Eng katta afeliyga ega bo‘lgan obyektlar bo‘yicha quyosh tizimidagi jismlar ro‘yxati

Bu ro‘yxat Quyosh tizimi obyektlarining eng katta afeliyiga ega bo‘lgan obyektlar ro‘yxatidir. Agar Quyosh va obyekt olamdagi yagona jismlar bo‘lsa, orbitasi uni Quyoshdan eng uzoqqa olib borishi mumkin bo‘lgan masofa. Bu obyektlar faqat Quyoshni ikki jismli tizimda aylanayotganini anglatadi, yaʼni planetalar, o‘tib ketayotgan yulduzlar yoki galaktikaning ta’siri hisobga olinmayotgani anglatadi. Afeliy, sayyoralar va boshqa yulduzlarning gravitatsion ta’siri natijasida sezilarli darajada o‘zgarishi mumkin. Ushbu obyektlarning ko‘pi hisoblangan orbitada harakatlanayotgan kometalar bo‘lib, ular bevosita kuzatilmasligi mumkin. Misol uchun, Hale-Bopp kometasi 2013-yilda magnituda 24 da oxirgi marta kuzatildi va hali ham so‘nishni davom ettirmoqda, bu esa uni faqat eng kuchli teleskoplar yordamida ko‘rish imkonini beradi.

Quyoshning gravitatsion maydoni eng kuchli ta’sir qiladigan hudud, ya'ni Hill sharlari, 1960-yillarda olib borilgan hisob-kitoblarga ko‘ra, 230,000 AU (3,6 yy)gacha kengayishi mumkin. Ayrim kometalar hozirda Quyoshdan 150,000 AU (2 yy)dan uzoqlashgan bo‘lsa, ular yulduzlararo makonga yo‘qolgan deb hisoblanishi mumkin. Ma’lum bo‘lgan eng yaqin yulduz — Proxima Centauri, uning masofasi 269,000 AU (4,25 yy)NASA – Imagine the Universe: The Nearest Starni tashkil etadi, undan keyin esa Alpha Centauri joylashgan bo‘lib, uning masofasi taxminan 4,35 yorug‘lik yili.

Oort bulutidagi kometalarning orbitasi Quyosh atrofida katta masofalarga cho‘ziladi, ammo o‘tib ketayotgan yulduzlar va galaktik to‘lqinlar ularni ta’sir qilib, orbitasini o‘zgartirishi mumkin.Frequently Asked Questions About General Astronomy  Ichki Quyosh tizimiga kirib yoki undan chiqib ketayotganda, ular sayyoralar ta’sirida orbitasini o‘zgartirishi yoki Quyosh tizimidan chiqarilishi mumkin.Shuningdek, ular Quyosh yoki biror sayyora bilan to‘qnashishi ham mumkin.

S/2021 N 1 (Neptunning eng uzoqdagi yoʻldoshi) Neptun atrofida 27 yildan koʻproq vaqt ichida aylanadi, kometalar esa Quyosh atrofida aylanib yetishishi uchun 30 million yillargacha vaqt olishi mumkin, va Quyosh Galaktika atrofida 230 million yil ichida (galaktik yil) aylanib chiqadi.

+Yoʻldoshlarning orbital davri yoki markaziy qismining orbital davri Yoʻldosh Orbital davr(years) Markaziy qism Markaziy qismni orbital davrining foizi S/2021 N 1  27.4  Neptun  16.6% Oort buluti kometasi 30 million  Quyosh  13% Quyosh  230 million  Somon yoʻli  N/A

 Sharh 
Barytsentrik va Geliosentrik orbitalar

Ko‘plab quyidagi ro‘yxatda keltirilgan obyektlar Quyosh tizimidagi eng g‘ayrioddiy orbitalarga ega bo‘lib, ularning harakati vaqtga bogʻliq boʻlganligi uchun ularning orbitasini aniq tasvirlash qiyin. Ko‘plab obyektlar uchun heliotsentrik maʼlumotlar bazasi (Quyoshning gravitatsion markaziga nisbatan) ularning orbitasini tushunish uchun yetarli hisoblanadi. Biroq, obyektlarning orbitalari Quyosh tizimining chiqish tezligiga yaqinlashganida, yaʼni yuzlab yoki minglab yillar davom etadigan uzoq orbitalar mavjud bo‘lsa, ularning orbitasini tasvirlash uchun boshqacha maʼlumotlar bazasi talab qilinadi: barysentrik maʼlumotlar bazasi. Barysentrik maʼlumotlar bazasi asteroiddan uning orbita markazini faqat Quyoshdan emas, balki butun Quyosh tizimining gravitatsion markaziga nisbatan o‘lchaydi. Asosan tashqi gaz gigantlarining taʼsiri tufayli, Quyosh tizimi barysentrining joylashuvi quyosh radiusining ikki baravarigacha o‘zgarishi mumkin.

Bu farq uzoq davrli kometalar va uzoq masofadagi asteroidlarning orbitalarida sezilarli o‘zgarishlarga olib kelishi mumkin. Ko‘plab kometalar heliotsentrik maʼlumotlar bazasida giperkubik (bog‘lanmagan) orbitaga ega bo‘lsa-da, barysentrik maʼlumotlar bazasida ularning orbitalari ancha mustahkam bog‘langan bo‘ladi, faqat bir nechta kometalar haqiqatan ham giperkubik orbitada qoladi.

Orbitaning aylanadan og‘ishi(Essentriklik) va Vinf
Orbita parametri, obyektning orbitasi necha darajada doiraviy emasligini tasvirlash uchun ishlatiladigan parametr – essentriklik (e). e=0 bo‘lgan obyektning orbita mukammal doiraviy bo‘lib, uning perihelion masofasi afelion masofasi bilan bir xil bo‘ladi, yaʼni, Quyoshga eng yaqin nuqtasi ham, eng uzoq nuqtasi ham bir xil masofada joylashadi. e qiymati 0 va 1 orasida bo‘lgan obyekt elliptik orbitaga ega bo‘ladi. Masalan, e=0.5 bo‘lgan obyektning perihelion masofasi afelion masofasidan ikki barobar yaqin bo‘ladi. Agar obyektning e qiymati 1 ga yaqinlashsa, uning orbita shakli tobora cho‘zilib boradi va e=1 bo‘lganida obyektning orbitasi parabolik bo‘lib, Quyosh tizimiga bog‘lanmagan holatga keladi (yaʼni, u boshqa orbitaga qaytmaydi). Agar e 1 dan katta bo‘lsa, orbita giperkubik bo‘ladi va u ham Quyosh tizimiga bog‘lanmagan bo‘ladi.

Comets with greatest aphelion (2 body heliocentric)


 Object HeliocentricAphelion (Q)(Sun)Perihelion epoch BarycentricAphelion (AD)(Sun+Jupiter)epoch 2200 BarycentricAphelionepoch 1800 C/2004 R2 (ASAS)    13000 AUBarycentric solution for 2004 R2  4000 AU C/2015 O1 (PANSTARRS)    15000 AUBarycentric solution for 2015 O1  60000 AU C/2012 S4 (PANSTARRS)    5700 AUBarycentric solution for 2012 S4  8400 AU C/2012 CH17 (MOSS)    7283 AU  26000 AU C/2008 C1 (Chen-Gao)    3822 AU  520 AU C/1992 J1 (Spacewatch)    3700 AU  75000 AU C/2007 N3 (Lulin)    2419 AU  64000 AU C/2017 T2 (PANSTARRS)    2975 AU  84000 AU C/1937 N1 (Finsler)    7121 AU  16000 AU C/1972 X1 (Araya)    5630 AU  4200 AU C/2014 R3 (PANSTARRS)    12841 AU  19000 AU C/2015 O1 (PANSTARRS)    21753 AU  52000 AU C/2001 C1 (LINEAR)    ejection  98000 AU C/2002 J4 (NEAT)    ejection  59000 AU C/1958 D1 (Burnham)    1110 AU  7800 AU C/1986 V1 (Sorrells)    8946 AU  5400 AU C/2005 G1 (LINEAR)    40572 AU  110000 AU C/2006 W3 (Christensen)    8212 AU  5300 AU C/2009 W2 (Boattini)    3847 AU  4200 AU C/2005 L3 (McNaught)    6851 AU  33000 AU C/2004 YJ35 (LINEAR)    2480 AU  75000 AU C/2003 H3 (NEAT)    ejection  4900 AU C/2010 L3 (Catalina)    21094 AU  12000 AU C/1902 R1 (Perrine)    2306 AU  74000 AU C/1889 G1 (Barnard)    1575 AU  2100 AU C/2007 VO53 (Spacewatch)    16835 AU  22000 AU

 Distant comets with long observation arcs and/or barycentric 

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.

Comet West 70,000 AU (Solution using the Solar System Barycenter. Select Ephemeris Type:Elements and Center:@0) (1.1 light-years)
C/1999 F1 (Catalina) 66,600 AU (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0) (1.05 light-years)
C/2012 S4 (PANSTARRS) 5700 AU (barycentric) (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
Comet Hyakutake (C/1996 B2) 3410 AU (Horizons)
C/1910 A1 (Great January comet) about 2974 AU (barycentric) (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
C/1992 J1 (Spacewatch) 3650 AU (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
C/2007 N3 (Lulin) 2400 AU (Solution using the Solar System Barycenter. Select Ephemeris Type:Elements and Center:@0)

 Minor planets 

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 that take them far beyond Pluto's aphelion of 49.3 AU. Some of these TNOs with an extreme aphelion are detached objects such as , 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 , 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 minor planets with the largest aphelion in descending order.

 Minor planets with a heliocentric aphelion greater than 400 AU 

ObjectAphelion (AU)Absolute Magnitude (H)RefA/2020 M4  29020.06 ±420  14.01 ±0.28    20162.05 ±6000  14.08  A/2024 D13875.88 ±245611.45 ±0.52  3559.58 ±220  6.19  541132 Leleākūhonua  2713.25 ±360  5.57 ±0.13   2419.67 ±320  14.21 ±0.33   2314.82 ±51  6.74±0.12    2261.12 ±2.4  10.88  2115.35 ±69012.80±0.43  2108.10 ±450  6.35 ±0.14   2062.42 ±1.6  7.94  A/2022 B3  1957.25 ±11  16.56 ±0.76   1877.78 ±1.3  7.12   1718.93 ±50  6.84   1717.16 ±300  14.10   1418.77 ±320  6.72 ±0.24   A/2019 G2  1397.41 ±1.7  16.31 ±0.55  A/2021 E4 1388.62 ±1.2  14.26 ±0.45  A/2018 W3 1341.59 ±10  10.70 ±0.29   1326.78 ±0.76  9.10   1295.34 ±51  15.30   1241.82 ±7.2  8.20   1118.81 ±0.64  6.47  1052.34 ±0.519.92 ±0.37 1032.63 ±0.62  8.16 ±0.35   1015.61 ±9.9  11.74 ±0.79   1008.19 ±2.7  6.23 ±0.22  90377 Sedna  1006.90±2.7  1.50   990.67 ±0.62  14.55 ±0.37  986.20 ±0.3710.56 ±0.43 933.55 ±2.5  4.34   888.63 ±8.1  6.20    859.76 ±4.7  8.38 ±0.52   853.72 ±1.7  14.50 ±0.26   846.98 ±0.49  9.30 ±0.42   828.61 ±0.46  10.30   816.45 ±11  14.90 ±0.47   776.26 ±30  8.70   773.46 ±4.1  7.06 ±0.32   767.45 ±0.085  9.74   762.63 ±0.1  10.30   753.12 ±16  8.22 ±0.31    732.44 ±7.7  15.30    731.06±7.6  6.70 ±0.33    704.80 ±2.0  7.86 ±0.44    689.35±0.57  12.23 ±0.41  684.64 ±2700008.52 ±0.10A/2020 H9  680.42 ±1.1  17.70 ±0.34   663.36 ±2.3  6.46    653.9 ±0.91  7.13 ±0.33   650.82 ±140  21.20    648.32 ±0.27  8.07 ±0.44   637.57 ±0.22  12.04 ±0.18    630.26 ±14  6.74   601.90 ±2.4  6.46   579.67 ±0.35  13.10   570.60 ±0.17  10.55    560.73 ±1.2  7.26 ±0.27   554.67 ±4.5  8.50   552.06 ±0.56  13.90   545.94 ±34  7.76 ±0.05  543.67 ±0.159.95 519.49 ±2.7  7.20   511.63 ±16  17.90  505.11 ±2.38.78 ±0.11  484.56 ±1.2  7.81 ±0.36    480.63 ±0.028  11.06 ±0.44    467.17 ±0.99  4.09    464.64±0.39  7.50 ±0.41    449.66 ±9.0  8.90  A/2021 E2  430.46 ±8.3  17.90 ±0.44  411.63 ±0.327.53 ±0.24400.29 ±1.26.14

Greatest barycentric aphelion
The following asteroids have an incoming barycentric aphelion of at least 1000 AU.
namediameter (km) (assumed)perihelion (AU)Barycentric aphelion (AU) (1800)Barycentric aphelion (AU) (2200)Change (%)A/2020 M4  5.2  5.95  5580  4500  -24  206.8  36.33  3071  3060  -0.36  3.0  2.691  2320  1190  -49  5.2  4.106  2140  1700  -21541132 Leleākūhonua  272.6  65.08  2280  2280  0A/2022 B3  1.9  3.708  2100  2540  +21  5.2  4.456  2040  2840  +28  130.5  14.57  2000  2050  +2.4  23.7  8.355  1850  1920  +3.6  94.5  24.14  1540  1560  +1.3  156.8  50.03  1410  1410  0  78.6  40.50  1320  1320  0  29.9  7.927  1260  827  -34  3.6  2.677  1190  852  -28  78.6  23.52  1130  1120  -0.9  49.6  20.73  1120  1070  -4.5

 Comparison 

 See also 
 List of trans-Neptunian objects (numbered minor planets only)
 List of unnumbered trans-Neptunian objects
 List of artificial objects leaving the Solar System
 List of Solar System objects most distant from the Sun (then-year distance from the Sun)
 List of nearest stars and brown dwarfs
 List of the most distant astronomical objects
About comets
 List of hyperbolic comets
 List of comets with no meaningful orbit
 List of near-parabolic comets
 List of periodic comets
 List of numbered comets
 Interstellar object
Objects of interest
 1996 PW
 C/2015 ER61
 C/1980 E1
Others





 References 


 External links 
 A distant planet may lurk far beyond Neptune
 Mysterious Planet X May Really Lurk Undiscovered in Our Solar System

Aphelion