[ad_1]
Quaoar 링의 아티스트 인상. 출처: 파리 천문대
ESA의 Cheops는 난쟁이 행성 Quaoar 주변에서 예기치 않은 고리를 찾습니다.
다른 별 주위의 행성을 관찰하던 중 휴식 시간에 유럽 우주국의 ExOPlanet Satellite tv for pc(Cheops) 임무 특성화 관찰했다 왜 소행성 태양계 주변에 밀집된 물질 고리를 발견하는 데 결정적인 기여를 했습니다.
왜소 행성은 Quaoar로 알려져 있습니다. Quaoar 반지름의 거의 7.5배 거리에 있는 고리의 존재는 천문학자들이 해결해야 할 미스터리를 열어줍니다. 왜 이 물질이 작은 달로 합쳐지지 않았는가?
난쟁이 행성 Quaoar와 그 고리에 대한 예술가의 인상. Quaoar의 위성 Weywot가 왼쪽에 표시됩니다. Quaoar의 고리는 2018년에서 2021년 사이에 발생한 일련의 관측을 통해 발견되었습니다. 천문학자들은 지상 기반 망원경 모음과 ESA의 우주 기반 망원경 Cheops를 사용하여 Quaoar가 일련의 멀리 있는 별들 앞에서 교차하는 것을 관찰했습니다. 그것이 지나갈 때 그들의 빛을 끄십시오. 크레딧: ESA, CC BY-SA 3.0 IGO
태양계에서 먼 물체를 관찰하는 방법
이 고리는 2018년에서 2021년 사이에 발생한 일련의 관측을 통해 발견되었습니다. 천문학자들은 지상 기반 망원경 컬렉션과 우주 기반 망원경 Cheops를 사용하여 Quaoar가 일련의 멀리 있는 별들 앞에서 교차하는 것을 관찰했습니다. 그것이 지나갈 때 그들의 빛을 끄십시오.
이러한 사건을 엄폐라고 합니다. 가려진 별에서 나오는 빛이 어떻게 떨어지는지 관찰하면 가려진 물체의 크기와 모양에 대한 정보를 얻을 수 있고 중간 물체에 대기가 있는지 여부를 알 수 있습니다. 이 경우 주요 엄폐 전후의 작은 방울은 Quaoar 주위를 공전하는 물질의 존재를 드러냈습니다.
Quaoar는 Trans-Neptunian 물체로 알려진 작고 먼 세계 모음 중 하나입니다.[{” attribute=””>TNOs). Roughly 3000 are known. As the name suggests, TNOs are found in the outer reaches of the Solar System, beyond the orbit of planet Neptune. The largest of the TNOs are Pluto and Eris. With an estimated radius of 555 km, Quaoar ranks around number seven on the size list, and is orbited by a small moon called Weywot, roughly 80 km in radius.
Studying these dwarf planets is difficult because of their small sizes and extreme distances. Quaoar itself orbits the Sun at almost 44 times the Sun-Earth distance. So, occultations are particularly valuable tools. Until recently, however, it has been difficult to predict exactly when and where they will take place.
For an occultation to occur, the alignment between the occulting object (here the TNO), the star, and the observing telescope must be extremely precise. In the past, it has been almost impossible to meet the stringent accuracy requirements to be certain of seeing an event. Nevertheless, to pursue this goal the European Research Council Lucky Star project, coordinated by Bruno Sicardy, Sorbonne University & Paris Observatory – PSL (LESIA), was created to predict upcoming occultations by TNOs, and to co-ordinate the observation of these events from professional and amateur observatories around the globe.
Artist’s impression of Cheops, ESA’s Characterising Exoplanet Satellite, in orbit above Earth. In this view the satellite’s telescope cover is open. Credit:
ESA / ATG medialab
Precise alignment
Recently, the number of observed stellar occultations has increased. In large part, this is due to the contribution of data from ESA’s star mapping mission Gaia. The spacecraft has delivered such stunning accuracy in its stellar positions that the predictions made by the Lucky Star team has become much more certain.
One of the people involved in the Lucky Star project is Isabella Pagano of the INAF’s Astrophysical Observatory of Catania, Italy, and a member of the Cheops Board. Isabella was contacted by Kate Isaak, ESA’s Project Scientist for the Cheops mission, who was curious whether the space telescope would also be able to catch an occultation.
“I was a little skeptical about the possibility to do this with CHEOPS,” admits Isabella, “But we investigated the feasibility.”
The main issue was that the satellite’s trajectory can be slightly modified because of drag in the upper parts of the Earth’s atmosphere. This is due to the unpredictable solar activity that can hit our planet and puff up its atmosphere.
Indeed, the first time the team attempted to observe an occultation with Cheops, which involved Pluto, the prediction was not quite accurate enough, and no occultation could be observed.
The alignment was more favourable on the second attempt, however, when they observed Quaoar. In doing so, they made the first ever detection of a stellar occultation by a trans-Neptunian object from space.
Artist’s impression of CHEOPS. Credit: © ESA / ATG medialab
Put a ring on it
“The Cheops data are amazing for signal to noise,” says Isabella. The signal to noise is a measure of how strong the detected signal is to the random noise in the system. Cheops gives a great signal to noise because the telescope is not looking through the distorting effects of the Earth’s lower atmosphere.
This clarity proved decisive in recognizing Quaoar’s ring system because it allowed the researchers to eliminate the possibility that the drops in light were caused by a spurious effect in Earth’s atmosphere. By combining several secondary detections, taken with telescopes on Earth, it was possible to be certain that they were caused by a ring system surrounding Quaoar.
Bruno Morgado, Universidade Federal do Rio de Janeiro, Brazil, led the analysis. He combined the Cheops data with that from large professional observatories around the world and amateur citizen scientists, all of whom had observed Quaoar occult various stars over the last few years. “When we put everything together, we saw drops in brightness that were not caused by Quaoar, but that pointed to the presence of material in a circular orbit around it. The moment we saw that we said, ‘Okay, we are seeing a ring around Quaoar.’”
When it comes to ring systems, the giant planet Saturn holds the crown. Known as the ringed planet, Saturn boasts a collection of dust and small moonlets that circle the planet’s equator. In spite of being an impressive observational sight, the mass of the ring system is quite small. If collected it would make between one-third and one half the mass of Saturn’s moon Mimas, or about half the mass of Earth’s Antarctic ice shelf.
Quaoar’s ring is much smaller than Saturn’s but no less intriguing. It is not the only ring system known to exist around a dwarf or minor planet. Two others – around Chariklo and Haumea – have been detected through ground-based observations. What makes Quaoar’s ring unique, however, is where it is found relative to Quaoar itself.
The Roche limit
Any celestial object with an appreciable gravitational field will have a limit within which an approaching celestial object will be pulled to pieces. This is known as the Roche limit. Dense ring systems are expected to exist inside of the Roche limit, which is the case for Saturn, Chariklo and Haumea.
“So, what is so intriguing about this discovery around Quaoar is that the ring of material is much farther out than the Roche limit,” says Giovanni Bruno, INAF’s Astrophysical Observatory of Catania, Italy.
This is a mystery because according to conventional thinking, rings beyond the Roche limit will coalesce into a small moon within just a few decades. “As a result of our observations, the classical notion that dense rings survive only inside the Roche limit of a planetary body must be thoroughly revised,” says Giovanni.
Early results suggest that the frigid temperatures at Quaoar may play a role in preventing the icy particles from sticking together but more investigations are needed.
“The Cheops observations have played a key role in establishing the presence of a ring around Quaoar, in an application of high precision, high cadence photometry that goes beyond the more typical exoplanet science of the mission,” says Kate.
While the theoreticians get to work on how the Quaoar rings can survive, the Lucky Star project will continue to look at Quaoar and also other TNOs as they occult distant stars to measure their physical characteristics and see how many others also have ring systems.
And Cheops will return to its original mission to study nearby exoplanets.
Reference: “A dense ring of the trans-Neptunian object Quaoar outside its Roche limit” by B. E. Morgado, B. Sicardy, F. Braga-Ribas, J. L. Ortiz, H. Salo, F. Vachier, J. Desmars, C. L. Pereira, P. Santos-Sanz, R. Sfair, T. de Santana, M. Assafin, R. Vieira-Martins, A. R. Gomes-Júnior, G. Margoti, V. S. Dhillon, E. Fernández-Valenzuela, J. Broughton, J. Bradshaw, R. Langersek, G. Benedetti-Rossi, D. Souami, B. J. Holler, M. Kretlow, R. C. Boufleur, J. I. B. Camargo, R. Duffard, W. Beisker, N. Morales, J. Lecacheux, F. L. Rommel, D. Herald, W. Benz, E. Jehin, F. Jankowsky, T. R. Marsh, S. P. Littlefair, G. Bruno, I. Pagano, A. Brandeker, A. Collier-Cameron, H. G. Florén, N. Hara, G. Olofsson, T. G. Wilson, Z. Benkhaldoun, R. Busuttil, A. Burdanov, M. Ferrais, D. Gault, M. Gillon, W. Hanna, S. Kerr, U. Kolb, P. Nosworthy, D. Sebastian, C. Snodgrass, J. P. Teng and J. de Wit, 8 February 2023, Nature.
DOI: 10.1038/s41586-022-05629-6
Cheops is a collaboration between the European Space Agency (ESA) and a consortium of 11 countries, led by Switzerland and the University of Bern. The consortium, including Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the UK, has made significant contributions to the mission.
ESA holds the role of mission architect, managing the procurement and testing of the satellite, launch, early operations, and in-orbit commissioning, as well as the Guest Observers’ Program that allows scientists worldwide to observe with Cheops. Airbus Defence and Space in Madrid, Spain is the prime contractor for the spacecraft’s design and construction.
The Mission Operations Centre for the Cheops mission is located at INTA near Madrid, Spain, while the Science Operations Centre is based at the University of Geneva, Switzerland. Both centers are run by the consortium.
[ad_2]
Source_