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)ni 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. 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.

## 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 V<sub>inf</sub>
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)

### 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 (1.1 light-years)
*C/1999 F1 (Catalina) 66,600 AU (1.05 light-years)
*C/2012 S4 (PANSTARRS) 5700&nbsp;AU (barycentric)
*Comet Hyakutake (C/1996 B2) 3410 AU
*C/1910 A1 (Great January comet) about 2974 AU (barycentric)
*C/1992 J1 (Spacewatch) 3650&nbsp;AU
*C/2007 N3 (Lulin) 2400&nbsp;AU

## 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&nbsp;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&nbsp;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

}|| 552.06 ±0.56 || 13.90 || 
|-
||| 545.94 ±34 || 7.76 ±0.05 || 
|-
|
|543.67 ±0.15
|9.95
|
|-
||| 519.49 ±2.7 || 7.20 || 
|-
||| 511.63 ±16 || 17.90 || 
|-
|
|505.11 ±2.3
|8.78 ±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 ±0.32
|7.53 ±0.24
|
|-
|
|400.29 ±1.2
|6.14
|
|}

### Greatest barycentric aphelion
The following asteroids have an incoming barycentric aphelion of at least 1000 AU.

## 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