活跃小行星
![](http://images.weserv.nl/?url=//upload.wikimedia.org/wikipedia/commons/thumb/9/9f/596_Scheila%2C_5_minute_exposure%2C_Dec._12%2C_2010.jpg/250px-596_Scheila%2C_5_minute_exposure%2C_Dec._12%2C_2010.jpg)
活跃小行星是有著小行星般的轨道,是会呈现出彗星的视觉特征,但有著小行星轨道的太阳系小天体。也就是说,它们显示出彗发、彗尾或其它质量损失的视觉特征(像彗星),但它们的轨道仍在木星的轨道内(像小行星)[1][2]。这些天体在2006年被天文学家大卫·朱维特和Henry Hsieh命名为主带彗星(main-belt comets,MBCs)。但这个名字意味著它们的组成必然像彗星一样冰冷,也只存在于主小行星带;然而,随著活跃小行星数量的增长,情况并非总是如此[1][3][4]。
小行星(7968) 埃尔斯特-皮萨罗(Elst–Pizarro)是发现的第一颗活跃小行星。它在1979年被发现时是一颗小行星,后来在1996年被艾瑞克·怀特·埃尔斯特和圭多·皮萨罗(Guido Pizarro)发现它有尾巴,于是被命为133P/埃尔斯特-皮萨罗彗星[1][5]。
轨道
不同于彗星,活跃小行星的轨道大部分都在木星轨道附近或者离太阳更远的地方,它们的轨道通常与小行星的标准轨道没有区别(小行星)。朱维特对活跃小行星的定义为除了具有质量损失的视觉证据外,还具有以下轨道的天体[2]:
朱维特选择蒂塞朗参数3.08而不是3.0,来区分彗星和小行星,是因为木星本身的蒂塞朗参数是3.0。这样可以避免实际的太阳系偏离理想的限制性三体问题造成的模糊情况(与木星族彗星混淆) [2]。
最初确认的三颗活跃小行星轨道都靠在主小行星带的外侧运行[6]。
活动
![](http://images.weserv.nl/?url=//upload.wikimedia.org/wikipedia/commons/thumb/5/55/14060-Asteroid-P2013R3-Disintegration-20140306.jpg/300px-14060-Asteroid-P2013R3-Disintegration-20140306.jpg)
一些活跃小行星只在轨道的一部分,即近日点的附近,显示出彗星的尘埃尾。这有力的说明它们表面的挥发物在升华,同时带走了尘埃物质[9]。133P/埃尔斯特-皮萨罗彗星的活动是周期性的反复出现,在最近三次经过近日点附近时都观测到其活动[1]。这种活动在5-6年的轨道周期中,持续一或数个月[6],可能是由于在过去的100-1,000年中,轻微的撞击导致冰在表面覆盖或露出[6]。怀疑是撞击挖掘出这些表面下的挥发性物质,使它们暴露在太阳辐射下[6]。
在2010年1月发现的P/2010 A2 (LINEAR),被认为表现出彗星状的升华,因而最初被赋予彗星的名称:354P/LINEAR[10]。但P/2010 A2现在被认为是小行星撞击小行星后的残馀物[11][12]。对 (596) Scheila的观测表明,大量的尘埃是被另一颗直径约35米的小行星撞击产生的。
P/2013 R3
P/2013 R3 (卡特琳娜-泛星)是由R.E. Hill使用卡特琳娜巡天的0.68米施密特望远镜,和Bryce T. Bolin使用在哈雷卡拉的1.8米泛星1号望远镜的两位观测者独立发现的[13]。 泛星1号望远镜拍摄的照片显示,两个不同的辐射源相距仅3英寸,并有一条包覆著这两个辐射源的尾巴。在2013年10月,使用在拉帕尔马岛上的10.4米加那利大型望远镜后续观测拍摄的P/2013 R3影像,显示这颗彗星正在分裂[14]。叠加10月11和12日的CCD影像,检查后发现这颗主带彗星中心有一个明亮的凝聚体,伴随著它一起运行的还有3个分别标示为a、b、c的碎片。最亮的一个碎片在内华达山脉天文台1.52米望远镜的CCD影样中也检测得到[14]。
NASA报导了哈伯太空望远镜在2013年10月29日至2014年1月14日期间拍摄的一系列影像,显示这4个主体之间的间隔越来越大[15]。这是由太阳光照射产生的YORP效应增加了旋转的速度,使得离心力导致碎石堆分离[15]。
组成
一些活跃小行星显示出组成份像传统彗星一样冰冷的迹象,而另一些则被视为像岩石化的小行星一样。因为地球海洋的氘氢比太低,传统的彗星不可能是主要来源,因此有人假设主带彗星(活跃小行星)可能是地球上水的来源[16]。欧洲的科学家提出了一个名为"卡洛琳"(" Caroline ")的主带彗星样品返回任务",以收集灰尘样品并分析挥发物的含量[9]。
成员
'主带彗星'这个名词是基于轨道和它存在的位置扩展出来的分类,这并不意味著这些天体是彗星,或是环绕在核心周围的物质是如同彗星的挥发性物质。
该类别的确定成员包括:
名称 | 半长轴(AU) | 近日点 (AU) | TJup | 直径(km) | 原因 |
---|---|---|---|---|---|
谷神星 | 2.77 | 2.56 | 3.309 | 939 | 水升华[2] |
493 Griseldis | 3.12 | 2.57 | 3.140 | 46 | 撞击[17] |
596 Scheila | 2.92 | 2.44 | 3.209 | 113 | 撞击[18][19][20] |
2201 Oljato | 2.18 | 0.62 | 3.299 | 1.8 | 释气[21] |
3200法厄同 | 1.27 | 0.14 | 4.510 | 5.8 | 热压制和/或干燥裂缝[22] |
威尔逊-哈灵顿彗星 | 2.64 | 0.98 | 3.082 | 4 | 升华[23][24] |
6478 Gault | 2.31 | 1.86 | 3.461 | 3.7 | 旋转自旋增加[25][26][27] |
7968埃尔斯特-皮萨罗 (133P/埃尔斯特-皮萨罗,P/1996 N2) |
3.15 | 2.64 | 3.184 | 3.9 | 撞击/冰升华[28][29] |
(62412) 2000 SY178 | 3.15 | 2.90 | 3.197 | 5 | Rubble pile disintegration[30] |
101955 贝努 | 1.13 | 0.90 | 5.525 | 0.49 | 热压裂、挥发成分释放和/或撞击[31] |
118401 林尼尔(176P/林尼尔) | 3.19 | 2.57 | 3.167 | 4 | 撞击/冰升华[32] |
(300163) 2006 VW139(彗星288P) | 3.05 | 2.44 | 3.204 | 1.8 | 冰升华[33] |
233P/拉萨格拉(P/2005 JR71) | 3.04 | 1.79 | 3.081 | 撞击/冰升华 | |
238P/Read(P/2005 U1) | 3.16 | 2.36 | 3.154 | 0.6 | 撞击/冰升华[34] |
259P/加里德 (P/2008 R1) | 2.72 | 1.79 | 3.217 | 0.6 | 冰升华/轨道变化[35] |
311P/PANSTARRS (P/2013 P5) | 2.19 | 1.95 | 3.661 | 0.5 | 碎石堆崩解[36][37][38] |
313P/吉布斯(P/2003 S10) | 3.16 | 2.39 | 3.133 | 1.0 | 冰升华[39] |
324P/拉萨格拉(P/2010 R2) | 3.10 | 2.62 | 3.100 | 撞击/冰升华[40] | |
331P/吉布斯(P/2012 F5) | 3.00 | 2.88 | 3.228 | 碎石堆崩解[41][42] | |
348P/泛星(P/2011 A5) | 3.17 | 2.21 | 3.062 | ||
354P/林尼尔(P/2010 A2) | 2.29 | 2.00 | 3.583 | 0.22 | 撞击[43] |
358P/泛星(P/2012 T1) | 3.15 | 2.41 | 3.134 | 0.32 | 撞击/冰升华[44] |
367P/卡特琳娜(P/2011 CR42) | 3.51 | 2.53 | 3.042 | ||
P/2013 R3-A (卡特琳娜-泛星) | 3.03 | 2.20 | 3.184 | 0.2 | 碎石堆崩解[45] |
P/2013 R3-B (卡特琳娜-泛星) | 3.03 | 2.20 | 3.184 | 0.2 | Rubble pile disintegration[45] |
P/2014 C1(托塔) | 3.04 | 1.69 | 3.077 | ||
P/2015 X6(泛星) | 2.75 | 2.29 | 3.319 | 碎石堆崩解或冰升华[46] | |
P/2016 G1(泛星) | 2.58 | 2.04 | 3.367 | 0.2 | 撞击[47] |
P/2016 J1-A(泛星) | 3.17 | 2.45 | 3.113 | 0.5 | 撞击/冰升华/碎石堆崩解[48] |
P/2016 J1-B (泛星) | 3.17 | 2.45 | 3.113 | 0.2 | Impact/ice sublimation/rubble pile disintegration[48] |
P/2016 P1 (泛星) | 3.23 | 2.28 | 2.967 | ||
P/2017 S5 (阿特拉斯) | 3.17 | 2.18 | 3.092 | 0.5 | 冰升华[49] |
P/2017 S8 (泛星) | 2.78 | 1.68 | 3.040 | ||
P/2017 S9 (泛星) | 3.16 | 2.20 | 3.087 | ||
P/2018 P3 (泛星) | 3.01 | 1.76 | 3.096 | ||
P/2019 A3 (泛星) | 3.15 | 2.31 | 3.100 | ||
P/2019 A4 (泛星) | 2.61 | 2.36 | 3.365 | ||
P/2019 A7 (泛星) | 3.19 | 2.68 | 3.103 | ||
P/2020 O1 (莱蒙-泛星) | 2.65 | 2.33 | 3.376 | ||
P/2021 A5 (泛星) | 3.05 | 2.62 | 3.147 |
探索
![](http://images.weserv.nl/?url=//upload.wikimedia.org/wikipedia/commons/thumb/2/23/PIA23554-AsteroidBennu-EjectingParticles-20190106.jpg/300px-PIA23554-AsteroidBennu-EjectingParticles-20190106.jpg)
卡斯塔利亚是一个提议中的太空任务,用机器人探测133P/埃尔斯特-皮萨罗,并对小行星带中的水进行首次的"原地"量测,从而帮助解开地球水起源之谜[50]。领导人是来自英国开放大学的科林·斯诺德格拉斯(Colin Snodgrass)。 卡斯塔利亚是在2015年和2016年向欧洲太空总署的宇宙视觉计画M4和M5两度提出企划,但都没有被选中。团队仍在持续完善任务概念和科学目标[50]。由于建造时间和轨道动力学的要求,建议发射日期为2028年10月[50]。
OSIRIS-REx在进入近地小行星101955 贝努的绕行轨道后不久,在2019年1月6日,首度观测到这颗小行星发生粒子抛射事件,导致它被划分为活跃小行星;这也是太空船首次近距离观测到小行星的活动。自此次事件之后,它至少观测到10起其它的此类事件[3]。这些观测到的质量损失事件规模,比以前用望远镜在其它小行星上观测到的要小得多,表明在活跃小行星上存在质量损失事件量级的连续与统一是一体的 [31]。
相关条目
外部链接
- Henry Hsieh's 主带彗星,对细节有较详尽的说明。
- 行星学会在MBCs 的文章。(页面存档备份,存于互联网档案馆)
- 在 MBCs讨论主带彗星和其他彗星在水的特征上可能有的区别。(页面存档备份,存于互联网档案馆)
- 大卫·朱维特的活跃小行星(页面存档备份,存于互联网档案馆)
- YouTube 对大卫·朱维特的访问(页面存档备份,存于互联网档案馆) (大约在影带的第9分钟有谈到主带彗星)
- 大卫·朱维特触发撞击机制的图。(页面存档备份,存于互联网档案馆)
- Comet-like appearance of (596) Scheila(页面存档备份,存于互联网档案馆)
- Project T3: Finding Comets in the Asteroid Population
- Proper elements of active asteroids at Asteroid Families Portal (页面存档备份,存于互联网档案馆)
- Discussion of possible differences in characteristics of the water in MBCs and other comets (页面存档备份,存于互联网档案馆)
- Jewitt, David. The Active Asteroids. The Astronomical Journal. 2012, 143 (3): 66. Bibcode:2012AJ....143...66J. S2CID 45208650. arXiv:1112.5220
. doi:10.1088/0004-6256/143/3/66.
- Hsieh, Henry H.; Yang, Bin; Haghighipour, Nader; Kaluna, Heather M.; Fitzsimmons, Alan; Denneau, Larry; Novaković, Bojan; Jedicke, Robert; Wainscoat, Richard J.; Armstrong, James D.; Duddy, Samuel R.; Lowry, Stephen C.; Trujillo, Chadwick A.; Micheli, Marco; Keane, Jacqueline V.; Urban, Laurie; Riesen, Timm; Meech, Karen J.; Abe, Shinsuke; Cheng, Yu-Chi; Chen, Wen-Ping; Granvik, Mikael; Grav, Tommy; Ip, Wing-Huen; Kinoshita, Daisuke; Kleyna, Jan; Lacerda, Pedro; Lister, Tim; Milani, Andrea; et al. DISCOVERY OF MAIN-BELT COMET P/2006 VW 139 BY Pan-STARRS1. The Astrophysical Journal. 2012, 748 (1): L15. Bibcode:2012ApJ...748L..15H. S2CID 8693844. arXiv:1202.2126
. doi:10.1088/2041-8205/748/1/L15.
- New Comet: P/2012 T1 (PANSTARRS) (页面存档备份,存于互联网档案馆) (Remanzacco Observatory : 16 Oct 2012)
- Ferrín, Ignacio; Zuluaga, Jorge; Cuartas, Pablo. The location of Asteroidal Belt Comets (ABCs), in a comet's evolutionary diagram: The Lazarus Comets. Monthly Notices of the Royal Astronomical Society. 2013, 434 (3): 1821–1837. Bibcode:2013MNRAS.434.1821F. S2CID 118177774. arXiv:1305.2621
. doi:10.1093/mnras/stt839.
- P/2013 R3: a Main Belt Comet that is breaking apart. J. Licandro (页面存档备份,存于互联网档案馆) New images obtained with the GTC
参考资料
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|journal=
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