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The Crystal Structures and Powder Diffraction Patterns of the Uranium Tellurides: A Critical Review
- Robert L. Snyder, Monte C. Nichols, Dale R. Boehme
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- Journal:
- Powder Diffraction / Volume 6 / Issue 4 / December 1991
- Published online by Cambridge University Press:
- 10 January 2013, pp. 204-227
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A critical review of all the reported structures and powder diffraction patterns in the uranium telluride system has been undertaken. Our recommendations are:
1. Structures that are correct:
• Cubic – UTe: no experimental pattern exists. Retain calculated 15–865.
• Cubic – U3Te4: retain poor quality 12-610 but adopt the pattern calculated here.
• Cubic U2Te3: no experimental pattern exists. Adopt pattern calculated here.
• Orthorhombic UTe2: Adopt the new pattern of Boehme et al.
• Monoclinic αUTe3: Adopt the new pattern of Boehme et al.
• Orthorhombic βUTe3: Adopt the pattern calculated here.
• Orthorhombic UTe5: Adopt the new pattern of Boeheme et al.
2. Structures in need of refinement:
• Orthorhombic U2Te3: Adopt pattern calculated here over 34-807.
• Hexagonal U7Te12: Adopt pattern calculated here but retain 24-1368.
• Orthorhombic UTe1.78: Adopt pattern calculated here and retain our modified 21-1404 reported for U4Te7.
• Orthorhombic UTe2.5: Adopt pattern calculated here.
• Orthorhombic UTe3.4: Accept recent pattern of Boehme et al.
3. Phases for which no structures or reliable patterns exist:
• Orthorhombic U3Te4: no published pattern.
• Tetragonal U3Te5: three patterns 21-1407, 34-766 and 34-896 exist but all are of very poor quality.
4. Phases which probably do not exist:
• Tetragonal UTe1.77
• Tetragonal UTe2
• Cubic UTe2
• U3Te7 (21-1402)
• U3Te8 (21-1406)
The science of EChO
- Giovanna Tinetti, James Y-K. Cho, Caitlin A. Griffith, Olivier Grasset, Lee Grenfell, Tristan Guillot, Tommi T. Koskinen, Julianne I. Moses, David Pinfield, Jonathan Tennyson, Marcell Tessenyi, Robin Wordsworth, Alan Aylward, Roy van Boekel, Angioletta Coradini, Therese Encrenaz, Ignas Snellen, Maria R. Zapatero-Osorio, Jeroen Bouwman, Vincent Coudé du Foresto, Mercedes Lopez-Morales, Ingo Mueller-Wodarg, Enric Pallé, Franck Selsis, Alessandro Sozzetti, Jean-Philippe Beaulieu, Thomas Henning, Michael Meyer, Giuseppina Micela, Ignasi Ribas, Daphne Stam, Mark Swain, Oliver Krause, Marc Ollivier, Emanuele Pace, Bruce Swinyard, Peter A.R. Ade, Nick Achilleos, Alberto Adriani, Craig B. Agnor, Cristina Afonso, Carlos Allende Prieto, Gaspar Bakos, Robert J. Barber, Michael Barlow, Peter Bernath, Bruno Bézard, Pascal Bordé, Linda R. Brown, Arnaud Cassan, Céline Cavarroc, Angela Ciaravella, Charles Cockell, Athéna Coustenis, Camilla Danielski, Leen Decin, Remco De Kok, Olivier Demangeon, Pieter Deroo, Peter Doel, Pierre Drossart, Leigh N. Fletcher, Matteo Focardi, Francois Forget, Steve Fossey, Pascal Fouqué, James Frith, Marina Galand, Patrick Gaulme, Jonay I. González Hernández, Davide Grassi, Matt J. Griffin, Ulrich Grözinger, Manuel Guedel, Pactrick Guio, Olivier Hainaut, Robert Hargreaves, Peter H. Hauschildt, Kevin Heng, David Heyrovsky, Ricardo Hueso, Pat Irwin, Lisa Kaltenegger, Patrick Kervella, David Kipping, Geza Kovacs, Antonino La Barbera, Helmut Lammer, Emmanuel Lellouch, Giuseppe Leto, Mercedes Lopez Morales, Miguel A. Lopez Valverde, Manuel Lopez-Puertas, Christophe Lovi, Antonio Maggio, Jean-Pierre Maillard, Jesus Maldonado Prado, Jean-Baptiste Marquette, Francisco J. Martin-Torres, Pierre Maxted, Steve Miller, Sergio Molinari, David Montes, Amaya Moro-Martin, Olivier Mousis, Napoléon Nguyen Tuong, Richard Nelson, Glenn S. Orton, Eric Pantin, Enzo Pascale, Stefano Pezzuto, Ennio Poretti, Raman Prinja, Loredana Prisinzano, Jean-Michel Réess, Ansgar Reiners, Benjamin Samuel, Jorge Sanz Forcada, Dimitar Sasselov, Giorgio Savini, Bruno Sicardy, Alan Smith, Lars Stixrude, Giovanni Strazzulla, Gautam Vasisht, Sandrine Vinatier, Serena Viti, Ingo Waldmann, Glenn J. White, Thomas Widemann, Roger Yelle, Yuk Yung, Sergey Yurchenko
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- Journal:
- Proceedings of the International Astronomical Union / Volume 6 / Issue S276 / October 2010
- Published online by Cambridge University Press:
- 10 November 2011, pp. 359-370
- Print publication:
- October 2010
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The science of extra-solar planets is one of the most rapidly changing areas of astrophysics and since 1995 the number of planets known has increased by almost two orders of magnitude. A combination of ground-based surveys and dedicated space missions has resulted in 560-plus planets being detected, and over 1200 that await confirmation. NASA's Kepler mission has opened up the possibility of discovering Earth-like planets in the habitable zone around some of the 100,000 stars it is surveying during its 3 to 4-year lifetime. The new ESA's Gaia mission is expected to discover thousands of new planets around stars within 200 parsecs of the Sun. The key challenge now is moving on from discovery, important though that remains, to characterisation: what are these planets actually like, and why are they as they are?
In the past ten years, we have learned how to obtain the first spectra of exoplanets using transit transmission and emission spectroscopy. With the high stability of Spitzer, Hubble, and large ground-based telescopes the spectra of bright close-in massive planets can be obtained and species like water vapour, methane, carbon monoxide and dioxide have been detected. With transit science came the first tangible remote sensing of these planetary bodies and so one can start to extrapolate from what has been learnt from Solar System probes to what one might plan to learn about their faraway siblings. As we learn more about the atmospheres, surfaces and near-surfaces of these remote bodies, we will begin to build up a clearer picture of their construction, history and suitability for life.
The Exoplanet Characterisation Observatory, EChO, will be the first dedicated mission to investigate the physics and chemistry of Exoplanetary Atmospheres. By characterising spectroscopically more bodies in different environments we will take detailed planetology out of the Solar System and into the Galaxy as a whole.
EChO has now been selected by the European Space Agency to be assessed as one of four M3 mission candidates.
34 - Pediatric Seizures
- from SECTION V - PEDIATRIC NEUROLOGICAL EMERGENCIES
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- By Mont R. Roberts, Sparrow Healthcare System Sparow Hospital/MSU Emergency Medicine Residency Program Lansing, Michigan, Rae R. Hanson, Midelfort Clinic Eau Claire, Wisconsin
- Edited by Sid M. Shah, Michigan State University, Kevin M. Kelly, Drexel University, Philadelphia
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- Book:
- Principles and Practice of Emergency Neurology
- Published online:
- 06 August 2009
- Print publication:
- 18 February 2003, pp 337-349
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Summary
The average age of childhood status epilepticus (SE) is under 3 years old. The acute management requires a planned treatment schedule and a specific time line. The duration of SE is the greatest risk to the patient; the longer SE lasts, the more difficult it is to treat. The three goals of treatment are to control seizures, to preserve vital functions, and to diagnose the underlying pathology. Absence SE, partial absence SE, or complex partial SE may present as nonconvulsive SE. Neonatal seizures occur in patients under 29 days old, and they are usually related to significant neurological disease. Pediatric patients are unique in that several characteristic epileptic syndromes have an age-dependent appearance, one or more characteristic seizure types, a natural history, and a prognosis. Some major syndromes include febrile seizures, infantile spasms, Lennox-Gastaut syndrome, and benign rolandic epilepsy (BRE).
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