The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta
The rotation state of 67P/Churyumov-Gerasimenko from approach observations with the OSIRIS cameras on Rosetta
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使用罗塞塔上的 OSIRIS 相机进行进近观测所得的 67P/Churyumov-Gerasimenko 的旋转状态
DOI：
10.1051/0004-6361/201424590
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发表时间：
2014
影响因子：
6.5
通讯作者：
Mottola S
中科院分区：
文献类型：
--
作者：
Mottola S
AimsApproach观测与光学，光谱，和红外远程成像系统（OSIRIS）实验板载罗塞塔被用来确定旋转周期，旋转轴的方向，和状态的旋转彗星67 P的nucleus.MethodsPhotometric时间序列的67 P已被收购OSIRIS自后唤醒调试的有效载荷在2014年3月。傅立叶分析和凸形反演方法已被应用到罗塞塔数据，以及现有的地面observation.ResultsEvidence发现，67 P的旋转速率已显着改变附近的时间，其2009年近日点通道，可能是由于升华引起的扭矩。发现2009年近日点前后的恒星自转周期P1 = 12.76129 ± 0.00005 h和P2 = 12.4043 ± 0.0007 h与观测值拟合最好。在光变曲线中没有发现多重周期性的迹象，这意味着彗星目前正处于围绕其最大惯性矩轴的简单旋转状态。我们导出了自旋矢量为J2000的黄道坐标λ= 65° ± 15°，β= + 59° ± 15°，对应于赤道坐标RA = 22°，Dec = + 76°的黄道自转模型。然而，我们发现，在λ= 275° ± 15°，β= + 50° ± 15°（或RA = 274°，Dec = + 27°）的镜像解也是可能的，因为在黄道面附近进行观测的测光问题的内在模糊性。
AimsApproach observations with the Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) experiment onboard Rosetta are used to determine the rotation period, the direction of the spin axis, and the state of rotation of comet 67P’s nucleus.MethodsPhotometric time series of 67P have been acquired by OSIRIS since the post wake-up commissioning of the payload in March 2014. Fourier analysis and convex shape inversion methods have been applied to the Rosetta data as well to the available ground-based observations.ResultsEvidence is found that the rotation rate of 67P has significantly changed near the time of its 2009 perihelion passage, probably due to sublimation-induced torque. We find that the sidereal rotation periodsP1= 12.76129 ± 0.00005 h andP2= 12.4043 ± 0.0007 h for the apparitions before and after the 2009 perihelion, respectively, provide the best fit to the observations. No signs of multiple periodicity are found in the light curves down to the noise level, which implies that the comet is presently in a simple rotation state around its axis of largest moment of inertia. We derive a prograde rotation model with spin vector J2000 ecliptic coordinatesλ= 65° ± 15°,β= + 59° ± 15°, corresponding to equatorial coordinates RA = 22°, Dec = + 76°. However, we find that the mirror solution, also prograde, atλ= 275° ± 15°,β= + 50° ± 15° (or RA = 274°, Dec = + 27°), is also possible at the same confidence level, due to the intrinsic ambiguity of the photometric problem for observations performed close to the ecliptic plane.
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