Bennu was the target of the OSIRIS-REx mission that returned samples of the asteroid to Earth.[14][15][16] The spacecraft, launched in September 2016, arrived at the asteroid two years later and mapped its surface in detail, seeking potential sample collection sites.[17] Analysis of the orbits allowed calculation of Bennu's mass and its distribution.[18] In October 2020, OSIRIS-REx briefly touched down and collected a sample of the asteroid's surface.[19][20][21] A capsule containing the sample was returned and landed on Earth in September 2023, with distribution and analysis of the sample ongoing.[22][23][24]
Discovery and observation
Series of Goldstone radar images in 1999 showing Bennu's rotation.
Bennu was discovered on 11 September 1999 during a Near-Earth asteroid survey by the Lincoln Near-Earth Asteroid Research (LINEAR).[3] The asteroid was given the provisional designation1999 RQ36 and classified as a near-Earth asteroid.[25] Bennu was observed extensively by the Arecibo Observatory and the Goldstone Deep Space Network using radar imaging as Bennu closely approached Earth on 23 September 1999.[26][12]
Naming
The name Bennu was selected from more than eight thousand student entries from dozens of countries around the world who entered a "Name that Asteroid!" contest run by the University of Arizona, The Planetary Society, and the LINEAR Project in 2012.[1][27] Third-grade student Michael Puzio from North Carolina proposed the name in reference to the Egyptian mythological bird Bennu. To Puzio, the OSIRIS-REx spacecraft with its extended TAGSAM arm resembled the Egyptian deity, which is typically depicted as a heron.[1]
Its features will be named after birds and bird-like creatures in mythology.[28]
Physical characteristics
Animation of Bennu rotating, imaged by OSIRIS-REx in December 2018.
Bennu has a roughly spheroidal shape, resembling a spinning top. Bennu's axis of rotation is tilted 178 degrees to its orbit; the direction of rotation about its axis is retrograde with respect to its orbit.[5] While the initial ground based radar observations indicated that Bennu had a fairly smooth shape with one prominent 10–20 m boulder on its surface,[29] high resolution data obtained by OSIRIS-REx revealed that the surface is much rougher with more than 200 boulders larger than 10 m on the surface, the largest of which is 58 m across.[5] The boulders contain veins of high albedocarbonate minerals believed to have formed prior to the formation of the asteroid due to hot water channels on the much larger parent body.[30][31] The veins range from 3 to 15 centimeters wide, and can be over one meter in length, much bigger than carbonate veins seen in meteorites.[31]
There is a well-defined ridge along the equator of Bennu. The presence of this ridge suggests that fine-grained regolith particles have accumulated in this area, possibly because of its low gravity and fast rotation (about once every 4.3 hours).[29] Observation by the OSIRIS-REx spacecraft has shown that Bennu is rotating faster over time.[32] This change in Bennu's rotation is caused by the Yarkovsky–O'Keefe–Radzievskii–Paddack effect.[32] Due to the uneven emission of thermal radiation from its surface as Bennu rotates in sunlight, the rotation period of Bennu decreases by about one second every 100 years.[32]
Observations of this minor planet by the Spitzer Space Telescope in 2007 gave an effective diameter of 484±10 m, which is in line with other studies. It has a low visible geometric albedo of 0.046±0.005. The thermal inertia was measured and found to vary by approximately 19% during each rotational period. It was based on this observation that scientists (incorrectly) estimated a moderate regolith grain size, ranging from several millimeters up to a centimeter, evenly distributed. No emission from a potential dust coma has been detected around Bennu, which puts a limit of 106 g of dust within a radius of 4750 km.[33]
Astrometric observations between 1999 and 2013 have demonstrated that 101955 Bennu is influenced by the Yarkovsky effect, causing the semimajor axis of its orbit to drift on average by 284±1.5 meters/year. Analysis of the gravitational and thermal effects has given a bulk density of ρ = 1190±13 kg/m3, which is only slightly denser than water. Therefore, the predicted macroporosity is 40±10%, suggesting the interior has a rubble pile structure or even hollows.[34] The estimated mass is (7.329±0.009)×1010 kg.[5]
Photometry and spectroscopy
Photometric observations of Bennu in 2005 yielded a synodic rotation period of 4.2905±0.0065 h. It has a B-type classification, which is a sub-category of carbonaceous asteroids. Polarimetric observations show that Bennu belongs to the rare F subclass of carbonaceous asteroids, which is usually associated with cometary features.[8] Measurements over a range of phase angles showed a phase function slope of 0.040 magnitudes per degree, which is similar to other near-Earth asteroids with low albedo.[35]
According to Dante Lauretta,[51] OSIRIS-REx Principal Investigator, "Bennu appears to be a very water-rich target, and water is the most interesting and perhaps the most lucrative commodity that you would mine from an asteroid".[52][53]
Predicted beforehand,[54] Dante Lauretta (University of Arizona) reiterates that Bennu is water-rich- already detectable while OSIRIS-REx was still technically in approach.[55]
Preliminary spectroscopic surveys of the asteroid's surface by OSIRIS-REx confirmed magnetite and the meteorite-asteroid linkage,[56][57][58] dominated by phyllosilicates.[59][60][61] Phyllosilicates, among others, hold water.[62][63][64]
Bennu's water spectra were detectable on approach,[57][65] reviewed by outside scientists,[66][42] then confirmed from orbit.[39][67][68][69]
OSIRIS-REx observations have resulted in a (self-styled) conservative estimate of about 7 x 108 kg water in one form alone, neglecting additional forms. This is a water content of ~1 wt.%, and potentially much more. In turn this suggests transient pockets of water beneath Bennu's regolith. The surficial water may be lost from the collected samples. However, if the sample return capsule maintains low temperatures, the largest (centimeter-scale) fragments may contain measurable quantities of adsorbed water, and some fraction of Bennu's ammonium compounds.[69] A separate estimate, including other forms of water storage, is 6.2 wt%.[70]
NASA and university sample facilities are preparing to secure, study, and curate the sample, predicted to be rich in water and organic compounds.[71][72][73]
The German SAL (Sample Analysis Laboratory) is preparing to receive cosmochemical water from Ryugu, Bennu, and other airless bodies.[74]
Wide angle shot of the Northern Hemisphere of Bennu, imaged by OSIRIS-REx at an altitude of approximately 1.8 km (1.1 mi)
Bennu's regolith-covered surface as imaged by OSIRIS-REx
The Nightingale sample site imaged by OSIRIS-REx at touchdown. The circular TAGSAM head in the center of the frame is 0.30 m (1 ft) in diameter.
All geological features on Bennu are named after various species of birds and bird-like figures in mythology.[95] The first features to be named were the final four candidate OSIRIS-REx sample sites, which were given unofficial names by the team in August 2019.[96] On 6 March 2020 the IAU announced the first official names for 12 Bennu surface features, including regiones (broad geographic regions), craters, dorsa (ridges), fossae (grooves or trenches) and saxa (rocks and boulders).[97]
Analysis showed that the particles making up Bennu's exterior are loosely packed and lightly bound to each other; "The spacecraft would have sunk into Bennu had it not fired its thrusters to back away immediately after it grabbed dust and rock from the asteroid's surface."[98] Analysis also revealed that the Sun's heat fractures rocks on Bennu in just 10,000 to 100,000 years instead of millions of years as was thought before.[99]
Abundant fine-grained material with a large variation in color. Primary sample collection site.[101]
Kingfisher
11°N 56°E
A relatively new crater with the highest water signature of all four sites.
Osprey
11°N 80°E
Located on a low albedo patch with a large variety of rocks. Backup sample collection site.[101]
Sandpiper
47°S 322°E
Located between two young craters, located in rough terrain. Minerals vary in brightness with hints of hydrated minerals.
On 12 December 2019, after a year of mapping Bennu's surface, a target site was announced. Named Nightingale, the area is near Bennu's north pole and lies inside a small crater within a larger crater. Osprey was selected as the backup sample site.[101]
The final four candidate OSIRIS-REx sample sites
IAU named features
Map of Bennu showing the locations of the IAU-named surface features
List of official IAU-named Bennu surface features[102]
The carbonaceous material that composes Bennu originally came from the breakup of a much larger parent body—a planetoid or a proto-planet. But like nearly all other matter in the Solar System, the origins of its minerals and atoms are to be found in dying stars such as red giants and supernovae.[103] According to the accretion theory, this material came together 4.5 billion years ago during the formation of the Solar System.
Bennu's basic mineralogy and chemical nature would have been established during the first 10 million years of the Solar System's formation, where the carbonaceous material underwent some geologic heating and chemical transformation inside a much larger planetoid or a proto-planet capable of producing the requisite pressure, heat and hydration (if need be)—into more complex minerals.[29] Bennu probably began in the inner asteroid belt as a fragment from a larger body with a diameter of 100 km.[104] Simulations suggest a 70% chance it came from the Polana family and a 30% chance it derived from the Eulalia family.[105] Impactors on boulders of Bennu indicate that Bennu has been in near Earth orbit (separated from the main asteroid belt) for 1–2.5 million years.[106]
Subsequently, the orbit drifted as a result of the Yarkovsky effect and mean motion resonances with the giant planets, such as Jupiter and Saturn. Various interactions with the planets in combination with the Yarkovsky effect modified the asteroid, possibly changing its spin, shape, and surface features.[107]
Cellino et al. have suggested a possible cometary origin for Bennu, based on similarities of its spectroscopic properties with known comets. The estimated fraction of comets in the population of near Earth objects is 8%±5%.[8] This includes rock comet3200 Phaethon, discovered and still numbered as an asteroid.[108][109]
Orbit
Diagram of the orbits of Bennu and the inner planets around the Sun.
Bennu orbits the Sun with a period of 1.19 years (435 days) as of 2022[update].[3] Earth gets as close as about 480,000 km (0.0032 au) from its orbit around 23 to 25 September. On 22 September 1999 Bennu passed 0.0147 au from Earth, and six years later on 20 September 2005 it passed 0.033 au from Earth.[1] The next close approaches of less than 0.04 au will be 30 September 2054 and then 23 September 2060, which will perturb the orbit slightly. Between the close approach of 1999 and that of 2060, Earth completes 61 orbits and Bennu 51. An even closer approach will occur on 25 September 2135 around 0.0014 au (see table).[1] In the 75 years between the 2060 and 2135 approaches, Bennu completes 64 orbits, meaning its period will have changed to 1.17 years (427 days).[110] The Earth approach of 2135 will increase the orbital period to about 1.24 years (452 days).[110] Before the 2135 Earth approach, Bennu's maximum distance from the Earth occurs on 27 November 2045 at a distance of 2.34 AU (350 million km).[111]
Bennu approaches less than 0.05AU Position uncertainty and increasing divergence[1]
≈0.3 AU (40 million km) (Gravity Simulator)[112][113] 1.1 AU (160 million km) (NEODyS)[114]
±370 million km
Possible Earth impact
On average, an asteroid with a diameter of 500 m (1,600 ft; 0.31 mi) can be expected to impact Earth about every 130,000 years or so.[115] A 2010 dynamical study by Andrea Milani and collaborators predicted a series of eight potential Earth impacts by Bennu between 2169 and 2199. The cumulative probability of impact is dependent on physical properties of Bennu that were poorly known at the time, but was found to not exceed 0.071% for all eight encounters.[116] The authors recognized that an accurate assessment of 101955 Bennu's probability of Earth impact would require a detailed shape model and additional observations (either from the ground or from spacecraft visiting the object) to determine the magnitude and direction of the Yarkovsky effect.
The publication of the shape model and of astrometry based on radar observations obtained in 1999, 2005, and 2011[26] made possible an improved estimate of the Yarkovsky acceleration and a revised assessment of the impact probability. In 2014, the best estimate of the impact probability was a cumulative probability of 0.037% in the interval 2175 to 2196.[117] This corresponds to a cumulative score on the Palermo scale of −1.71. If an impact were to occur, the expected kinetic energy associated with the collision would be 1,200 megatons in TNT equivalent (for comparison, TNT equivalent of Tsar Bomba, the most powerful nuclear weapon ever tested, was approximately 54 megatons,[10] and that of the Tunguska event, the most energetic impact event in recorded history, has been estimated at 3-5 megatons,[118] though another estimate is 20-30 megatons[119]).
The 2021 orbit solution extended the virtual impactors from the year 2200 to the year 2300 and slightly increased the cumulative Palermo impact scale to −1.42. The solution even included the estimated masses of 343 other asteroids and represents about 90% of the total mass of the main asteroid belt.[11]
2060/2135 close approaches
Animation of 101955 Bennu's position relative to the Earth, as both orbit the Sun, in the years 2128 to 2138. 2135 close approach is shown near the end of the animation. Earth· 101955 Bennu
Bennu will pass 0.005 au (750,000 km; 460,000 mi) from Earth on 23 September 2060,[1] while for comparison the Moon's average orbital distance (lunar distance) is 384,402 km (238,856 mi) and will only change to 384,404 km in 50 years time. Bennu will be too dim to be seen with common binoculars.[120] The close approach of 2060 causes divergence in the close approach of 2135. On 25 September 2135, the Earth approach distance is 0.00136 au (203,000 km; 126,000 mi) ±20 thousand km.[1] There is no chance of an Earth impact in 2135.[121][10] The 2135 approach will create many lines of variations and Bennu may pass through a gravitational keyhole during the 2135 passage which could create an impact scenario at a future encounter. The keyholes are all less than ~20 km wide with some keyholes being only 5 meters wide.[122]
2182
The most threatening virtual impactor is on Tuesday, 24 September 2182 when there is a 1 in 2,700 chance of an Earth impact,[10] but the asteroid could be as far as the Sun is from Earth.[114] To impact Earth on 24 September 2182 Bennu must pass through a keyhole roughly 5 km wide on 25 September 2135.[122] The next two biggest risks occur in 2187 (1:14,000) and 2192 (1:26,000).[10] There is a cumulative 1 in 1,800 chance of an Earth impact between 2178 and 2290.[10]
Long term
Lauretta et al. reported in 2015 their results of a computer simulation, concluding that it is more likely that 101955 Bennu will be destroyed by some other cause:
The orbit of Bennu is intrinsically dynamically unstable, as are those of all NEOs. In order to glean probabilistic insights into the future evolution and likely fate of Bennu beyond a few hundred years, we tracked 1,000 virtual "Bennus" for an interval of 300 Myr with the gravitational perturbations of the planets Mercury–Neptune included. Our results ... indicate that Bennu has a 48% chance of falling into the Sun. There is a 10% probability that Bennu will be ejected out of the inner Solar System, most likely after a close encounter with Jupiter. The highest impact probability for a planet is with Venus (26%), followed by the Earth (10%) and Mercury (3%). The odds of Bennu striking Mars are only 0.8% and there is a 0.2% chance that Bennu will eventually collide with Jupiter.[107]
The successful October 2020 sample collection, showing OSIRIS-REx touching down on the Nightingale sample site
The OSIRIS-REx mission of NASA's New Frontiers program was launched towards 101955 Bennu on 8 September 2016. On 3 December 2018, the spacecraft arrived at the asteroid Bennu after a two-year journey.[17] One week later, at the American Geophysical Union Fall Meeting, investigators announced that OSIRIS-REx had discovered spectroscopic evidence for hydrated minerals on the surface of the asteroid, implying that liquid water was present in Bennu's parent body before it split off.[124][5]
On 20 October 2020, OSIRIS-REx descended to the asteroid and "pogo-sticked off"[19] it while successfully collecting a sample.[125] On 7 April 2021, OSIRIS-REx completed its final flyover of the asteroid and began slowly drifting away from it.[126] On 10 May 2021, the departure was completed with OSIRIS-REx while still managing to contain the asteroid sample.[24] OSIRIS-REx returned samples to Earth in 2023[127] via a capsule-drop by parachute, ultimately, from the spacecraft to the Earth's surface in Utah on 24 September 2023.[19]
Shortly after the sample container was retrieved and transferred to an airtight chamber at the Johnson Space Center in Houston, Texas, the lid on the container was opened. Scientists commented that they "found black dust and debris on the avionics deck of the OSIRIS-REx science canister" on the initial opening. Further study is planned. On 11 October 2023, the recovered capsule was opened to reveal a "first look" at the asteroid sample contents.[128] Since 3 November 2023, a part of the sample is exhibited at the Hall of Meteorites of the National Museum of Natural History (Washington, DC).[129] On 13 December 2023, further studies of the returned sample were reported and revealed organic molecules as well as unknown materials which require more study to have a better idea of their compostion and makeup.[130][131] On 11 January 2024, NASA reported finally fully opening, after three months of trying, the recovered container with samples from the Bennu asteroid.[132][133][134] The total weight of the recovered material weighed 121.6 g (4.29 oz), over twice the mission's goal.[135]
Selection
The asteroid Bennu was selected from over half a million known asteroids by the OSIRIS-REx selection committee. The primary constraint for selection was close proximity to Earth, since proximity implies low impulse (Δv) required to reach an object from Earth orbit.[136] The criteria stipulated an asteroid in an orbit with low eccentricity, low inclination, and an orbital radius of 0.8–1.6 au.[137] Furthermore, the candidate asteroid for a sample-return mission must have loose regolith on its surface, which implies a diameter greater than 200 meters. Asteroids smaller than this typically spin too fast to retain dust or small particles. Finally, a desire to find an asteroid with pristine carbon material from the early Solar System, possibly including volatile molecules and organic compounds, reduced the list further.
With the above criteria applied, five asteroids remained as candidates for the OSIRIS-REx mission, and Bennu was chosen, in part for its potentially hazardous orbit.[137]
OSIRIS-REx - 101955 Bennu - Earth
Trajectory in the Solar System from 9 August 2016 to 24 September 2023
Trajectory around 101955 Bennu from 25 December 2018
^ abcdHergenrother, Carl W; Maria Antonietta Barucci; Barnouin, Olivier; Bierhaus, Beau; Binzel, Richard P; Bottke, William F; Chesley, Steve; Clark, Ben C; Clark, Beth E; Cloutis, Ed; Christian Drouet d'Aubigny; Delbo, Marco; Emery, Josh; Gaskell, Bob; Howell, Ellen; Keller, Lindsay; Kelley, Michael; Marshall, John; Michel, Patrick; Nolan, Michael; Rizk, Bashar; Scheeres, Dan; Takir, Driss; Vokrouhlický, David D; Beshore, Ed; Lauretta, Dante S (2018). "Unusual polarimetric properties of (101955) Bennu: similarities with F-class asteroids and cometary bodies". Monthly Notices of the Royal Astronomical Society: Letters. 481 (1): L49–L53. arXiv:1808.07812. Bibcode:2018MNRAS.481L..49C. doi:10.1093/mnrasl/sly156. S2CID119226483.
^"Sentry Risk Table". NASA/JPL Near-Earth Object Program Office. Archived from the original on 11 September 2016. Retrieved 20 March 2018. (Use Unconstrained Settings)
^Emery, J.; et al. (July 2014), Muinonen, K. (ed.), "Thermal infrared observations and thermophysical characterization of the OSIRIS-REx target asteroid (101955) Bennu", Conference Proceedings Asteroids, Comets, Meteors 2014: 148, Bibcode:2014acm..conf..148E.
^Hergenrother, Carl W.; et al. (September 2013), "Lightcurve, Color and Phase Function Photometry of the OSIRIS-REx Target Asteroid (101955) Bennu", Icarus, 226 (1): 663–670, Bibcode:2013Icar..226..663H, doi:10.1016/j.icarus.2013.05.044.
^Takir, D; Emery, J; Hibbits, C (2017). 3-μm Spectroscopy Of Water-Rich Meteorites And Asteroids: New Results And Implications. Hayabusa Symposium 2017.
^Mason, B (1962). Meteorites. New York and London: John Wiley and Sons Inc. p. 60. OCLC468300914. an important constituent in many of the carbonaceous chondrites
^Brearley, A (2006). "The Action of Water". Meteorites and the Early Solar System II. Tucson: University of Arizona Press. p. 587. ISBN978-0-8165-2562-1.
^All About Bennu: A Rubble Pile with a Lot of Surprises. Kimberly M. S. Cartier, EOS Planetary Sciences. 21 March 2019. "In terms of spectra and minerology, Bennu's rocks 'look a lot like the rarest, most fragile meteorites in our collection,' Lauretta said, referring to the CM carbonaceous chondrites"
^Kurokawa, H.; Shibuya, T.; Sekine, Y.; Ehlmann, B. L.; Usui, F.; Kikuchi, S.; Yoda, M. (January 2022). "Distant Formation and Differentiation of Outer Main Belt Asteroids and Carbonaceous Chondrite Parent Bodies". AGU Advances. 3 (1). arXiv:2112.10284. Bibcode:2022AGUA....300568K. doi:10.1029/2021AV000568. S2CID245302669.
^Montoya, M.; Plummer, J.; Martinez, S. III; Snead, C. J.; Lunning, N.; Righter, K.; Allums, K.; Rodriguez, M.; Funk, R. C.; Connelly, W.; Gonzalez, C.; Calva, C.; Ferrodous, J.; Lugo, G.; Hernandez Gomez, N.; Connolly, H. C. Jr. (2023). Materials-Compliant Containers in Preparation for OSIRIS-REx Sample Return. 86th Meteoritical Society Meeting. p. 6050.
^Prince, B. S.; Zega, T. J.; Connolly, H. C. Jr.; Lauretta, D. S. (2023). Developing Fluid Inclusion Analysis Techniques in Anticipation of OSIRIS-REx Sample Return. 86th MetSoc. p. 6155.
^Bonato, E.; Helbert, J.; Schwinger, S.; Maturilli, A.; Greshake, A.; Hecht, -L. (2023). The Sample Analysis Laboratory At DLR And Its Extension To Curation Facility for MMX. 86th MetSoc. p. 6035.
^Lim, L (2019). OSIRIS-REx update. 21st NASA Small Bodies Assessment Group. "Bennu is an Active Asteroid!"
^ abBarrucci, M; Michel, P (September 2019). Asteroid-Comet continuum: no doubt but many questions. 2019 EPSC-DPS conference. pp. 202–1.
^Hergenrother, C; Adam, C; Antreasian, P; Al Asad, M; Balram-Knutson, S (September 2019). (101955) Bennu is an active asteroid. 2019 EPSC-DPS conference. pp. 852–1.
^Boe, B; Jedicke, R; Wiegert, P; Meech, K; Morbidelli, A (September 2019). Distinguishing Between Solar System Formation Models with Manxes (or not). 2019 EPSC-DPS conference. pp. 626–2.[page needed]
^Gounelle, M (2012). The Asteroid-Comet Continuum: Evidence from Extraterrestrial Samples. 2012 European Planetary Science Congress. p. 220.
^Rickman, H (2018). Origin and Evolution of Comets: Ten Years after the Nice Model, One Year after Rosetta. Singapore: World Scientific. pp. 162–168. Sec. 4.3 Dormancy and Rejuvenation
^Marsset, M; DeMeo, F; Polishook, D; Binzel, R (September 2019). Near-infrared spectral variability on the newly active asteroid (6478) Gault. 2019 EPSC-DPS conference. Epsc-DPS Joint Meeting 2019. Vol. 2019. pp. EPSC-DPS2019-280. Bibcode:2019EPSC...13..280M.
^Robert Marcus; H. Jay Melosh & Gareth Collins (2010). "Earth Impact Effects Program". Imperial College London / Purdue University. Retrieved 7 February 2013. (solution using density of 2,600 kg/m^3, sped of 17km/s, and impact angle of 45 degrees)
^Chesley, Steven R.; Farnocchia, Davide; Nolan, Michael C.; Vokrouhlický, David; Chodas, Paul W.; Milani, Andrea; Spoto, Federica; Rozitis, Benjamin; Benner, Lance A.M.; Bottke, William F.; Busch, Michael W.; Emery, Joshua P.; Howell, Ellen S.; Lauretta, Dante S.; Margot, Jean-Luc; Taylor, Patrick A. (2014). "Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu". Icarus. 235: 5–22. arXiv:1402.5573. Bibcode:2014Icar..235....5C. doi:10.1016/j.icarus.2014.02.020. ISSN0019-1035. S2CID30979660.
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