Английская Википедия:(458271) 2010 UM26 and 2010 RN221

Материал из Онлайн справочника
Перейти к навигацииПерейти к поиску

Шаблон:Short description

Шаблон:Use dmy dates Шаблон:Infobox planet

Шаблон:Mp and Шаблон:Mp are a pair of sub-kilometer-sized asteroids that have extremely similar orbits in the main asteroid belt. These two asteroids are thought to have dissociated from a binary system sometime in the 2000s, which would make them one of the youngest asteroid pairs known. The largest member of this pair, Шаблон:Mp (or simply Шаблон:Mp), is about Шаблон:Cvt in diameter and was discovered on 10 November 2006 by the Spacewatch survey at Kitt Peak Observatory. The smaller member, Шаблон:Mp, is about Шаблон:Cvt in diameter and was discovered on 11 September 2010 by the Mount Lemmon Survey at Mount Lemmon Observatory. It was not until February 2022 that astronomers began to recognize the similar orbits of these asteroids.

History

Observations

Шаблон:Mp was discovered on 10 November 2006 by the Spacewatch survey at Kitt Peak Observatory.[1] In that year, the asteroid received follow-up observations from Spacewatch and Mount Lemmon Survey only on 13 December 2006.[1] However, the number of observations was too sparse to accurately determine the asteroid's orbit, so it did not receive a provisional minor planet designation from the Minor Planet Center (MPC) and became a lost minor planet for nearly four years.[1] On 11 September and 28–29 October 2010, Mt. Lemmon Survey and Spacewatch reobserved the asteroid and other observatories began providing follow-up observations in November 2010 to secure its orbit.[1] The MPC gave the asteroid its provisional designation Шаблон:Mp on 7 November 2010 and later linked its 2010 observations to its 2006 discovery on 26 December 2010.[2]Шаблон:Rp[3]Шаблон:Rp The MPC gave Шаблон:Mp its permanent minor planet catalog number 458271 on 22 February 2016 and established official discovery credit to Spacewatch's 2006 observations.[4]Шаблон:Rp

Шаблон:Mp was discovered on 11 September 2010 by the Mt. Lemmon Survey at Mount Lemmon Observatory.[5] However, the MPC did not recognize the asteroid's existence until 14 December 2021.[6]Шаблон:Rp

Asteroid pair discovery

Файл:2010 UM26-2010 RN221 CFHT 2005-05-14 labeled.png
Canada–France–Hawaii Telescope precovery image of Шаблон:Mp and Шаблон:Mp from 14 May 2005

On 15 February 2022, Alessandro Odasso reported to the online Minor Planets Mailing List that Шаблон:Mp and Шаблон:Mp had extremely similar orbits.[7] He noticed that the two asteroids approached very close to each other in 2003 according to his numerical integration of their orbits, which led him to suspect that they may have separated from a common progenitor.[8][9]Шаблон:Rp Odasso was unable to prove the possibility that these asteroids are a single object; Peter Vereš of the MPC staff team confirmed that they are indeed two separate asteroids.[7] On that same day, Sam Deen found precovery observations of Шаблон:Mp and Шаблон:Mp appearing close together in archival Canada–France–Hawaii Telescope images from 14 May 2005.[10] A more rigorous study of the asteroid pair was published in Astronomy & Astrophysics by David Vokrouhlický and collaborators in November 2022, who acknowledged Odasso and Deen for independently discovering the asteroid pair.[9]Шаблон:Rp

Orbit

Файл:2010 UM26 orbit.jpg
Orbit diagram of Шаблон:Mp and Шаблон:Mp. The orbits and positions of these two asteroids are virtually identical in this diagram.

Шаблон:Mp and Шаблон:Mp both orbit the Sun in the middle zone of the main asteroid belt. They share extremely similar elliptical orbits with semi-major axes of 2.58 astronomical units (Шаблон:Convert) and orbital periods of 4.14 years.[9]Шаблон:Rp With orbital eccentricities of 0.326, the two asteroids come as close as Шаблон:Convert from the Sun at perihelion to as far as Шаблон:Convert at aphelion.[11][12] The asteroids' orbits are inclined 3.9° with respect to the plane of the Solar System.[9]Шаблон:Rp The asteroids' mean anomalies, or angular positions along their orbits, differ by less than 0.01°.[11][12][9]Шаблон:Rp

Formation

Asteroid pairs and binaries are thought to have formed from the rotational fissioning of a single precursor asteroid, as a result of accelerated rotation by the uneven reflection of sunlight off the asteroid's surface—a phenomenon known as the Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect. For asteroids with diameters under Шаблон:Cvt, the YORP effect can double their rotation rates within timescales of 1 million years, eventually leading to the ejection of surface material and disruption of their internal structures due to excessive centrifugal forces.[13]Шаблон:Rp Rotational fission preferentially occurs if the precursor asteroid's internal structure is weak, like a rubble pile consisting of rocks and dust loosely held together by gravity.[13]Шаблон:Rp

Numerical integrations of the orbits of Шаблон:Mp and Шаблон:Mp indicate that there is a 55% probability that the two asteroids separated after the year 2000, with the most likely date being March 2003.[9]Шаблон:Rp According to these numerical integrations, the two asteroids came within Шаблон:Cvt of each other in March 2003, with a range of possible close approach distances that could reach inside the ≈Шаблон:Cvt-radius Hill sphere of Шаблон:Mp.[9]Шаблон:Rp The relative velocities between the two asteroids in March 2003 were extremely small; there is a 99% probability that their relative velocities were less than Шаблон:Cvt at that time, which is much less than the ≈Шаблон:Cvt escape velocity of Шаблон:Mp.[9]Шаблон:Rp It is possible but very unlikely that Шаблон:Mp and Шаблон:Mp could have separated before the 2000s.[9]Шаблон:Rp

On 4 January 2023, David Jewitt and collaborators observed Шаблон:Mp and Шаблон:Mp with the Hubble Space Telescope to search for dusty debris that might have been ejected from the separation of Шаблон:Mp and Шаблон:Mp. They found no evidence of a dust trail nor macroscopic fragments larger than Шаблон:Cvt in diameter, which implies that the asteroid pair did not separate directly through rotational fission like the fragmenting active asteroid 331P/Gibbs.[14]Шаблон:Rp Jewitt and collaborators proposed that the pair separated by dissociating from a preexisting binary system, as a result of orbital expansion by gravitational perturbations and solar radiation pressure.[14]Шаблон:Rp A binary system like this can be formed by rotational fissioning of a single asteroid, but the split components can remain in orbit for over 100 years, enough time for solar radiation pressure to completely clear any dust and macroscopic fragments from the binary system by the time they dissociate.[14]Шаблон:Rp

Physical characteristics

Little is known about the sizes, albedos, and spectral types of Шаблон:Mp and Шаблон:Mp, since none these properties have been directly measured.[14]Шаблон:Rp Jewitt and collaborators examined archival Wide-field Infrared Survey Explorer (WISE) images of the asteroid pair from 2010, but were unable to detect any conclusive signs of infrared thermal emissions from either asteroid, thus precluding the measurement of their albedos.[14]Шаблон:Rp Nevertheless, Jewitt and collaborators assume a silicate (S-type) composition with a geometric albedo of 0.20 for Шаблон:Mp and Шаблон:Mp, since other asteroid pairs are known to have these characteristics.[14]Шаблон:Rp Using this assumed albedo for the asteroids' absolute magnitudes, they estimate diameters of Шаблон:Cvt and Шаблон:Cvt for Шаблон:Mp and Шаблон:Mp, respectively.[14]Шаблон:Rp

Hubble observations of Шаблон:Mp and Шаблон:Mp in 2023 showed that Шаблон:Mp is slightly elongated (aspect ratio 1.15:1) and rotates in 5.9 hours, whereas Шаблон:Mp is highly elongated (aspect ratio >2.5:1) and rotates slowly with a period of at least 20 hours.[14]Шаблон:Rp The particularly elongated shape of Шаблон:Mp challenges previous theories that elongated secondary components of binary asteroid systems should have been destroyed by rotational fission; this implies that Шаблон:Mp had either somehow avoided rotational fission or had undergone reshaping after it had fissioned from the primary component.[14]Шаблон:Rp

See also

References

Шаблон:Reflist

External links

Шаблон:Commons Шаблон:Commons Шаблон:Mp

Шаблон:Mp

Шаблон:Minor planets navigator Шаблон:Small Solar System bodies Шаблон:Portal bar

Партнерские ресурсы
Криптовалюты
Магазины
Хостинг
Разное

  1. ↑ 1,0 1,1 1,2 1,3 Ошибка цитирования Неверный тег <ref>; для сносок MPC-UM26 не указан текст
  2. ↑ Ошибка цитирования Неверный тег <ref>; для сносок MPS353965 не указан текст
  3. ↑ Ошибка цитирования Неверный тег <ref>; для сносок MPS362802 не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок MPC98597 не указан текст
  5. ↑ Ошибка цитирования Неверный тег <ref>; для сносок MPC-RN221 не указан текст
  6. ↑ Ошибка цитирования Неверный тег <ref>; для сносок MPS1524895 не указан текст
  7. ↑ 7,0 7,1 Ошибка цитирования Неверный тег <ref>; для сносок Odasso-37322 не указан текст
  8. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Odasso-blog не указан текст
  9. ↑ 9,0 9,1 9,2 9,3 9,4 9,5 9,6 9,7 9,8 Ошибка цитирования Неверный тег <ref>; для сносок Vokrouhlicky2022 не указан текст
  10. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Deen-37323 не указан текст
  11. ↑ 11,0 11,1 Ошибка цитирования Неверный тег <ref>; для сносок jpldata-UM26 не указан текст
  12. ↑ 12,0 12,1 Ошибка цитирования Неверный тег <ref>; для сносок jpldata-RN221 не указан текст
  13. ↑ 13,0 13,1 Ошибка цитирования Неверный тег <ref>; для сносок Polishook2014 не указан текст
  14. ↑ 14,0 14,1 14,2 14,3 14,4 14,5 14,6 14,7 14,8 Ошибка цитирования Неверный тег <ref>; для сносок Jewitt2023 не указан текст
Источник — http://wikihandbk.com/ruwiki/index.php?title=Английская_Википедия:(458271)_2010_UM26_and_2010_RN221&oldid=12480374