To get the best science return from the flyby, the spacecraft had to be manouevred to the limits of its design, including flipping over and changing its orientation rapidly. – Így add tovább! Another large crater in the centre of the asteroid is about 650 m wide and 80 m deep and was named "Topaz". Several hundred images covering four rotation periods without interruption, were acquired. In the asteroid belt, however, the accretion process was halted with the birth of Jupiter because its enormous gravity shepherded the asteroids into more orderly orbits. Several hundred images covering four rotation periods without interruption, were acquired. Analysis of the data revealed that the light curve of asteroid 2867 Steins is double peaked with an amplitude of approximately 0.23 mag. The structure suggests that Steins will eventually fall apart. The images showed a gaping hole at the south pole of Steins – a large impact crater about 2 km wide and nearly 300 m deep. Highlights from the Rosetta mission thus far, Planetary protection for the Rosetta mission, From harbingers of doom to celestial wanderers, Selecting a landing site for Rosetta's lander, Philae. A 2867 Šteins egy E típusú kisbolygók, amely a kisbolygóövben kering. Light curve of asteroid (2867) Steins from OSIRIS data, March 2006. Rosetta imaged Steins regularly with its cameras from about one month before closest approach, allowing more precise calculations of the asteroid’s orbit. Otkrio ga je 4. studenog 1969. sovjetski astronom Nikolaj Chernykh na Krimskom astrofizičkom opservatoriju u Naučniju na Krimskom poluotoku. Located in the main asteroid belt, lying between the orbit of Mars and Jupiter, this space rock is being intercepted by Rosetta, which is on its way to comet 67P/Churyumov-Gerasimenko. The effect would have caused landslides to fill in the smaller craters. 2867 Steins (1969 VC) Discovered 1969-Nov-04 by Chernykh, N. at Nauchnyj Reference: DISCOVERY.DB Last Updated: 2003-08-29 In this case, the change in rotation rate resulted in some material moving towards the equator of the asteroid. The features visible in the images obtained near closest approach give further clues about the asteroid’s history and future. To date, planetary scientists have used various spacecraft to visit eight different asteroids, with six fly-bys and two close orbits. On 5 September 2008, the Rosetta spacecraft will make it nine. képek a 2867 Steins kisbolygóról, melyeket a Rosetta űrszonda készített a 2008 augusztusi elhaladáskor. (2008): Roseta target asteroid 2867 Steins: An unusual E-type asteroid. 2867 Šteins este un mic asteroid din Centura principală descoperit în 1969 de astronomul Nikolai Cernîh la Naucinîi. Apart from delivering brand-new science, this fly-by acts as a rehearsal for the campaign planned for asteroid Lutetia in 2010.
This was essential because the orbit was not well enough known based on observations from the ground to allow for a close fly-by. Closest approach is scheduled for 5 September 2008, 20:58 CEST. It will also take images and spectra, from which conclusions can be drawn about its composition and collisional history. 3.0. Such E-type asteroids are quite rare. For more information on asteroid types, please see article Debris of the Solar System: Asteroids. Steins surprised them: it turned out to be a kind of asteroid that no spacecraft had flown close to before. Anal… In their paper E-type asteroid (2867) Steins as Imaged by OSIRIS on board Rosetta, H. Uwe Keller and colleagues conclude that Steins probably gained its diamond shape from the YORP effect - the Yarkovsky-O'Keefe-Radzievskii-Paddack effect – in which photons from the Sun are re-radiated as infrared emission taking momentum from the body and altering the rotation rate. Continuous coverage of the asteroid, lasting more than 24 hours was obtained at a phase angle of 41.7 degrees – this is larger than the maximum phase angle of Steins (30 degrees) that can be seen from Earth. Images of asteroid (2867) Steins taken by the OSIRIS Wide Angle Camera on Rosetta during the fly-by of 5 September 2008. https://hu.wikipedia.org/w/index.php?title=2867_Šteins&oldid=21816035, Creative Commons Nevezd meg! In its asteroid fly-by mode, Rosetta’s orientation was automatically controlled by the on-board navigation cameras.
The observations by OSIRIS and VIRTIS on Rosetta brought new information that could not have been gained from the ground. Asteroid (2867) Steins is the first scientific target of ESA’s comet chaser Rosetta. The rotation period was determined to be 6.052 ± 0.007 hours which confirmed previous measurements obtained from ground.
2867 Šteins, privremene oznake 1969 VC, nepravilni je asteroid iz unutarnjih područja asteroidnog pojasa, promjera oko 5 km.
A lap utolsó módosítása: 2019. október 17., 07:47. Ο Στέινς (Šteins) είναι ένας μικρός αστεροειδής της Κύριας Ζώνης Αστεροειδών με απόλυτο μέγεθος (όπως ορίζεται για το Ηλιακό Σύστημα) 12,90. It was later struck by other objects, creating impact craters. Located in the main asteroid belt, lying between the orbit of Mars and Jupiter, this space rock is being intercepted by Rosetta, which is on its way to comet 67P/Churyumov-Gerasimenko. 5. In preparation for the flyby, observations of asteroid Steins were performed using Rosetta’s OSIRIS camera in March 2006. After its orbit was firstly established, it received the number 2867 and was named after Karlis Augustovich Steins, the former director of the Latvian University Astronomical Observatory. This type of loosely bound structure is also consistent with the YORP effect hypothesis. Rosetta was at a distance of 800 km with a relative speed with respect to Steins of 8.6 km/s, or about 31 000 km/h. This is the first time that the YORP effect has been seen in a main-belt asteroid. Asteroid (2867) Steins was imaged at limited spatial resolution by the OSIRIS cameras during the September 2009 flyby by the Rosetta spacecraft.
Asteroid 2867 Steins is the first target of the Rosetta space mission with a flyby scheduled in September 2008. ).
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