Dean Cain Bettina Zimmermann

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DEAN CAIN BETTINA ZIMMERMANN POST IMPACT POST IMPACT In 2012, a meteor crashes into tion plane to Europe is destroyed Siberia with the force of several by a mysterious satellite signal, thousand nuclear warheads. In controlled from the ruins of Berlin, 2015, a few survivors will travel a city that was considered dead into “the death zone”, to try and and buried – under 30 feet of ice locate a device that could give and snow – the President of the mankind new hope – or forever New United Northern Sates orders finish it… a new expedition to find and destroy the base and the satellite. In 2012, a meteor strikes Earth, Tom Parker (Dean Cain) volunteers causing earthquakes, tidal waves, to lead a group of highly trained and a dust cloud that soon covers specialists on a suicide mission most of the Northern hemisphere, to Berlin – with ground vehicles, turning it into an ice-covered no reliable intel, and zero radio “death-zone”. contact. Three years later, most of the sur- In the ruins of what was once one vivors have settled in the only hab- of the most dynamic cities in itable territories below the equa- Europe, a desperate fight ensues tor. It’s a harsh life, with little hope for the power to change every- of Earth’s climate ever reverting thing – for better or for worse… back to normal. When an expedi- POST IMPACT SNOWBLIND LLC presents a TANDEM PRODUCTIONS GMBH, UFO IPS LLC in co-production with LUCKY 7 PRODUCTIONS LLC and AMERICAN FILM CINEMA in association with RTL TELEVISION GMBH and THE TOWER LIMITED LIABILITY PARTNERSHIP Production • “POST IMPACT” starring DEAN CAIN, BETTINA ZIMMERMANN, NIGEL BENNETT, JOANNA TAYLOR, JOHN KEOGH and HANS ZISCHLER Associate Producers TJ SAKASEGAWA, JOHN CAPPILLA, JEFF RANK and TORSTEN DEWI Production Designer SVETLANA ‘KES’ BONNET • Visual Effects Director RYAN ‘SPIKE’ DAUNER Director of Special Effects KEVIN GENERAU • Director of Photography LORENZO SENATORE Executive Producer ROLA BAUER, ANTONY BLAKEY and PHILIPPE MARTINEZ Co-Produced By PHILLIP ROTH, TIM HALKIN, JEFFERY BEACH and ALAN LATHAM Written By TORSTEN DEWI and CARLOS MARIA SANCHEZ Directed By CHRISTOPH SCHREWE *credits not contractual Distributed by: Sonnenstrasse 14, 80331 Munich, Germany Phone +49 (89) 96 22 83 00 [email protected] www.studiocanaltvseries.com In association with.

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Cross-References ASTEROID IMPACT Definition and Introduction History of Impact Cratering Studies
18 ASTEROID IMPACT Tedesco, E. F., Noah, P. V., Noah, M., and Price, S. D., 2002. The identification and confirmation of impact structures on supplemental IRAS minor planet survey. The Astronomical Earth were developed: (a) crater morphology, (b) geo- 123 – Journal, , 1056 1085. physical anomalies, (c) evidence for shock metamor- Tholen, D. J., and Barucci, M. A., 1989. Asteroid taxonomy. In Binzel, R. P., Gehrels, T., and Matthews, M. S. (eds.), phism, and (d) the presence of meteorites or geochemical Asteroids II. Tucson: University of Arizona Press, pp. 298–315. evidence for traces of the meteoritic projectile – of which Yeomans, D., and Baalke, R., 2009. Near Earth Object Program. only (c) and (d) can provide confirming evidence. Remote Available from World Wide Web: http://neo.jpl.nasa.gov/ sensing, including morphological observations, as well programs. as geophysical studies, cannot provide confirming evi- dence – which requires the study of actual rock samples. Cross-references Impacts influenced the geological and biological evolu- tion of our own planet; the best known example is the link Albedo between the 200-km-diameter Chicxulub impact structure Asteroid Impact Asteroid Impact Mitigation in Mexico and the Cretaceous-Tertiary boundary. Under- Asteroid Impact Prediction standing impact structures, their formation processes, Torino Scale and their consequences should be of interest not only to Earth and planetary scientists, but also to society in general. ASTEROID IMPACT History of impact cratering studies In the geological sciences, it has only recently been recog- Christian Koeberl nized how important the process of impact cratering is on Natural History Museum, Vienna, Austria a planetary scale.
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Mercurian Impact Ejecta: Meteorites and Mantle
Meteoritics & Planetary Science 44, Nr 2, 285–291 (2009) Abstract available online at http://meteoritics.org Mercurian impact ejecta: Meteorites and mantle Brett GLADMAN* and Jaime COFFEY University of British Columbia, Department of Physics and Astronomy, 6244 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada *Corresponding author. E-mail: [email protected] (Submitted 28 January 2008; revision accepted 15 October2008) Abstract–We have examined the fate of impact ejecta liberated from the surface of Mercury due to impacts by comets or asteroids, in order to study 1) meteorite transfer to Earth, and 2) reaccumulation of an expelled mantle in giant-impact scenarios seeking to explain Mercury’s large core. In the context of meteorite transfer during the last 30 Myr, we note that Mercury’s impact ejecta leave the planet’s surface much faster (on average) than other planets in the solar system because it is the only planet where impact speeds routinely range from 5 to 20 times the planet’s escape speed; this causes impact ejecta to leave its surface moving many times faster than needed to escape its gravitational pull. Thus, a large fraction of Mercurian ejecta may reach heliocentric orbit with speeds sufficiently high for Earth-crossing orbits to exist immediately after impact, resulting in larger fractions of the ejecta reaching Earth as meteorites. We calculate the delivery rate to Earth on a time scale of 30 Myr (typical of stony meteorites from the asteroid belt) and show that several percent of the high-speed ejecta reach Earth (a factor of 2–3 less than typical launches from Mars); this is one to two orders of magnitude more efficient than previous estimates.
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Post-Impact Hydrothermal Activity in Meteorite Impact Craters and Potential Opportunities for Life
Bioastronomy 2002: Life Among the Stars IAU Symposium, Vol. 213, 2004 R.P.Norris and F.H.Stootman (eds.) Post-Impact Hydrothermal Activity in Meteorite Impact Craters and Potential Opportunities for Life Christian Koeberl Department of Geological Sciences, University of Vienna, Althanstrasse 14, A-1090 Vienna, Austria, [email protected] Wolf Uwe Reimold Impact Cratering Research Group, School of Geosciences, University of the Witwatersrand, Johannesburg 2050, South Africa, [email protected] Abstract. Impact craters are prominent landforms on all objects with a solid surface in the solar system. The formation of an impact structure is a high-energy, high-temperature transient event which introduces large amounts of energy into a limited area. This energy can, in part, be expanded on the creation and activation of a hydrothermal system within and even outside of the crater. Depending on the crater size and geology of the target region, this hydrothermal system may persist for extended periods of time. Such impact-induced hydrothermal systems could well have provided conditions supportive of the development of life on the early Earth and it is not unreasonable to assume that similar conditions could have led to life-favoring circumstances on other planets and satellites. 1. Introduction Studies during the last few decades have convinced most workers that the planets formed by collision and hierarchical growth starting from small objects, Le., from dust to planetesimals to planets. All planets and satellites of the solar system that have solid surfaces (e.g., Mercury, Venus, Mars, the asteroids) are covered by craters. Impact cratering has been either the most important, or one of the most important processes that affected the shaping of their surfaces.
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Facts, Theories and Further Questions Around the Ries-Steinheim Simultaneous Impact Event: a Review
40th Lunar and Planetary Science Conference (2009) 1542.pdf FACTS, THEORIES AND FURTHER QUESTIONS AROUND THE RIES-STEINHEIM SIMULTANEOUS IMPACT EVENT: A REVIEW. K. Mihályi1, A. Gucsik2,3, J. Szabó1, Sz. Bérczi4. 1University of Debrecen, Department of Physical Geography and Geoinformatics, H-4032 Debrecen, Egyetem tér 1., Hungary, P.O. box 9., email: [email protected]; 2Max Planck Institute for Chemistry, Department of Geochemistry, D-55020 Mainz, Germany; 3Savaria University Center, University of West of Hungary, Károlyi Gáspár tér 4., H-9700, Szombathely, Hungary; 4Eötvös University, Faculty of Science, Institute of Physics, Department of Materials Physics, H-1117 Budapest, Pázmány Péter sétány 1/a, Hungary Introduction: Nördlingen-Ries impact structure event. However, Steinheim structure hasn’t such well (Germany, Bavaria) is one of the best known terrestrial preserved distal ejecta remnants, but assuming some impact structures. Steinheim meteorite crater (often kind of linking between meteorites formed Ries and called Steinheim-basin) is located ~40 km from Ries, Steinheim (as mentioned above), angle and direction of in the southwestern direction. Diameter of Ries is impact must be similar to Ries. Stöffler et al. [1] found about 24 km, Steinheim is about 3.8 km. Their age is 30-45° for ideal impact angle to produce Ries-type the same: 15.1 million years [1,2], which is a key-point tektite (moldavite) strewn-field. for these two impact forms: it is strongly suggested not Binary asteroid or broken-up asteroid? Speaking about ’some kind’ of relationship between impacting only the occurrence of simultaneous (or nearly meteorites during double-impact, there are two simultaneous) impact, but also some kind of possible ways: (1) the asteroids were formed relationship between parental meteorites of these two separately, but later the smaller became satellite- craters (because chance of simultaneous impact of two asteroid of the bigger one, captured by gravitational meteorites in such a small area, without any linking or forces.
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Planetary Defense Final Report I
Team Project - Planetary Defense Final Report i Team Project - Planetary Defense Final Report ii Team Project - Planetary Defense Cover designed by: Tihomir Dimitrov Images courtesy of: Earth Image - NASA US Geological Survey Detection Image - ESA's Optical Ground Station Laser Tags ISS Deflection Image - IEEE Space Based Lasers Collaboration Image - United Nations General Assembly Building Outreach Image - Dreamstime teacher with students in classroom Evacuation Image - Libyan City of Syrte destroyed in 2011 Shield Image - Silver metal shield PNG image The cover page was designed to include a visual representation of the roadmap for a robust Planetary Defense Program that includes five elements: detection, deflection, global collaboration, outreach, and evacuation. The shield represents the idea of defending our planet, giving confidence to the general public that the Planetary Defense elements are reliable. The orbit represents the comet threat and how it is handled by the shield, which represents the READI Project. The curved lines used in the background give a sense of flow representing the continuation and further development for Planetary Defense programs after this team project, as we would like for everyone to be involved and take action in this noble task of protecting Earth. The 2015 Space Studies Program of the International Space University was hosted by the Ohio University, Athens, Ohio, USA. While all care has been taken in the preparation of this report, ISU does not take any responsibility for the accuracy of its content.
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SOFIA Infrared Spectrophotometry of Comet C/2012 K1 (Pan-STARRS)
ApJ Accepted 2015.July.22 SOFIA Infrared Spectrophotometry of Comet C/2012 K1 (Pan-STARRS) Charles E. Woodward1, Michael S. P. Kelley2, David E. Harker3, Erin L. Ryan2, Diane H. Wooden4, Michael L. Sitko5, Ray W. Russell6, William T. Reach7, Imke de Pater8, Ludmilla Kolokolova2, Robert D. Gehrz9 ABSTRACT We present pre-perihelion infrared 8 to 31 µm spectrophotometric and imaging observations of comet C/2012 K1 (Pan-STARRS), a dynamically new Oort Cloud comet, conducted with NASA’s Stratospheric Observatory for Infrared Astronomy (SOFIA) facility (+FORCAST) in 2014 June. As a “new” comet (first inner solar system passage), the coma grain population may be extremely pristine, unencumbered by a rime and insufficiently irradiated by the Sun to carbonize its surface organics. The comet exhibited a weak 10 µm silicate feature ≃ 1.18 ± 0.03 above the underlying best-fit 215.32 ± 0.95 K continuum blackbody. Thermal modeling of the observed spectral energy distribution indicates that the coma grains are fractally solid with a porosity factor D = 3 and the peak in the grain size distribution, apeak = 0.6 µm, 1Minnesota Institute for Astrophysics, University of Minnesota, 116 Church St, SE Minneapolis, MN 55455, USA; [email protected] 2University of Maryland, Department of Astronomy, College Park, MD 20742-2421, USA arXiv:1508.00288v1 [astro-ph.EP] 2 Aug 2015 3University of California, San Diego, Center for Astrophysics & Space Sciences, 9500 Gilman Dr. Dept 0424, La Jolla, CA 92093-0424, USA 4NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035-0001, USA 5Department of Physics, University of Cincinnati, Cincinnati, OH 45221, USA 6The Aerospace Corporation, Los Angeles, CA 90009, USA 7USRA-SOFIA Science Center, NASA Ames Research Center, Moffett Field, CA 94035, USA 8Astronomy Department, 601 Campbell Hall, University of California, Berkeley, CA 94720, USA 9Minnesota Institute for Astrophysics, University of Minnesota, 116 Church St, SE Minneapolis, MN 55455, USA –2– large.
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The Impact-Origin of Life Hypothesis
Development of a Concept: The Inner Solar System Impact Cataclysm Hypothesis & The Impact-Origin of Life Hypothesis The Chicxulub impact event and its link to the Cretaceous-Tertiary (K/T) boundary mass extinction event (e.g., Kring et al., 1991; Hildebrand et al., 1991; Kring and Boynton, 1992) demonstrates that impact cratering can affect both the geologic and biologic evolution of a planet as proposed by Nobel-winning L. Alvarez and others. This has led scientists to wonder if impact cratering may have affected the evolution of life at other times. For example, several teams, including one led by Dr. Kring, have been examining the causes of two of the other “big five” mass extinction events on Earth at the Permian- Triassic (P/T) and Triassic-Jurassic (T/J) boundaries. Pushing farther back in time, Dr. Kring has also been examining the earliest impact events to affect Earth to determine if impact cratering may have affected the origin and early evolution of life. Previous Apollo-era analyses suggested the Moon was severely bombarded ~3.9 billion years ago, leading to the concept of a lunar cataclysm. As summarized below, Dr. Kring and his colleagues have been testing this hypothesis and finding that new evidence supports the idea that the Moon was severely bombarded nearly 4 billion years ago. He has also argued that this impact cataclysm affected Earth and all other inner solar system planetary surfaces, a concept now known as the inner solar system impact cataclysm hypothesis. He further suggests that the impact events delivered biogenic elements and, more importantly, created subsurface hydrothermal systems that were crucibles for pre-biotic chemistry and provided habitats for the early evolution of life, a new concept that he has called the impact-origin of life hypothesis.
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Post-Impact Structural Crater Modification Due to Sediment Loading: an Overlooked Process
Meteoritics & Planetary Science 42, Nr 11, 2013–2029 (2007) Abstract available online at http://meteoritics.org Post-impact structural crater modification due to sediment loading: An overlooked process Filippos TSIKALAS†* and Jan Inge FALEIDE2 Department of Geosciences, University of Oslo, P.O. Box 1047 Blindern, NO-0316 Oslo, Norway †Present address: ENI Norge AS, P.O. Box 101 Forus, NO-4064 Stavanger, Norway *Corresponding author. E-mail: [email protected]; [email protected] (Received 02 November 2006; revision accepted 16 February 2007) Abstract–Post-impact crater morphology and structure modifications due to sediment loading are analyzed in detail and exemplified in five well-preserved impact craters: Mjølnir, Chesapeake Bay, Chicxulub, Montagnais, and Bosumtwi. The analysis demonstrates that the geometry and the structural and stratigraphic relations of post-impact strata provide information about the amplitude, the spatial distribution, and the mode of post-impact deformation. Reconstruction of the original morphology and structure for the Mjølnir, Chicxulub, and Bosumtwi craters demonstrates the long-term subsidence and differential compaction that takes place between the crater and the outside platform region, and laterally within the crater structure. At Mjølnir, the central high developed as a prominent feature during post-impact burial, the height of the peak ring was enhanced, and the cumulative throw on the rim faults was increased. The original Chicxulub crater exhibited considerably less prominent peak- ring and inner-ring/crater-rim features than the present crater. The original relief of the peak ring was on the order of 420–570 m (currently 535–575 m); the relief on the inner ring/crater rim was 300– 450 m (currently ∼700 m).
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Post-Impact Depositional Environments As a Proxy for Crater Morphology, Late Devonian Alamo Impact, Nevada
Crater morphology of the Late Devonian Alamo impact, Nevada Post-impact depositional environments as a proxy for crater morphology, Late Devonian Alamo impact, Nevada Andrew J. Retzler1,†,*, Leif Tapanila1,2,*, Julia R. Steenberg3,*, Carrie J. Johnson4,*, and Reed A. Myers5,* 1Department of Geosciences, Idaho State University, 921 South 8th Avenue, Pocatello, Idaho 83209-8072, USA 2Division of Earth Science, Idaho Museum of Natural History, 921 South 8th Avenue, Pocatello, Idaho 83209-8096, USA 3Minnesota Geological Survey, 2642 University Avenue W., St. Paul, Minnesota 55114-1032, USA 4Chesapeake Energy Corporation, Building 05, Offi ce 249, 6001 North Classen Boulevard, Oklahoma City, Oklahoma 73118, USA 5Department of Earth and Atmospheric Sciences, 1-26 Earth Sciences Building, University of Alberta, Edmonton, Alberta T6G2E3, Canada ABSTRACT INTRODUCTION as expected for marine bolide impacts (Dypvik and Jansa, 2003; Dypvik and Kalleson, 2010). Marine facies of carbonate and siliciclas- Marine bolide impact events are under- Estimates of the fi nal crater diameter have relied tic sediments deposited on top of the upper represented in the rock record due to their low exclusively on the extent and composition of the Devonian Alamo Breccia Member identify preservation potential. Consequently, few stud- Alamo Breccia Member and not on geomorphic the shape and size of the Alamo impact cra- ies exist documenting marine impact crater size, features specifi c to marine impact craters. ter in south-central Nevada (western USA). morphology, and effects on sedimentation pat- The aim of this paper is to interpret crater There are 13 measured sections that record terns; of the 27 known marine impact craters on morphology based on post-impact deposi- peritidal to deep-subtidal deposition across Earth, 20 of them are currently located on land tional environments in the context of a regional the impacted platform, and these are corre- (Dypvik and Jansa, 2003).
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Arxiv:2007.05407V1 [Astro-Ph.EP] 10 Jul 2020 Carlo Approaches
Use of the Semilinear Method to predict the Impact Corridor on Ground L. Dimarea, A. Del Vignaa,b, D. Bracali Ciocia, F. Bernardia aSpace Dynamics Services s.r.l., via Mario Giuntini, Navacchio di Cascina, Pisa, Italy bDipartimento di Matematica, Universitàdi Pisa, Largo Bruno Pontecorvo 5, Pisa, Italy Abstract We propose an adaptation of the semilinear algorithm for the prediction of the impact corridor on ground of an Earth- impacting asteroid. The proposed algorithm provides an efficient tool, able to reliably predict the impact regions at fixed altitudes above ground with 5 orders of magnitudes less computations than Monte Carlo approaches. Efficiency is crucial when dealing with imminent impactors, which are characterized by high impact probabilities and impact times very close to the times of discovery. The case of 2008 TC3 is a remarkable example, but there are also recent cases of imminent impactors, 2018 LA and 2019 MO, for which the method has been successfully used. Moreover, its good performances make the tool suitable also for the analysis of the impact regions on ground of objects with a more distant impact time, even of the order of many years, as confirmed by the test performed with the first batch of observations of Apophis, giving the possibility of an impact 25 years after its discovery. Keywords: Near-Earth Asteroid, Impact Monitoring, Semilinear Method, Impact Corridor 1. Introduction The semilinear algorithm was first introduced in Milani (1999) for the recovery of lost asteroids. The aim was to have an efficient algorithm to determine an approximation of the boundary of the recovery region on the sky plane where the asteroid is supposed to be found at a given time.
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