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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, planetalar 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.[1] Misol uchun, Hale-Bopp kometasi 2013-yilda magnituda 24[2] da oxirgi marta kuzatildi va hali ham so‘nishni davom ettirmoqda, bu esa uni faqat eng kuchli teleskoplar yordamida ko‘rish imkonini beradi.

The orbit of Sedna lies well beyond these objects, and extends many times their distances from the Sun
The orbit of Sedna (red) set against the orbits of outer Solar System objects (Pluto's orbit is purple).

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.[3] 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)[4]ni tashkil etadi, undan keyin esa Alpha Centauri joylashgan bo‘lib, uning masofasi taxminan 4,35 yorug‘lik yili.[4]

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.[5] Ichki Quyosh tizimiga kirib yoki undan chiqib ketayotganda, ular sayyoralar ta’sirida orbitasini o‘zgartirishi yoki Quyosh tizimidan chiqarilishi mumkin.[5]Shuningdek, ular Quyosh yoki biror sayyora bilan to‘qnashishi ham mumkin.[5]

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

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Barytsentrik va Geliosentrik orbitalar

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Quyosh tizimi barytsentrining Quyosh atrofidagi harakati.

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

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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)

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C/1910 A1 during its 1910 close approach
 
Proxima Centauri is 271,000 AU or 4.25 light years away

Andoza:Sticky header

Object Heliocentric[1]
Aphelion (Q)
(Sun)
Perihelion epoch 		Barycentric
Aphelion (AD)
(Sun+Jupiter)
epoch 2200 		Barycentric
Aphelion
epoch 1800
C/2004 R2 (ASAS) 3,238,164 AU (51 ly) 13000 AU[6] 4000 AU
C/2015 O1 (PANSTARRS) 1,302,400 AU (21 ly) 15000 AU[7] 60000 AU
C/2012 S4 (PANSTARRS) 504,443 AU (8.0 ly) 5700 AU[8] 8400 AU
C/2012 CH17 (MOSS) 279,825 AU (4.4 ly) 7283 AU 26000 AU
C/2008 C1 (Chen-Gao) 203,253 AU (3.2 ly) 3822 AU 520 AU
C/1992 J1 (Spacewatch) 226,867 AU (3.6 ly) 3700 AU 75000 AU
C/2007 N3 (Lulin) 144,828 AU (2.3 ly) 2419 AU 64000 AU
C/2017 T2 (PANSTARRS) 117,212 AU (1.9 ly) 2975 AU 84000 AU
C/1937 N1 (Finsler) 115,031 AU (1.8 ly) 7121 AU 16000 AU
C/1972 X1 (Araya) 108,011 AU (1.7 ly) 5630 AU 4200 AU
C/2014 R3 (PANSTARRS) 80,260 AU (1.3 ly) 12841 AU 19000 AU
C/2015 O1 (PANSTARRS) 77,092 AU (1.2 ly) 21753 AU 52000 AU
C/2001 C1 (LINEAR) 76,230 AU (1.2 ly) ejection 98000 AU
C/2002 J4 (NEAT) 57,793 AU (0.91 ly) ejection 59000 AU
C/1958 D1 (Burnham) 46,408 AU (0.73 ly) 1110 AU 7800 AU
C/1986 V1 (Sorrells) 37,825 AU (0.60 ly) 8946 AU 5400 AU
C/2005 G1 (LINEAR) 37,498 AU (0.59 ly) 40572 AU 110000 AU
C/2006 W3 (Christensen) 35,975 AU (0.57 ly) 8212 AU 5300 AU
C/2009 W2 (Boattini) 31,059 AU (0.49 ly) 3847 AU 4200 AU
C/2005 L3 (McNaught) 26,779 AU (0.42 ly) 6851 AU 33000 AU
C/2004 YJ35 (LINEAR) 26,433 AU (0.42 ly) 2480 AU 75000 AU
C/2003 H3 (NEAT) 26,340 AU (0.42 ly) ejection 4900 AU
C/2010 L3 (Catalina) 25,609 AU (0.40 ly) 21094 AU 12000 AU
C/1902 R1 (Perrine) 25,066 AU (0.40 ly) 2306 AU 74000 AU
C/1889 G1 (Barnard) 24,784 AU (0.39 ly) 1575 AU 2100 AU
C/2007 VO53 (Spacewatch) 24,383 AU (0.39 ly) 16835 AU 22000 AU

Distant comets with long observation arcs and/or barycentric

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Comet West in 1976

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.

Minor planets

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Yana qarang: List of trans-Neptunian objects va List of Solar System objects most distant from the Sun

Andoza:Bar graph

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 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 minor planets with the largest aphelion in descending order.[16]

Minor planets with a heliocentric aphelion greater than 400 AU

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Object Aphelion (AU) Absolute Magnitude (H) Ref
A/2020 M4 29020.06 ±420 14.01 ±0.28 Andoza:M+J
2010 LN135 20162.05 ±6000 14.08 Andoza:M+J
A/2024 D1 3875.88 ±2456 11.45 ±0.52 Andoza:M+J
2014 FE72 3559.58 ±220 6.19 Andoza:M+J
541132 Leleākūhonua 2713.25 ±360 5.57 ±0.13 Andoza:M+J
2017 MB7 2419.67 ±320 14.21 ±0.33 Andoza:M+J
2021 RR205 2314.82 ±51 6.74±0.12 Andoza:M+J
2013 BL76 2261.12 ±2.4 10.88 Andoza:M+J
A/2019 N2 2115.35 ±690 12.80±0.43 Andoza:M+J
2019 EU5 2108.10 ±450 6.35 ±0.14 Andoza:M+J
(308933) 2006 SQ372 2062.42 ±1.6 7.94 Andoza:M+J
A/2022 B3 1957.25 ±11 16.56 ±0.76 Andoza:M+J
(668643) 2012 DR30 1877.78 ±1.3 7.12 Andoza:M+J
2013 SY99 1718.93 ±50 6.84 Andoza:M+J
2005 VX3 1717.16 ±300 14.10 Andoza:M+J
2021 DK18 1418.77 ±320 6.72 ±0.24 Andoza:M+J
A/2019 G2 1397.41 ±1.7 16.31 ±0.55 Andoza:M+J
A/2021 E4 1388.62 ±1.2 14.26 ±0.45 Andoza:M+J
A/2018 W3 1341.59 ±10 10.70 ±0.29 Andoza:M+J
(87269) 2000 OO67 1326.78 ±0.76 9.10 Andoza:M+J
2002 RN109 1295.34 ±51 15.30 Andoza:M+J
2015 KG163 1241.82 ±7.2 8.20 Andoza:M+J
(523622) 2007 TG422 1118.81 ±0.64 6.47 Andoza:M+J
2015 SA57 1052.34 ±0.51 9.92 ±0.37 Andoza:M+J
2013 GW141 1032.63 ±0.62 8.16 ±0.35 Andoza:M+J
2012 KA51 1015.61 ±9.9 11.74 ±0.79 Andoza:M+J
2013 RA109 1008.19 ±2.7 6.23 ±0.22 Andoza:M+J
90377 Sedna (2003 VB12) 1006.90±2.7 1.50 Andoza:M+J
2020 QN6 990.67 ±0.62 14.55 ±0.37 Andoza:M+J
2014 GQ101 986.20 ±0.37 10.56 ±0.43 Andoza:M+J
2015 BP519 933.55 ±2.5 4.34 Andoza:M+J
2015 RX245 888.63 ±8.1 6.20 Andoza:M+J
2015 AD298 859.76 ±4.7 8.38 ±0.52 Andoza:M+J
2015 FK37 853.72 ±1.7 14.50 ±0.26 Andoza:M+J
2020 YR3 846.98 ±0.49 9.30 ±0.42 Andoza:M+J
2010 BK118 828.61 ±0.46 10.30 Andoza:M+J
2007 DA61 816.45 ±11 14.90 ±0.47 Andoza:M+J
2013 RF98 776.26 ±30 8.70 Andoza:M+J
2014 SX403 773.46 ±4.1 7.06 ±0.32 Andoza:M+J
(418993) 2009 MS9 767.45 ±0.085 9.74 Andoza:M+J
2013 AZ60 762.63 ±0.1 10.30 Andoza:M+J
2014 RK86 753.12 ±16 8.22 ±0.31 Andoza:M+J
2018 MP8 732.44 ±7.7 15.30 Andoza:M+J
2016 SD106 731.06±7.6 6.70 ±0.33 Andoza:M+J
2014 TU115 704.80 ±2.0 7.86 ±0.44 Andoza:M+J
2021 CP5 689.35±0.57 12.23 ±0.41 Andoza:M+J
2022 LO17 684.64 ±270000 8.52 ±0.10 Andoza:M+J
A/2020 H9 680.42 ±1.1 17.70 ±0.34 Andoza:M+J
474640 Alicanto 663.36 ±2.3 6.46 Andoza:M+J
2013 SL102 653.9 ±0.91 7.13 ±0.33 Andoza:M+J
2017 UR52 650.82 ±140 21.20 Andoza:M+J
(689335) 2013 FL28 648.32 ±0.27 8.07 ±0.44 Andoza:M+J
2021 PN72 637.57 ±0.22 12.04 ±0.18 Andoza:M+J
2010 GB174 630.26 ±14 6.74 Andoza:M+J
2014 SR349 601.90 ±2.4 6.46 Andoza:M+J
2011 OR17 579.67 ±0.35 13.10 Andoza:M+J
(336756) 2010 NV1 570.60 ±0.17 10.55 Andoza:M+J
2014 WB556 560.73 ±1.2 7.26 ±0.27 Andoza:M+J
2015 GT50 554.67 ±4.5 8.50 Andoza:M+J
1996 PW 552.06 ±0.56 13.90 Andoza:M+J
2018 VM35 545.94 ±34 7.76 ±0.05 Andoza:M+J
(523719) 2014 LM28 543.67 ±0.15 9.95 Andoza:M+J
2013 FT28 519.49 ±2.7 7.20 Andoza:M+J
2017 SN33 511.63 ±16 17.90 Andoza:M+J
2015 DM319 505.11 ±2.3 8.78 ±0.11 Andoza:M+J
2016 SA59 484.56 ±1.2 7.81 ±0.36 Andoza:M+J
(582301) 2015 RM306 480.63 ±0.028 11.06 ±0.44 Andoza:M+J
2012 VP113 467.17 ±0.99 4.09 Andoza:M+J
2016 SG58 464.64±0.39 7.50 ±0.41 Andoza:M+J
2015 RY245 449.66 ±9.0 8.90 Andoza:M+J
A/2021 E2 430.46 ±8.3 17.90 ±0.44 Andoza:M+J
2014 QW510 411.63 ±0.32 7.53 ±0.24 Andoza:M+J
(148209) 2000 CR105 400.29 ±1.2 6.14 Andoza:M+J

Greatest barycentric aphelion

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

name diameter (km) (assumed) perihelion (AU) Barycentric aphelion (AU) (1800) Barycentric aphelion (AU) (2200) Change (%)
A/2020 M4 5.2 5.95 5580 4500 -24
2014 FE72 206.8 36.33 3071 3060 -0.36
2002 RN109 3.0 2.691 2320 1190 -49
2005 VX3 5.2 4.106 2140 1700 -21
541132 Leleākūhonua 272.6 65.08 2280 2280 0
A/2022 B3 1.9 3.708 2100 2540 +21
2017 MB7 5.2 4.456 2040 2840 +28
(668643) 2012 DR30 130.5 14.57 2000 2050 +2.4
2013 BL76 23.7 8.355 1850 1920 +3.6
(308933) 2006 SQ372 94.5 24.14 1540 1560 +1.3
2013 SY99 156.8 50.03 1410 1410 0
2015 KG163 78.6 40.50 1320 1320 0
2013 AZ60 29.9 7.927 1260 827 -34
2007 DA61 3.6 2.677 1190 852 -28
2013 GW141 78.6 23.52 1130 1120 -0.9
(87269) 2000 OO67 49.6 20.73 1120 1070 -4.5

Comparison

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The orbit of Andoza:Dp, 2012 VP113, Leleākūhonua, and other very distant objects along with the predicted orbit of Planet Nine. The three sednoids (pink) along with the red-colored extreme trans-Neptunian object (eTNO) orbits are suspected to be aligned with the hypothetical Planet Nine while the blue-colored eTNO orbits are anti-aligned. The highly elongated orbits colored brown include centaurs and damocloids with large aphelion distances over 200 AU.

See also

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About comets
Objects of interest
Others

References

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  1. ↑ 1,0 1,1 JPL Small-Body Database Search Engine: Q > 20000 (au)
  2. ↑ „C/1995 O1 (Hale-Bopp)“. Minor Planet Center. Qaraldi: 2018-yil 14-mart.
  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. ↑ 4,0 4,1 NASA – Imagine the Universe: The Nearest Star
  5. ↑ 5,0 5,1 5,2 Frequently Asked Questions About General Astronomy
  6. ↑ Barycentric solution for 2004 R2
  7. ↑ Barycentric solution for 2015 O1
  8. ↑ Barycentric solution for 2012 S4
  9. ↑ Horizons output. „Barycentric Osculating Orbital Elements for Comet C/1975 V1-A (West)“. Qaraldi: 2011-yil 1-fevral. (Solution using the Solar System Barycenter. Select Ephemeris Type:Elements and Center:@0)
  10. ↑ Horizons output. „Barycentric Osculating Orbital Elements for Comet C/1999 F1 (Catalina)“. Qaraldi: 2011-yil 7-mart. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
  11. ↑ Horizons output. „Barycentric Osculating Orbital Elements for Comet C/2012 S4 (PANSTARRS)“. Qaraldi: 2015-yil 26-sentyabr. (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 Hyakutake (C/1996 B2)“ (2011-yil 30-yanvar). Qaraldi: 2011-yil 30-yanvar. (Horizons)
  13. ↑ Horizons output. „Barycentric Osculating Orbital Elements for Comet C/1910 A1 (Great January comet)“. Qaraldi: 2011-yil 7-fevral. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
  14. ↑ Horizons output. „Barycentric Osculating Orbital Elements for Comet C/1992 J1 (Spacewatch)“. Qaraldi: 2012-yil 7-oktyabr. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
  15. ↑ Horizons output. „Barycentric Osculating Orbital Elements for Comet Lulin (C/2007 N3)“. Qaraldi: 2011-yil 30-yanvar. (Solution using the Solar System Barycenter. Select Ephemeris Type:Elements and Center:@0)
  16. ↑ Manba xatosi: Invalid <ref> tag; no text was provided for refs named :0
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