Comet Shoemaker–Levy 9
More exciting for planetary astronomers was that the best orbital calculations suggested that the comet would pass within 45,000 km (28,000 mi) of the center of Jupiter, a distance smaller than the planet's radius, meaning that there was an extremely high probability that SL9 would collide with Jupiter in July 1994. Studies suggested that the train of nuclei would plow into Jupiter's atmosphere over a period of about five days.
Predictions for the collision
The discovery that the comet was likely to collide with Jupiter caused great excitement within the astronomical community and beyond, as astronomers had never before seen two significant Solar System bodies collide. Intense studies of the comet were undertaken, and as its orbit became more accurately established, the possibility of a collision became a certainty. The collision would provide a unique opportunity for scientists to look inside Jupiter's atmosphere, as the collisions were expected to cause eruptions of material from the layers normally hidden beneath the clouds.
Astronomers estimated that the visible fragments of SL9 ranged in size from a few hundred metres to two kilometres across, suggesting that the original comet may have had a nucleus up to 5 km (3.1 mi) across – somewhat larger than Comet Hyakutake, which became very bright when it passed close to the Earth in 1996. One of the great debates in advance of the impact was whether the effects of the impact of such small bodies would be noticeable from Earth, apart from a flash as they disintegrated like giant meteors. Other suggested effects of the impacts were seismic waves travelling across the planet, an increase in stratospheric haze on the planet due to dust from the impacts, and an increase in the mass of the Jovian ring system. However, given that observing such a collision was completely unprecedented, astronomers were cautious with their predictions of what the event might reveal.
Anticipation grew as the predicted date for the collisions approached, and astronomers trained terrestrial telescopes on Jupiter. Several space observatories did the same, including the Hubble Space Telescope, the ROSAT X-ray observing satellite, and significantly the Galileo spacecraft, then on its way to a rendezvous with Jupiter scheduled for 1995. While the impacts took place on the side of Jupiter hidden from Earth, Galileo, then at a distance of 1.6 AU from the planet, was able to see the impacts as they occurred. Jupiter's rapid rotation brought the impact sites into view for terrestrial observers a few minutes after the collisions.
Two other satellites made observations at the time of the impact: the Ulysses spacecraft, primarily designed for solar observations, was pointed towards Jupiter from its location 2.6 AU away, and the distant Voyager 2 probe, some 44 AU from Jupiter and on its way out of the Solar System following its encounter with Neptune in 1989, was programmed to look for radio emission in the 1–390 kHz range.
The first impact occurred at 20:13 UTC on July 16, 1994, when fragment A of the nucleus entered Jupiter's southern hemisphere at a speed of about 60 km/s. Instruments on Galileo detected a fireball which reached a peak temperature of about 24,000 K, compared to the typical Jovian cloudtop temperature of about 130 K, before expanding and cooling rapidly to about 1500 K after 40 s. The plume from the fireball quickly reached a height of over 3,000 km. A few minutes after the impact fireball was detected, Galileo measured renewed heating, probably due to ejected material falling back onto the planet. Earth-based observers detected the fireball rising over the limb of the planet shortly after the initial impact.
Astronomers had expected to see the fireballs from the impacts, but did not have any idea in advance how visible the atmospheric effects of the impacts would be from Earth. Observers soon saw a huge dark spot after the first impact. The spot was visible even in very small telescopes, and was about 6,000 km (3,700 mi) (one Earth radius) across. This and subsequent dark spots were thought to have been caused by debris from the impacts, and were markedly asymmetric, forming crescent shapes in front of the direction of impact.
Over the next 6 days, 21 distinct impacts were observed, with the largest coming on July 18 at 07:33 UTC when fragment G struck Jupiter. This impact created a giant dark spot over 12,000 km across, and was estimated to have released an energy equivalent to 6,000,000 megatons of TNT (600 times the world's nuclear arsenal). Two impacts 12 hours apart on July 19 created impact marks of similar size to that caused by fragment G, and impacts continued until July 22, when fragment W struck the planet.
Observations and discoveries
Observers hoped that the impacts would give them a first glimpse of Jupiter beneath the cloud tops, as lower material was exposed by the comet fragments punching through the upper atmosphere. Spectroscopic studies revealed absorption lines in the Jovian spectrum due to diatomic sulfur (S2) and carbon disulfide (CS2), the first detection of either in Jupiter, and only the second detection of S2 in any astronomical object. Other molecules detected included ammonia (NH3) and hydrogen sulfide (H2S). The amount of sulfur implied by the quantities of these compounds was much greater than the amount that would be expected in a small cometary nucleus, showing that material from within Jupiter was being revealed. Oxygen-bearing molecules such as sulfur dioxide were not detected, to the surprise of astronomers.
As well as these molecules, emission from heavy atoms such as iron, magnesium and silicon was detected, with abundances consistent with what would be found in a cometary nucleus. While substantial water was detected spectroscopically, it was not as much as predicted beforehand, meaning that either the water layer thought to exist below the clouds was thinner than predicted, or that the cometary fragments did not penetrate deeply enough. The relatively low levels of water were later confirmed by Galileo's atmospheric probe, which explored Jupiter's atmosphere directly.
As predicted beforehand, the collisions generated enormous waves which swept across the planet at speeds of 450 m/s (1,476 ft/s) and were observed for over two hours after the largest impacts. The waves were thought to be travelling within a stable layer acting as a waveguide, and some scientists believed the stable layer must lie within the hypothesised tropospheric water cloud. However, other evidence seemed to indicate that the cometary fragments had not reached the water layer, and the waves were instead propagating within the stratosphere.
Radio observations revealed a sharp increase in continuum emission at a wavelength of 21 cm after the largest impacts, which peaked at 120% of the normal emission from the planet. This was thought to be due to synchrotron radiation, caused by the injection of relativistic electrons – electrons with velocities near the speed of light – into the Jovian magnetosphere by the impacts.
About an hour after fragment K entered Jupiter, observers recorded auroral emission near the impact region, as well as at the antipode of the impact site with respect to Jupiter's strong magnetic field. The cause of these emissions was difficult to establish due to a lack of knowledge of Jupiter's internal magnetic field and of the geometry of the impact sites. One possible explanation was that upwardly accelerating shock waves from the impact accelerated charged particles enough to cause auroral emission, a phenomenon more typically associated with fast-moving solar wind particles striking a planetary atmosphere near a magnetic pole.
Some astronomers had suggested that the impacts might have a noticeable effect on the Io torus, a torus of high-energy particles connecting Jupiter with the highly volcanic moon Io. High resolution spectroscopic studies found that variations in the ion density, rotational velocity, and temperatures at the time of impact and afterwards were within the normal limits.
One of the surprises of the impacts was the small amount of water revealed compared to prior predictions. Before the impact, models of Jupiter's atmosphere had indicated that the break-up of the largest fragments would occur at atmospheric pressures of anywhere from 30 kilopascals to a few tens of megapascals (from 0.3 to a few hundred bar), with some predictions that the comet would penetrate a layer of water and create a bluish shroud over that region of Jupiter.
Astronomers did not observe large amounts of water following the collisions, and later impact studies found that fragmentation and destruction of the cometary fragments in an 'airburst' probably occurred at much higher altitudes than previously expected, with even the largest fragments being destroyed when the pressure reached , well above the expected depth of the water layer. The smaller fragments were probably destroyed before they even reached the cloud layer.
The visible scars from the impacts could be seen on Jupiter for many months. They were extremely prominent, and observers described them as more easily visible even than the Great Red Spot. A search of historical observations revealed that the spots were probably the most prominent transient features ever seen on the planet, and that while the Great Red Spot is notable for its striking color, no spots of the size and darkness of those caused by the SL9 impacts have ever been recorded before.
Spectroscopic observers found that ammonia and carbon disulfide persisted in the atmosphere for at least fourteen months after the collisions, with a considerable amount of ammonia being present in the stratosphere as opposed to its normal location in the troposphere.
Counterintuitively, the atmospheric temperature dropped to normal levels much more quickly at the larger impact sites than at the smaller sites: at the larger impact sites, temperatures were elevated over a region 15,000 to 20,000 km (9,300 to 12,400 mi) wide, but dropped back to normal levels within a week of the impact. At smaller sites, temperatures 10 K higher than the surroundings persisted for almost two weeks. Global stratospheric temperatures rose immediately after the impacts, then fell to below pre-impact temperatures 2–3 weeks afterwards, before rising slowly to normal temperatures.
Frequency of impacts
SL9 is not unique in having orbited Jupiter for a time; five comets, (including 82P/Gehrels, 147P/Kushida–Muramatsu, and 111P/Helin–Roman–Crockett) are known to have been temporarily captured by the planet. Cometary orbits around Jupiter are unstable, as they will be highly elliptical and likely to be strongly perturbed by the Sun's gravity at apojove (the furthest point on the orbit from the planet).
By far the most massive planet in the Solar System, Jupiter can capture objects relatively frequently, but the size of SL9 makes it a rarity: one post-impact study estimated that comets 0.3 km in diameter impact the planet once in approximately 500 years and those 1.6 km (0.99 mi) in diameter do so just once in every 6,000 years.
There is very strong evidence that comets have previously been fragmented and collided with Jupiter and its satellites. During the Voyager missions to the planet, planetary scientists identified 13 crater chains on Callisto and three on Ganymede, the origin of which was initially a mystery. Crater chains seen on the Moon often radiate from large craters, and are thought to be caused by secondary impacts of the original ejecta, but the chains on the Jovian moons did not lead back to a larger crater. The impact of SL9 strongly implied that the chains were due to trains of disrupted cometary fragments crashing into the satellites.
Impact of July 19, 2009
On July 19, 2009, a new black spot about the size of the Pacific Ocean appeared in Jupiter's southern hemisphere. Thermal infrared measurements showed the impact site was warm and spectroscopic analysis detected the production of excess hot ammonia and silica-rich dust in the upper regions of Jupiter's atmosphere. Scientists have concluded that another impact event had occurred, but this time a more compact and strong object, probably a small undiscovered asteroid, was the cause.
Jupiter as a "cosmic vacuum cleaner"
The impact of SL9 highlighted Jupiter's role as a "cosmic vacuum cleaner" (or in deference to the ancients' planetary correspondences to the major organs in the human body, a "cosmic liver") for the inner Solar System. The planet's strong gravitational influence leads to many small comets and asteroids colliding with the planet, and the rate of cometary impacts on Jupiter is thought to be between two thousand and eight thousand times higher than the rate on Earth. If Jupiter were not present, the probability of asteroid impacts with the Solar System's inner planets would be much greater.
The extinction of the dinosaurs at the end of the Cretaceous period is generally believed to have been caused by the Cretaceous–Paleogene impact event which created the Chicxulub crater, demonstrating that impacts are a serious threat to life on Earth. Astronomers have speculated that without Jupiter to mop up potential impactors, extinction events might have been more frequent on Earth, and complex life might not have been able to develop. This is part of the argument used in the Rare Earth hypothesis.
In 2009, it was shown that the presence of a smaller planet at Jupiter's position in the Solar System might increase the impact rate of comets on the Earth significantly. A planet of Jupiter's mass still seems to provide increased protection against asteroids, but the total effect on all orbital bodies within the Solar System is unclear.
- "Comet Shoemaker–Levy 9 Collision with Jupiter".
- "IAU 5725 circular". 1993.
- Marsden, Brian G. (July 18, 1997). "Eugene Shoemaker (1928–1997)".
- Marsden, Brian G. (March 26, 1993). "Comet Shoemaker–Levy (1993e)".
- Burton, Dan (July 1994). "What will be the effect of the collision?". Frequently Asked Questions about the Collision of Comet Shoemaker–Levy 9 with Jupiter.
- Landis, R.R. (1994). "Comet P/Shoemaker–Levy's Collision with Jupiter: Covering HST's Planned Observations from Your Planetarium". Proceedings of the International Planetarium Society Conference held at the Astronaut Memorial Planetarium & Observatory, Cocoa, Florida, July 10–16, 1994.
- "D/1993 F2 Shoemaker–Levy 9". Gary W. Kronk's Cometography. 1994. Retrieved August 8, 2008.
- Benner, L.A.; McKinnon, W. B. (March 1994). "Pre-Impact Orbital Evolution of P/Shoemaker–Levy 9". Abstracts of the 25th Lunar and Planetary Science Conference, held in Houston, TX, March 14–18, 1994 25: 93.
- Chapman, Clark R. (June 1993). "Comet on target for Jupiter". Nature 363 (6429): 492–493.
- Boehnhardt, H. (November 2004). "Split comets". In Michel C. Festou, H. Uwe Keller and Harold A. Weaver. Comets II. University of Arizona Press. p. 301.
- Bruton, Dan (July 1994). "Can I see the effects with my telescope?". Frequently Asked Questions about the Collision of Comet Shoemaker–Levy 9 with Jupiter.
- "Hubble Ultraviolet Image of Multiple Comet Impacts on Jupiter". News Release Number: STScI-1994-35. Hubble Space Telescope Comet Team. July 23, 1994. Retrieved November 12, 2014.
- Yeomans, D.K. (December 1993). "Periodic comet Shoemaker-Levy 9 (1993e)". IAU Circulars (Cambridge, Massachusetts: Smithsonian Astrophysical Observatory) 5909. Retrieved July 5, 2011.
- Williams, David R. "Ulysses and Voyager 2". Lunar and Planetary Science.
- Martin, Terry Z. (September 1996). "Shoemaker–Levy 9: Temperature, Diameter and Energy of Fireballs". Bulletin of the American Astronomical Society 28: 1085.
- Weissman, P.R.; Carlson, R. W.; Hui, J.; Segura, M.; Smythe, W. D.; Baines, K. H.; Johnson, T. V.; Drossart, P.; Encrenaz, T. et al. (March 1995). "Galileo NIMS Direct Observation of the Shoemaker–Levy 9 Fireballs and Fall Back". Abstracts of the Lunar and Planetary Science Conference 26: 1483.
- Hammel, H.B. (December 1994). "The Spectacular Swan Song of Shoemaker–Levy 9". 185th AAS Meeting 26. American Astronomical Society. p. 1425.
- Bruton, Dan (February 1996). "What were some of the effects of the collisions?". Frequently Asked Questions about the Collision of Comet Shoemaker–Levy 9 with Jupiter.
- Yeomans, Don; Chodas, Paul (March 18, 1995). "Comet Crash Impact Times Request".
- Noll, K.S.; McGrath, MA; Trafton, LM; Atreya, SK; Caldwell, JJ; Weaver, HA; Yelle, RV; Barnet, C; Edgington, S (March 1995). "HST Spectroscopic Observations of Jupiter Following the Impact of Comet Shoemaker–Levy 9". Science 267 (5202): 1307–1313.
- Hu, Zhong-Wei; Chu, Yi; Zhang, Kai-Jun (May 1996). "On Penetration Depth of the Shoemaker–Levy 9 Fragments into the Jovian Atmosphere". Earth, Moon and Planets 73 (2): 147–155.
- Ingersoll, A. P.; Kanamori, H (April 1995). "Waves from the collisions of comet Shoemaker–Levy 9 with Jupiter". Nature 374 (6524): 706–708.
- Olano, C. A. (August 1999). "Jupiter's Synchrotron Emission Induced by the Collision of Comet Shoemaker–Levy 9".
- Bauske, Rainer; Combi, Michael R.; Clarke, John T. (November 1999). "Analysis of Midlatitude Auroral Emissions Observed during the Impact of Comet Shoemaker–Levy 9 with Jupiter".
- Hockey, T.A. (1994). "The Shoemaker–Levy 9 Spots on Jupiter: Their Place in History". Earth, Moon and Planets 66 (1): 1–9.
- McGrath, M.A.; Yelle, R. V.; Betremieux, Y. (September 1996). "Long-term Chemical Evolution of the Jupiter Stratosphere Following the SL9 Impacts". Bulletin of the American Astronomical Society 28: 1149.
- Bézard, B. (October 1997). "Long-term Response of Jupiter's Thermal Structure to the SL9 Impacts". Planetary and Space Science 45 (10): 1251–1271.
- Moreno, R.; Marten, A; Biraud, Y; Bézard, B; Lellouch, E; Paubert, G; Wild, W (June 2001). "Jovian Stratospheric Temperature during the Two Months Following the Impacts of Comet Shoemaker–Levy 9". Planetary and Space Science 49 (5): 473–486.
- Ohtsuka, Katsuhito; Ito, T.; Yoshikawa, M.; Asher, D. J.; Arakida, H. (October 2008). "Quasi-Hilda comet 147P/Kushida–Muramatsu. Another long temporary satellite capture by Jupiter". Astronomy and Astrophysics 489 (3): 1355–1362.
- Tancredi, G.; Lindgren, M.; Rickman, H. (November 1990). "Temporary Satellite Capture and Orbital Evolution of Comet P/Helin–Roman–Crockett".
- Roulston, M.S.; Ahrens, T (March 1997). "Impact Mechanics and Frequency of SL9-Type Events on Jupiter".
- Schenk, Paul M.; Asphaug, Erik; McKinnon, William B.; Melosh, H. J.; Weissman, Paul R. (June 1996). "Cometary Nuclei and Tidal Disruption: The Geologic Record of Crater Chains on Callisto and Ganymede".
- Greeley, R.; Klemaszewski, J.E.; Wagner, R.; the Galileo Imaging Team (2000). "Galileo views of the geology of Callisto". Planetary and Space Science 48 (9): 829–853.
- Mystery impact leaves Earth-sized mark on Jupiter
- Nakamura, T.; Kurahashi, H. (February 1998). "Collisional Probability of Periodic Comets with the Terrestrial Planets – an Invalid Case of Analytic Formulation". Astronomical Journal 115 (2): 848.
- "Images of Chicxulub Crater". NASA/JPL Near-Earth Object Program Office. August 22, 2005. Retrieved July 21, 2009.
- Jupiter – friend or foe? II: the Centaurs Jupiter http://arxiv.org/pdf/0903.3305
- Horner, J.; Jones, B.W. (July 2008). "Jupiter – friend or foe? I: The asteroids".
- Chodas P. W., and Yeomans D. K. (1996), The Orbital Motion and Impact Circumstances of Comet Shoemaker–Levy 9, in The Collision of Comet Shoemaker–Levy 9 and Jupiter, edited by K. S. Noll, P. D. Feldman, and H. A. Weaver, Cambridge University Press, pp. 1–30
- Chodas P. W. (2002), Communication of Orbital Elements to Selden E. Ball, Jr. Accessed February 21, 2006
- Comet Shoemaker–Levy 9 FAQ
- Comet Shoemaker–Levy 9 Photo Gallery
- Downloadable gif Animation showing time course of impact and size relative to earthsize
- Jupiter Swallows Comet Shoemaker Levy 9
- Comet Shoemaker–Levy Collision with Jupiter
- National Space Science Data Center information
- Simulation of the orbit of SL-9 showing the passage that fragmented the comet and the collision 2 years later
- YouTube video animation of impact
- Interactive space simulator that includes accurate 3D simulation of the Shoemaker Levy 9 collision