不確定警告:由于遙遠(yuǎn)天體體積較小，過于黯淡，其距離和公轉(zhuǎn)/自行速度無法被精確測量，數(shù)據(jù)來自維基百科詞條List of Solar System objects by greatest aphelion

AU:地球到太陽的平均距離149,597,582.503千米

LY:光年(1LY=63241.2488AU)

PC:秒差距(1PC=3.26157LY)

希爾斯云(奧爾特云內(nèi)層)離太陽最近距離約為2000-5000AU(0.03-0.08LY)

太陽系中的彗星被認(rèn)為有兩個(gè)獨(dú)立的起源地。短周期彗星（周期在200年以下）一般認(rèn)為來自于柯伊伯帶或離散盤，這兩個(gè)相互連接的圓盤形區(qū)域位于海王星的軌道以外，距離太陽約30天文單位，由冰小天體組成。長周期彗星（周期可達(dá)數(shù)千年），如海爾-波普彗星，則可能源自奧爾特云?？乱敛畮祗w的軌道相對穩(wěn)定，因此來自柯伊伯帶的彗星應(yīng)該為數(shù)不多；另一方面，離散盤在天體動(dòng)力學(xué)上較為活躍，作為彗星來源的可能性也大得多。來自離散盤的彗星進(jìn)入外行星的軌道之內(nèi)，此時(shí)被稱為半人馬小行星。繼續(xù)被移入內(nèi)太陽系的半人馬小行星，就成為了短周期彗星。

太陽系內(nèi)及進(jìn)入太陽系的系外彗星理論遠(yuǎn)日點(diǎn)

未經(jīng)說明，列表中所有彗星均為不回歸型彗星

C/2012 S4? ? ? ?504,443?AU (8.0 ly/2.45pc)

C/2012 CH17??279,825?AU (4.4?ly/1.35pc)

C/2008 C1? ? ? ?203,253?AU (3.2?ly/0.98pc)

C/1992 J1? ? ? ?154,202?AU (2.4?ly/0.73pc)

C/2007 N3? ??? 144,828?AU (2.3?ly)

C/2017 T2? ? ? ?117,212?AU (1.9?ly)

C/1937 N1? ?? ?115,031?AU (1.8?ly)

C/1972 X1? ? ? 108,011?AU (1.7?ly)

C/2014 R3? ? ? ?80,260?AU (1.3?ly)

C/2015 O1? ? ? ?77,092?AU (1.2?ly)

C/2001 C1? ? ? ?76,230?AU (1.2?ly)

C/2002 J4? ? ? ?57,793?AU (0.91?ly)

C/1910 A1? ? ? ?51,589?AU (0.82?ly)

C/1958 D1? ? ? ?46,408?AU (0.73?ly)

C/1986 V1? ? ? ?37,825?AU (0.60?ly)

C/2005 G1? ? ? ?37,498?AU (0.59?ly)

C/2006 W3? ? ??35,975?AU (0.57?ly)

C/2009 W2? ? ? 31,059?AU (0.49?ly)

C/2005 L3? ? ? ?26,779?AU (0.42?ly)

C/2004 YJ35? 26,433?AU (0.42?ly)

C/2003 H3? ? ??26,340?AU (0.42?ly)

C/2010 L3? ? ? ?25,609?AU (0.40?ly)

C/1902 R1? ?? ??25,066?AU (0.40?ly)

C/1889 G1? ? ? ?24,784?AU (0.39?ly)

C/2007 VO53? 24,383?AU (0.39?ly)

C/2012 U1? ? ? ?24,373 AU

C/1958 R1? ? ? ?24,299 AU

C/2010 D3? ? ? ?23,255 AU

C/2001 K5? ? ? ?22,810 AU

C/1991 R1? ? ???22313AU

C/2009 U5? ? ? ?21191AU

C/2014 OE4? ? ?21176AU

C/1977 V1? ? ? ?19631AU

C/1888 P1? ? ? ?19612AU

C/2011 N2? ? ? ?19536AU

C/1910 P1? ? ? ?19190AU

C/1882 F1? ? ? ?19135AU

C/1984 W2? ? ??19000AU

C/2002 K1? ? ? ?18858AU

C/2002 C2? ? ? ?18034AU

C/2008 Q3? ? ???17850AU

C/2013 F2? ? ? ?16812AU

C/2010 H1? ? ? ?16721AU

C/1999 T1? ? ? ?16693AU

C/2004 P1? ? ? ?16107AU

C/1974 F1?? ? ? ?15129AU

C/2013 J5?? ? ???14297AU

C/2006 Q1?? ? ? 13768AU

C/2014 Q6?? ?? ??13761AU

C/1975 V1-A?? ?13560AU

C/1999 F1? ? ? ??13390AU

觀測弧最遠(yuǎn)彗星

Comet West?70,000?AU?(1.1 ly)

C/1999 F1? ??66,600?AU(1.05ly)

C/2012 S4? ??5700?AU?

C/1996 B2? ? 3410?AU

C/1910 A1? ? 2974 AU?

C/1992 J1? ? 3650?AU

C/2007 N3?? ?2400AU

遠(yuǎn)日點(diǎn)最遠(yuǎn)的小行星和矮行星(大于200AU)

單位:AU? ? ?

2017 MB7? ? ???6082 ±282

2014 FE72? ? ? 3390 ±1400

2012 DR30? ?? 3248.7 ±7.5

2005 VX3? ? ? ? 2081 ±430

2013 BL76? ? ? 2064.1 ±5.1

541132 Leleākūhonua? ???2037 ±340

2015 KG163???1612 ±12

(308933) 2006 SQ372? ? ?1547 ±2

2013 SY99? ? ? 1297 ±41

2002 RN109? ?1126 ±49

2013 AZ60? ? ? 1062.00 ±0.49

(87269) 2000 OO67? ? ? ? ? 1000.3 ±3.8

2007 DA61? ? ???990 ±130

(523622) 2007 TG422? ? ? 902.29 ±0.44

90377 Sedna? ?890.5 ±1.1

2015 BP519? ? ?863 ±17

2017 UR52? ? ? ?822 ±230

2015 RX245? ? ?778 ±63

2010 BK118? ? ?772.20 ±0.46

2018 MP8? ? ? ? ?747 ±23

(418993) 2009 MS9? ? ? ? ?707.17 ±0.22

2010 GB174? ? ?671 ±46

2013 RF98? ? ? ?665 ±22

2015 GT50? ? ? ?626.7 ±5.6

(474640) 2004 VN112? ? ?583.6 ±3.2

2013 FT28? ? ???582 ±20

(336756) 2010 NV1? ? ? ?? ?570.76 ±0.18

2017 SN33? ? ? 560 ±56

2014 SR349? ? 545 ±33

2011 OR17? ? ??532.13 ±0.29

(523719) 2014 LM28? ? ? ?524.28 ±0.14

1996 PW? ? ? ? ? 500.56 ±0.64

2012 KA51? ? ??444 ±4000

2012 VP113? ? 431.2 ±2.3

2014 GR53? ? ? 421.47 ±0.08

(82158) 2001 FP185? ? ? ? 419.14 ±0.12

2015 RY245? ???414.5 ±7.7

2002 GB32? ? ???402.41 ±0.99

(148209) 2000 CR105? ? ?398.1 ±1.1

2015 FK37? ? ? ??377 ±130

2017 CW32? ????372.37 ±0.17

2013 FS28? ?? ? 360 ±180

2003 SS422? ?? 360 ±270

2015 GX55? ? ? ?352.6 ±2.6

(505478) 2013 UT15? ? ? ? 347.5 ±1.4

2012 GU11? ? ? ?346.89 ±0.13

(468861) 2013 LU28? ? ? ? ?342.26 ±0.22

2007 VJ305? ? ?342.13 ±0.30

2010 GW147? ?328.97 ±0.75

2017 DO121? ? 328 ±2300

(469750) 2005 PU21? ? ? ???313.15 ±0.12

2013 UH15? ????305 ±15

(506479) 2003 HB57? ? ? ? ?294.2 ±1.2

(508338) 2015 SO20? ? ? ? ?290.51 ±0.07

2015 KH163? ? 274.4 ±1.0

2015 TS350? ? ?272.23 ±0.13

(496315) 2013 GP136? ? ? ?269.08 ±0.33

2005 RH52? ? ? ?266.30 ±0.35

2017 UW51? ? ? 265.97 ±0.15

(445473) 2010 VZ98? ? ? ? ? 265.88 ±0.04

2013 JO64? ? ? ?263.03 ±0.22

2014 OS394? ???256.59 ±0.10

2014 JW80? ? ? ?247.08 ±0.17

2014 OR394? ? ?245.09 ±0.17

2014 SS349? ? ?243 ±24

2007 LH38? ? ? ?239.99 ±0.15

2007 TU431? ???234 ±2900

(353222) 2009 YD7? ? ? ? ? ?230.54 ±0.08

2014 UY224? ???230 ±16

2013 GJ138?? ? 226.99 ±0.12

2015 KE172? ? ?222.11 ±0.11

(54520) 2000 PJ30? ? ? ? ? ?222.0 ±1.9

2015 RB279? ? ?219.26 ±0.10

(523718) 2014 KZ101? ? ??218.84 ±0.02

2007 TC434? ? ?217.24 ±0.09

2018 VG18? ? ? ?208.5

(523726) 2014 MJ70? ? ? ? 205.51 ±0.04

(181902) 1999 RD215? ? ? 204.83 ±0.24

2014 NV65? ? ? ?204.6 ±1.5

2015 VD168? ? ?204.35 ±0.49

(523778) 2014 YK50? ? ? ? ?202.30 ±0.02

1999 CZ118? ? ?202.29 ±0.33

1999 DP8? ? ? ? ?200 ±5,500,000??(90?ly)

小于200AU

2018 DF4? ? ? ? ?198.71 ±0.11

2004 NN8? ? ? ??192.58 ±0.13

(65489) Ceto? ?186.92 ±0.02

(303775) 2005 QU? ? ? ? ????182?186.33 ±0.03

2018 KH3?? ? ???185.68 ±0.51

2015 DW224? ?185.08 ±0.05

(437360) 2013 TV158? ? ? 182.86 ±0.02

(523771) 2014 XP40? ? ? ? 182.01 ±0.02

2014 KA102? ? 179.21 ±0.09

2014 UZ224? ??179 ±16

(184212) 2004 PB112? ? ??177.93 ±0.19

(29981) 1999 TD10? ? ? ? ? 177.69 ±0.04

2000 KP65? ? ???177.2 ±3.5

2012 FL84? ? ? ?173.89 ±0.07

2014 DT143? ??173.56 ±0.07

2015 KR174? ??173.11 ±0.12

2014 WY508? ?172.85 ±0.03

(91554) 1999 RZ215? ? ? ? 172.23 ±0.12

2015 RC279? ??171.96 ±0.23

2015 GY55? ? ? 169.90 ±0.09

2014 FL72? ? ? ?169.7 ±5.3

2014 JE80? ? ? ?168.75 ±0.07

2014 SR350? ??166 ±23

2011 OB60? ? ? 164.26 ±0.09

2015 RK245? ??161.22 ±0.03

2014 YD50? ? ??160.36 ±0.03

2011 WJ157? ?159.95 ±0.03

2015 VB168? ??159.57 ±0.89

2010 ER65? ? ??159.38 ±0.01

2015 GU55? ? ??157.73 ±0.10

2013 LD16? ? ? 157.43 ±0.09

2011 BR163????157.12 ±0.04

(118702) 2000 OM67? ? ?157.08 ±0.20

2014 SU349? ? 160 ±310

旅行者一號(hào)距地距離? 159.39(0.926光天)

2008 ST291? ??156.40 ±0.34

2014 SW349? ?156 ±20

2011 HO60? ? ? 155.71 ±0.03

2003 QM112? ?155 ±12

(470593) 2008 LP17? ? ??153.25 ±0.02

(26181) 1996 GQ21? ? ? ?151.76 ±0.02

2014 FJ72? ? ? ? ?151.0 ±7.5

(145474) 2005 SA278???149.18 ±0.02

1999 CY118? ? ? 149.16 ±0.16

2005 RP43? ? ? ??148.63 ±0.02

2006 HQ122? ? ?148.05 ±0.03

2015 PK312? ? ??148 ±52

2010 JJ124? ? ???147.62 ±0.18

2017 RG16? ? ? ? ?147.45 ±0.03

2012 UK177? ? ???147.25 ±0.43

2014 XS3? ? ? ? ? ? 146.89 ±0.03

(523698) 2014 GD54? ??146.82 ±0.02

(307982) 2004 PG115? 144.93 ±0.01

(145451) 2005 RM43? ? 144.05 ±0.02

(500832) 2013 GZ136? ?143.43 ±0.06

2015 GB56? ? ? ? ??143.16 ±0.10

2007 FN51? ? ? ? ? 142.78 ±0.10

2014 OY393? ? ? ??142 ±20

(82155) 2001 FZ173? ? ??141.82 ±0.08

2003 YQ179? ? ? ??140.17 ±0.06

2002 PR170? ? ? ? 140 ±35

1999 CF119? ? ? ? 140.02 ±0.12

2007 LF38? ? ? ? ? ?138.90 ±0.09

2015 GW55? ? ? ???137.6 ±1.6

2008 JO41? ? ? ? ??137.60 ±0.05

2005 EF304? ? ?? ?137.55 ±0.10

(523798) 2017?? CX33?137.10 ±0.02

2015 PZ315? ? ? ??140 ±290

2010 JH124? ? ? ??136.55 ±0.14

(523797) 2016 NM56? ?136.46 ±0.01

2015 TH367? ? ? ? 140 ±120

2015 VL168? ? ? ? 136.0 ±2.2

2010 PU75? ? ? ? ? 135.38 ±0.01

2003 QY91? ? ? ? ??100 ±98000

(523755) 2014 WZ508? 132.99 ±0.01

2016 EJ203? ? ? ??132.23 ±0.02

旅行者二號(hào)距地距離? 133.24

1999 RZ214? ? ? ? 131.96 ±0.13

2000 CP105? ? ? ??100 ±73000

2015 VQ167? ? ? ? 131.49 ±0.47

1999 DG8? ? ? ? ? ??100 ±4000000

2013 BN27? ? ? ? ? 131 ±21

(15874) 1996 TL66? ? ? ???130.17 ±0.01

2014 XX40? ? ? ? ? 130.07 ±0.03

2017 MZ4? ? ? ? ? ?129.23 ±0.02

(523794) 2015 RR245? ? 128.62 ±0.03

2015 TJ367? ? ? ? 128 ±16

2006 HV122? ? ? ?127.61 ±0.17

2013 OR11? ? ?? ??127.57 ±0.01

2003 UA414? ? ? ?126.94 ±0.01

先驅(qū)者10號(hào)距地距離? 126.8(舊)

2014 WM510? ? ?125.27 ±0.10

2015 KU174? ? ???125.11 ±0.04

(523777) 2014 YF50? ?????125.10 ±0.01

2014 SY349? ? ? ?125 ±79

2001 FK194? ? ? ?100 ±10000

(523733) 2014 PR70? ? ? ?124.06 ±0.01

2014 SZ349? ? ? ?124 ±52

2005 NU125? ? ??122.94 ±0.02

2015 KZ173? ? ? 122.87 ±0.09

2014 DQ143? ? ??122.74 ±0.03

2010 GW64? ? ? ?122.73 ±0.19

2013 SE99? ? ? ? ?122.5 ±2.5

2013 JR64? ? ? ? ?122.54 ±0.04

2005 OE? ? ? ? ? ???122.41 ±0.10

2012 HD2? ? ? ? ? 122.21 ±0.02

(523767) 2014 WH510? ??121.42 ±0.01

2015 RL278? ? ? ?120.94 ±0.06

2004 TF282? ? ? ?120.43 ±0.02

2015 VS167? ? ? ?120.42 ±0.04

2001 KZ76? ? ? ? ?100 ±110000

2000 SQ331? ? ? ?100 ±78000

2010 JO179? ? ? ?119.04 ±0.03

2014 XQ40? ? ? ? ?118.80 ±0.01

2003 LA7? ? ? ? ? ? 118.53 ±0.28

2011 UW412?? ? ?117.73 ±0.56

2014 WN510? ? ?117.55 ±0.05

2012 BZ154? ? ? ?117.37 ±0.07

2014 OO394? ? ? 117 ±70

2017 OX68? ? ? ???116.29 ±0.01

2013 QQ95? ? ? ? ?116.10 ±0.12

2000 PF30? ? ? ? ??116.00 ±0.16

2013 JV64? ? ? ? ??116.0 ±1.7

2014 SO350? ? ???115.64 ±0.14

2000 PH30? ? ? ? ?115.23 ±0.12

2004 VM131? ? ??114.92 ±0.05

2003 FH129? ? ? ?114.67 ±0.10

(451657) 2012 WD36? ???114.32 ±0.08

2015 FQ345? ? ???114.06 ±0.04

2005 PT21? ? ? ? ?114.04 ±0.80

2015 VP166? ? ???114.02 ±0.13

(127546) 2002 XU93? ? ? 113.59 ±0.04

2015 VO166? ? ???112.82 ±0.62

2015 TN178? ? ? ?111.64 ±0.01

2011 UP411? ? ? ?111.63 ±0.05

2015 DA225? ? ? ?111.05 ±0.47

2009 KN30? ? ? ? ?110.82 ±0.06

2015 RK258? ? ? ?111 ±14

2015 RZ278? ? ? ?110.69 ±0.07

2012 BX154? ? ? ?110.30 ±0.08

2011 UJ413? ? ? ?110.16 ±0.03

2015 RB278? ? ???109.35 ±0.28

2016 SW50? ? ? ??109.30 ±0.61

2015 BZ517? ? ? ?110 ±150

2007 LJ38? ? ? ? ??108.70 ±0.06

2012 UR177? ? ???108.68 ±0.06

2015 VA168? ? ? ?108.67 ±0.06

2015 KO174? ? ???108.61 ±0.03

471143 Dziewanna? ? ? ? ? ?108.54 ±0.02

229762 G?kún∥?hòmdímà?108.28 ±0.01

2014 UV224? ? ? ?108.26 ±0.04

2011 YN79? ? ? ???108.04 ±0.04

2005 GX206? ? ???107.71 ±0.01

2007 TA418? ? ? ?107.46 ±0.08

2014 UV229? ? ? ?107.40 ±0.03

2012 DY98? ? ? ? ? 107.22 ±0.02

(160148) 2001 KV76? ? ? ? 107.11 ±0.18

2013 AR183? ? ? ? 107.09 ±0.03

2003 OS33? ? ? ? ? 106 ±72

2015 VR167? ? ? ? 106.19 ±0.28

(65407) 2002 RP120? ? ? ??105.99 ±0.01

(126619) 2002 CX154? ? ??105.83 ±0.10

2007 RM314? ? ???105.43 ±0.06

(145480) 2005 TB190? ? ? 104.90 ±0.01

2015 GC56? ? ? ? ? 104.69 ±0.04

先驅(qū)者11號(hào)距地距離? ? ? ?? 104.4(舊)

(523722) 2014 LV28? ? ? ? ?104.12 ±0.01

(523680) 2013 YJ151? ? ? ?103.84 ±0.01

2014 FC69? ? ? ? ? 104 ±16

(471272) 2011 FY9? ? ? ? ? ?103.64 ±0.02

(500876) 2013 JD64? ? ? ???103.63 ±0.04

2006 HX122? ? ? ? 104 ±8

2000 AB229? ? ? ? 103.47 ±0.42

2015 RH279? ? ? ? 103.30 ±0.16

2001 OM109? ? ? ?103.17 ±0.27

2014 WJ510? ? ? ??102.90 ±0.01

(523770) 2014 XO40? ? ? ? ? 102.64 ±0.01

2014 SD350? ? ? ? 102 ±98

2001 OT108? ? ? ??100 ±74000

2015 KF172? ? ? ? ?101 ±12

225088 Gonggong? ? ? ? ? ? ? 101.17 ±0.01

2015 VE168? ? ? ? ?101.13 ±0.05

2014 FC72? ? ? ? ? ?101.00 ±0.01

2015 DX224? ? ? ???100.86 ±0.03

2012 EE18? ? ? ? ? ? 100.82 ±0.04

2007 TR436? ? ? ???100 ±6200

2015 RA279? ? ? ???100.36 ±0.51

2005 LC54? ? ? ? ? ??100.18 ±0.13

2014 QC442? ? ? ? ?99.9 ±1.9

2016 PO66? ? ? ? ???100 ±2800

2001 FN194? ? ? ? ?100 ±72000

2011 UQ412? ? ? ? ?98.80 ±0.03

2014 UA225? ? ? ???98.80 ±0.02

2017 YG5? ? ? ? ? ? ? 99 ±25

2000 YY1? ? ? ? ? ? ??98 ±73

2006 HO122? ? ? ??100 ±170

2013 UE15? ? ? ? ? ?97.74 ±0.01

(523652) 2011? ?? LZ28?97.57 ±0.01

(136199) Eris? ? ? ?97.47 ±0.01

2003 QK91? ? ? ? ? ?96.98 ±0.06

2004 VH131? ? ? ??96.96 ±0.08

2000 SS331? ?? ???100 ±53000

2000 QK226? ? ? ? 100 ±8800

2014 OP394? ? ? ? 96.52 ±0.02

2014 FZ71? ? ? ? ? ?96.49 ±0.50

2006 QH181? ? ? ? 96.36 ±0.63

2009 DJ143? ? ? ? ?96.22 ±0.02

2004 VG131? ? ? ? ?95.53 ±0.11

2015 VG168? ? ? ? 95.49 ±0.19

(470599) 2008? ? OG19?95.39 ±0.01

(480017) 2014 QB442? ? ???95.32 ±0.01

(523800) 2017 KZ31? ? ? ? ??95.23 ±0.01

2013 UR15? ? ? ? ??95.08 ±0.03

2001 FJ194? ? ? ? 100 ±5300

2014 HC200? ? ???94.88 ±0.03

(523639) 2010 RE64? ? ? ? ?94.46 ±0.01

2000 PS30? ? ? ? ?100 ±17000

2006 QG181? ? ???93.79 ±0.08

2016 CO264? ? ???93.77 ±0.00

2009 DD47? ? ? ? ??94 ±18

(136120) 2003 LG7? ? ? ? ? ?93.56 ±0.11

(523753) 2014 WV508? ? ?93.33 ±0.01

2014 ON394? ? ? ?93.01 ±0.04

2014 QR441? ? ? ?92.98 ±0.30

2015 GZ55? ? ? ? ?92.93 ±0.09

2006 QJ181? ? ???92.83 ±0.01

2015 GD56? ? ? ???92.66 ±0.11

2011 US411? ? ? ?92.63 ±0.03

2013 RO98? ? ? ? ?90 ±250

2015 VN166? ? ???92.40 ±0.08

2014 WL510? ? ???91.91 ±0.06

2004 HQ79? ? ? ? ?91.89 ±0.04

2015 KY173? ? ???91.82 ±0.14

2014 FX71? ? ? ? ??91.60 ±0.54

(523787) 2015 DV224? ? ? ?91.38 ±0.01

2015 BB519? ? ? ?91.27 ±0.05

2001 KG77? ? ? ? ?90.97 ±0.13

2010 XE91? ? ? ? ?90.94 ±0.02

1998 XY95? ? ? ? ?90.91 ±0.01

2009 KX36? ? ? ? ?90 ±190

2015 RZ277? ? ? ?90.30 ±0.49

2015 VM166? ? ? 90.15 ±0.05

2015 UH87? ? ? ? ?90 ±22

冥王星遠(yuǎn)日點(diǎn)? ? ?49

新視野號(hào)距地距離? ? ? 47.8(舊)

海王星遠(yuǎn)日點(diǎn)? ? ?30.44

詞條原文

This is a?list of Solar System objects by greatest aphelion?or the greatest distance from the Sun that the orbit takes it. For the purposes of this list, it is implied that the object is orbiting the Sun?in a two-body solution?without the influence of the planets or passing stars. The aphelion can change significantly due to the gravitational influence of planets and other stars. Most of these objects are comets on a calculated path and may not be directly observable.[1]?For instance, comet?Hale-Bopp?was last seen in 2013 at?magnitude?24[2]?and continues to fade, making it invisible to all but the most powerful telescopes.

The maximum extent of the region in which the Sun's?gravitational field?is dominant, the?Hill sphere, may extend to 230,000 astronomical units (3.6 light-years) as calculated in the 1960s.[3]?But any comet currently more than about 150,000?AU?(2?ly) from the Sun can be considered lost to the?interstellar medium. The nearest known star is Proxima Centauri at 271,000 AU which is 4.22 light years,[4]?followed by Alpha Centauri at about 4.35 light years away according to NASA.[4]

Comets are thought to orbit the Sun at great distances, but then be perturbed by passing stars and the?galactic tides.[5]?As they come into or leave the inner Solar System they may have their orbit changed by the planets, or alternatively be ejected from the Solar System.[5]?It is also possible they may collide with the Sun or a planet.[5]

As many of the objects listed below have some of the most extreme orbits of any objects in the Solar System, describing their orbit precisely can be particularly difficult. For most objects in the Solar System, a heliocentric reference frame (relative to the gravitational center of the Sun) is sufficient to explain their orbits. However, as the orbits of objects become closer to the Solar System's escape velocity, with long orbital periods on the order of hundreds or thousands of years, a different reference frame is required to describe their orbit: a barycentric reference frame. A barycentric reference frame measures the asteroid's orbit relative to the gravitational center of the entire Solar System, rather than just the Sun. Mostly due to the influence of the outer gas giants, the Solar System barycenter varies by up to twice the radius of the Sun.

This difference in position can lead to significant changes in the orbits of long-period comets and distant asteroids. Many comets have hyperbolic (unbound) orbits in a heliocentric reference frame, but in a barycentric reference frame have much more firmly bound orbits, with only a Small handful remaining truly hyperbolic.

Eccentricity and VinfEdit

The?orbital parameter?used to describe how non-circular an object's orbit is, is?eccentricity(e). An object with an e of 0 has a perfectly circular orbit, with its?perihelion distancebeing just as close to the Sun as its aphelion distance. An object with an?e?of between 0 and 1 will have an elliptical orbit, with, for instance, an object with an?e?of 0.5 having a perihelion twice as close to the Sun as its aphelion. As an object's?e?approaches 1, its orbit will be more and more elongated before, and at?e=1, the object's orbit?will be parabolicand unbound to the Solar System (i.e. not returning for another orbit). An?e?greater than 1?will be hyperbolic?and still be unbound to the Solar System.

Although it describes how "unbound" an object's orbit is, eccentricity does not necessarily reflect how high an incoming velocity said object had before entering the Solar System (a parameter known as Vinfinity, or Vinf). An object would need a much lower velocity to be unbound from the Solar System if it didn't have an especially nearby perihelion, but an object with a perihelion inside the orbit of Mercury would need a much higher excess velocity to escape the Solar System. A clear example of this is the eccentricities of the two known?Interstellar objects?as of October 2019,?1I/'Oumuamua. and?2I/Borisov. 'Oumuamua had an incoming Vinf?of 26.5 kilometres per second (59,000?mph), but due to its low perihelion distance of only 0.255?au, it had an eccentricity of 1.200. However, Borisov's Vinfwas only slightly higher, at 32.3?km/s (72,000?mph), but due to its higher perihelion distance of ~2.003 au, its eccentricity was a comparably higher 3.340. In practice, no object originating from the Solar System should have an incoming heliocentric eccentricity much higher than 1, and should rarely have an incoming barycentric eccentricity of above 1, as that would imply that the object had originated from an indefinitely far distance from the Sun.

Orbital epochsEdit

Due to having the most eccentric orbits of any Solar System body, a comet's orbit typically intersects one or more of the planets in the Solar System. As a result, the orbit of a comet is frequently?perturbed?significantly, even over the course of a single pass through the inner Solar System. Due to the changing orbit, it's necessary to provide a calculation of the orbit of the comet (or similarly orbiting body) both before and after entering the inner Solar System. A standard epoch of 1600 is given for the incoming orbits, and 2400 for ouTGoing orbits. For example,?Comet ISON?was ~312 au from the Sun in 1600, and its remnants will be ~431 au from the Sun in 2400, both well outside of any significant gravitational influence from the planets.

Examples of comets with a more well-determined orbit. Comets are extremely Small relative to other bodies and hard to observe once they stop ouTGassing (see?Coma (cometary)). Because they are typically discovered close to the Sun, it will take some time even thousands of years for them to actually travel out to great distances. The?Whipple?proposal might be able to detect Oort cloud objects at great distances, but probably not a particular object.

A large number of?trans-Neptunian objects(TNOs) –?minor planets?orbiting beyond the orbit of?Neptune?– have been discovered in recent years. Many TNOs have orbits with an aphelion (farthest distance to the Sun) far beyond Neptune's orbit at 30.1?AU. Some of these TNOs with an extreme aphelion are?detached objects?such as?2010 GB174, which always reside in the outermost region of the Solar System, while for other TNOs, the extreme aphelion is due to an exceptionally high?eccentricity?such as for?2005 VX3, which orbits the Sun at a distance between 4.1 (closer than Jupiter) and 2200?AU (70 times farther from the Sun than Neptune). The following is a list of TNOs with the largest aphelion in descending order.[14][15]

參考

1. ^?a?b?JPL Small-Body Database Search Engine: Q > 20000 (au)
2. ^?"C/1995 O1 (Hale-Bopp)". Minor Planet Center. Retrieved?14 March?2018.
3. ^?Chebotarev, G.A. (1964), "Gravitational Spheres of the Major Planets, Moon and Sun",?Soviet Astronomy,?7?(5): 618–622,?Bibcode:1964SvA.....7..618C
4. ^?a?b?NASA – Imagine the Universe: The Nearest Star
5. ^?a?b?c?Frequently Asked Questions About General Astronomy
6. ^?a?b?c?Furthest SSB
7. ^?Horizons?output.?"Barycentric Osculating Orbital Elements for Comet C/1975 V1-A (West)". Retrieved?2011-02-01.?(Solution using the Solar System?Barycenter. Select Ephemeris Type:Elements and Center:@0)
8. ^?Horizons?output.?"Barycentric Osculating Orbital Elements for Comet C/1999 F1 (Catalina)". Retrieved?2011-03-07.?(Solution using the Solar System?Barycenter?and?barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
9. ^?Horizons?output.?"Barycentric Osculating Orbital Elements for Comet C/2012 S4 (PANSTARRS)". Retrieved?2015-09-26.?(Solution using the Solar System?Barycenter?and?barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
10. ^?Horizons?output (2011-01-30).?"Barycentric Osculating Orbital Elements for Comet Hyakutake (C/1996 B2)". Retrieved?2011-01-30.?(Horizons)
11. ^?Horizons?output.?"Barycentric Osculating Orbital Elements for Comet C/1910 A1 (Great January comet)". Retrieved?2011-02-07.?(Solution using the Solar System?Barycenter?and?barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
12. ^?Horizons?output.?"Barycentric Osculating Orbital Elements for Comet C/1992 J1 (Spacewatch)". Retrieved?7 October?2012.?(Solution using the Solar System?Barycenter?and?barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
13. ^?Horizons?output.?"Barycentric Osculating Orbital Elements for Comet Lulin (C/2007 N3)". Retrieved?2011-01-30.?(Solution using the Solar System?Barycenter. Select Ephemeris Type:Elements and Center:@0)
14. ^?a?b?c?JPL asteroids greater than 200 AU aphelion (Q)
15. ^?a?b?JPL asteroids aphelion greater than 800 AU
16. ^?Marc W. Buie.?"Orbit Fit and Astrometric record for 308933"?(2010-09-17 using 64 of 65 observations over 5.01 years). SwRI (Space Science Department). Retrieved?2008-09-05.
17. ^?Becker, J. C; et?al. (14 May 2018). "Discovery and Dynamical Analysis of an Extreme Trans-Neptunian Object with a High Orbital Inclination".?The Astronomical Journal.?156?(2): 81.?arXiv:1805.05355.?doi:10.3847/1538-3881/aad042.?S2CID?55163842.
18. ^?Marc W. Buie?(2007-11-08).?"Orbit Fit and Astrometric record for 04VN112". SwRI (Space Science Department). Archived from?the original?on 2010-08-18. Retrieved?2008-07-17.
19. ^?"JPL Small-Body Database Browser: (2004 VN112)". Retrieved?2011-05-20.
20. ^?JPL database down to 100 AU aphelion minor planets

更新截止至2023.2.12