分裂活动小行星P/2016 J1（PANSTARRS）
Split Active Asteroid P/2016 J1 (PANSTARRS)
摘要：
我们提出了一个光度和天体测量研究分裂活跃小行星P/2016 J1（PANSTARRS）。两个分量（以下称为J1-A和J1-B）在当前历元之前1500天（2012年5月至6月）或2300天（2010年4月）分离$\sim$，对于前一种情况，分离速度为$V_{\mathrm{sep}} = 0.70 \pm 0.02$ m s $^{-1}$，对于后一种情况，分离速度为$0.83 \pm 0.06$ m s $^{-1}$。凯克测光显示，这两个碎片具有类似太阳的颜色，与原始的C-和G-型小行星的颜色相当。对于一个名义上的彗星状的彗星，$p_{R} = 0.04$，有效的，灰尘污染的横截面估计为2.4公里$^{2}$的J1-A，和0.5公里$^{2}$的J1-B。我们估计J1-A的核半径在$140 \lesssim R_{\mathrm{N}} \lesssim 900$ m范围内，J1-B的核半径在$40 \lesssim R_{\mathrm{N}} \lesssim 400$ m范围内。一个syndyne-synchrone模拟表明，这两个组件已经活跃了3至6个月，通过喷射尘埃颗粒的速度$\sim$ 0.5 m s $^{-1}$与速率$\sim$ 1 kg s $^{-1}$为J1-A和0.1 kg s $^{-1}$为J1-B。在它目前的轨道上，2016 J1的旋转加速和脱挥发分时间与太阳系的年龄相比非常小，这就提出了为什么这个物体仍然存在的问题。我们认为，以前埋在这颗小行星内的冰可能通过一次小撞击暴露在表面，然后升华扭矩迅速驱使它分裂。由于旋转不稳定性，预计还会发生进一步的解体事件。
英文摘要：
We present a photometric and astrometric study of the split active asteroid P/2016 J1 (PANSTARRS). The two components (hereafter J1-A and J1-B) separated either $\sim$1500 days (2012 May to June) or 2300 days (2010 April) prior to the current epoch, with a separation speed $V_{\mathrm{sep}} = 0.70 \pm 0.02$ m s$^{-1}$ for the former scenario, or $0.83 \pm 0.06$ m s$^{-1}$ for the latter. Keck photometry reveals that the two fragments have similar, Sun-like colors which are comparable to the colors of primitive C- and G-type asteroids. With a nominal comet-like albedo, $p_{R} = 0.04$, the effective, dust-contaminated cross sections are estimated to be 2.4 km$^{2}$ for J1-A, and 0.5 km$^{2}$ for J1-B. We estimate that the nucleus radii lie in the range $140 \lesssim R_{\mathrm{N}} \lesssim 900$ m for J1-A and $40 \lesssim R_{\mathrm{N}} \lesssim 400$ m, for J1-B. A syndyne-synchrone simulation shows that both components have been active for 3 to 6 months, by ejecting dust grains at speeds $\sim$0.5 m s$^{-1}$ with rates $\sim$1 kg s$^{-1}$ for J1-A and 0.1 kg s$^{-1}$ for J1-B. In its present orbit, the rotational spin-up and devolatilization times of 2016 J1 are very small compared to the age of the solar system, raising the question of why this object still exists. We suggest that ice that was formerly buried within this asteroid became exposed at the surface, perhaps via a small impact, and that sublimation torques then rapidly drove it to break-up. Further disintegration events are anticipated due to the rotational instability.
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