这种障碍可以用无粘性碎石堆结构模型来解释。有几个例外，<rule>称为LSFR（大型超高速旋转器），如（455213）2001 OE84，（335433）2005 UW163和2011 XA3。近地小行星（436724）2011 UW158在2015年与地球飞越期间被一个国际光学和雷达观测小组跟踪。发现该NEA是一个新的候选LSFR。利用光学观测得到的光变曲线，我们可以得到振幅相位关系、恒星自转周期（$PS = 0.610752 \pm 0.000001$ h）、一个具有黄道坐标$ λ= 290^{\circ} \pm 3^{\circ}$、$β= 39^{\circ} \pm 2^{\circ}$和小行星3D模型的自转轴解。该模型与雷达观测结果定性一致。
英文摘要：
Asteroids of size larger than 0.15 km generally do not have periods smaller than 2.2 hours, a limit known as cohesionless spin barrier. This barrier can be explained by the cohesionless rubble-pile structure model. There are few exceptions to this <<rule>>, called LSFRs (Large Super-Fast Rotators), as (455213) 2001 OE84, (335433) 2005 UW163 and 2011 XA3. The near-Earth asteroid (436724) 2011 UW158 was followed by an international team of optical and radar observers in 2015 during the flyby with Earth. It was discovered that this NEA is a new candidate LSFR. With the collected lightcurves from optical observations we are able to obtain the amplitude-phase relationship, sideral rotation period ($PS = 0.610752 \pm 0.000001$ h), a unique spin axis solution with ecliptic coordinates $ λ= 290^{\circ} \pm 3^{\circ}$, $β= 39^{\circ} \pm 2^{\circ}$ and the asteroid 3D model. This model is in qualitative agreement with the results from radar observations.
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