Developing an Interactive Space Simulation Game Featuring Procedural Content Generation
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Glossary - Cellbiology
1 Glossary - Cellbiology Blotting: (Blot Analysis) Widely used biochemical technique for detecting the presence of specific macromolecules (proteins, mRNAs, or DNA sequences) in a mixture. A sample first is separated on an agarose or polyacrylamide gel usually under denaturing conditions; the separated components are transferred (blotting) to a nitrocellulose sheet, which is exposed to a radiolabeled molecule that specifically binds to the macromolecule of interest, and then subjected to autoradiography. Northern B.: mRNAs are detected with a complementary DNA; Southern B.: DNA restriction fragments are detected with complementary nucleotide sequences; Western B.: Proteins are detected by specific antibodies. Cell: The fundamental unit of living organisms. Cells are bounded by a lipid-containing plasma membrane, containing the central nucleus, and the cytoplasm. Cells are generally capable of independent reproduction. More complex cells like Eukaryotes have various compartments (organelles) where special tasks essential for the survival of the cell take place. Cytoplasm: Viscous contents of a cell that are contained within the plasma membrane but, in eukaryotic cells, outside the nucleus. The part of the cytoplasm not contained in any organelle is called the Cytosol. Cytoskeleton: (Gk. ) Three dimensional network of fibrous elements, allowing precisely regulated movements of cell parts, transport organelles, and help to maintain a cell’s shape. • Actin filament: (Microfilaments) Ubiquitous eukaryotic cytoskeletal proteins (one end is attached to the cell-cortex) of two “twisted“ actin monomers; are important in the structural support and movement of cells. Each actin filament (F-actin) consists of two strands of globular subunits (G-Actin) wrapped around each other to form a polarized unit (high ionic cytoplasm lead to the formation of AF, whereas low ion-concentration disassembles AF). -
Model Optimization for Deep Space Exploration Via Simulators and Deep Learning
Model Optimization for Deep Space Exploration via Simulators and Deep Learning James Bird1,∗, Kellan Colburn2,∗, Linda Petzold1, Philip Lubin2 Abstract Machine learning, and eventually true artificial intelligence techniques, are extremely im- portant advancements in astrophysics and astronomy. We explore the application of deep learning using neural networks in order to automate the detection of astronomical bodies for future exploration missions, such as missions to search for signatures or suitability of life. The ability to acquire images, analyze them, and send back those that are important, as determined by the deep learning algorithm, is critical in bandwidth-limited applications. Our previous foundational work solidified the concept of using simulator images and deep learning in order to detect planets. Optimization of this process is of vital importance, as even a small loss in accuracy might be the difference between capturing and completely missing a possibly-habitable nearby planet. Through computer vision, deep learning, and simulators we introduce methods that optimize the detection of exoplanets. We show that maximum achieved accuracy can hit above 98% for multiple model architectures, even with a relatively small training set. Keywords: computer vision, simulator, deep learning, space, universe, exoplanet, object detection, novelty detection, neural network, machine learning, transfer learning, interstellar travel, planet detection 1. Introduction This paper will address some of the challenges and possibilities of exoplanet -
Solar System Simulator NASA SUMMER of INNOVATION
National Aeronautics and Space Administration Solar System Simulator NASA SUMMER OF INNOVATION UNIT Earth and Space Science – Year of the Solar System DESCRIPTION This online software generates views of GRADE LEVELS the bodies of our planetary system at any th th 7 – 9 date from any artificial or natural point of observation. CONNECTION TO CURRICULUM Science and technology OBJECTIVES TEACHER PREPARATION TIME Students will: 1 hour • Investigate how to determine the relative position of the sun, LESSON TIME NEEDED planets, and a number of 30 minutes Complexity: Basic planetary spacecraft using a simple web-based program • Explore how planets change their position in space over time NATIONAL STANDARDS National Science Education Standards (NSTA) Science and Technology Standards • Abilities of technological design • Understanding about science and technology Earth and Space Science • Earth in the solar system • Objects in the sky Common Core State Standards for Mathematics (NCTM) Number and Operations in Base Ten • Perform operations with multi-digit whole numbers and with decimals to hundredths Operations and Algebraic Thinking • Generate and analyze patterns ISTE NETS and Performance Indicators for Students (ISTE) Creativity and Innovation • Use models and simulations to explore complex systems and issues. Technology Operations and Concepts • Understand and use technology systems Aerospace Education Services Project MANAGEMENT MATERIALS Take time to practice with this software. While simple, it offers a • Computer with Internet variety of views with which to become familiar. access On the simulator homepage, a FIELD OF VIEW of 2 will show the inner solar system very nicely. It will be difficult to see the position of ALL the planets at one time. -
A Review of Possible Planetary Atmospheres in the TRAPPIST-1 System
Space Sci Rev (2020) 216:100 https://doi.org/10.1007/s11214-020-00719-1 A Review of Possible Planetary Atmospheres in the TRAPPIST-1 System Martin Turbet1 · Emeline Bolmont1 · Vincent Bourrier1 · Brice-Olivier Demory2 · Jérémy Leconte3 · James Owen4 · Eric T. Wolf5 Received: 14 January 2020 / Accepted: 4 July 2020 / Published online: 23 July 2020 © The Author(s) 2020 Abstract TRAPPIST-1 is a fantastic nearby (∼39.14 light years) planetary system made of at least seven transiting terrestrial-size, terrestrial-mass planets all receiving a moderate amount of irradiation. To date, this is the most observationally favourable system of po- tentially habitable planets known to exist. Since the announcement of the discovery of the TRAPPIST-1 planetary system in 2016, a growing number of techniques and approaches have been used and proposed to characterize its true nature. Here we have compiled a state- of-the-art overview of all the observational and theoretical constraints that have been ob- tained so far using these techniques and approaches. The goal is to get a better understanding of whether or not TRAPPIST-1 planets can have atmospheres, and if so, what they are made of. For this, we surveyed the literature on TRAPPIST-1 about topics as broad as irradiation environment, planet formation and migration, orbital stability, effects of tides and Transit Timing Variations, transit observations, stellar contamination, density measurements, and numerical climate and escape models. Each of these topics adds a brick to our understand- ing of the likely—or on the contrary unlikely—atmospheres of the seven known planets of the system. -
The History of Planet Earth
SECOND EDITION Earth’s Evolving The History of Systems Planet Earth Ronald Martin, Ph.D. University of Delaware Newark, Delaware © Jones & Bartlett Learning, LLC, an Ascend Learning Company. NOT FOR SALE OR DISTRIBUTION 9781284457162_FMxx_00i_xxii.indd 1 07/11/16 1:46 pm World Headquarters Jones & Bartlett Learning 5 Wall Street Burlington, MA 01803 978-443-5000 [email protected] www.jblearning.com Jones & Bartlett Learning books and products are available through most bookstores and online booksellers. To contact Jones & Bartlett Learning directly, call 800-832-0034, fax 978-443-8000, or visit our website, www.jblearning.com. Substantial discounts on bulk quantities of Jones & Bartlett Learning publications are available to corporations, professional associations, and other qualified organizations. For details and specific discount information, contact the special sales department at Jones & Bartlett Learning via the above contact information or send an email to [email protected]. Copyright © 2018 by Jones & Bartlett Learning, LLC, an Ascend Learning Company All rights reserved. No part of the material protected by this copyright may be reproduced or utilized in any form, electronic or mechanical, including photocopying, recording, or by any information storage and retrieval system, without written permission from the copyright owner. The content, statements, views, and opinions herein are the sole expression of the respective authors and not that of Jones & Bartlett Learning, LLC. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise does not constitute or imply its endorsement or recommendation by Jones & Bartlett Learning, LLC, and such reference shall not be used for advertis- ing or product endorsement purposes. -
Nature Based Solutions FEMA
PROMOTING NATURE-BASED HAZARD MITIGATION THROUGH FEMA MITIGATION GRANTS ABBREVIATIONS ADCIRC – Advanced Circulation Model HGM Approach – Hydrogeomorphic Approach BCA – Benefit-Cost Analysis HMA – Hazard Mitigation Assistance BCR – Benefit-Cost Ratio HMGP – Hazard Mitigation Grant Program BRIC – Building Resilient Infrastructure and MSCP – Multiple Species Conservation Program Communities NBS – Nature-Based Solution C&CB – Capability- and Capacity-Building NFIP – National Flood Insurance Program CDBG-DR – Community Development Block Grant- Disaster Recovery NFWF – National Fish and Wildlife Foundation CDBG-MIT – Community Development Block NOAA – National Oceanic and Atmospheric Grant-Mitigation Administration D.C. – District of Columbia NOFO – Notice of Funding Opportunity DEM – Department of Emergency Management NPV – Net Present Value DOI – Department of the Interior SCC – State Coastal Conservancy EDYS – Ecological Dynamics Simulation SDG&E – San Diego Gas & Electric EMA – Emergency Management Agency SFHA – Special Flood Hazard Area EPA SWMM – Environmental Protection Agency SHMO – State Hazard Mitigation Officer Storm Water Management Model SLAMM – Sea Level Affecting Marshes Model FEMA – Federal Emergency Management Agency SRH-2D – Sedimentation and River Hydraulics – FIRM – Flood Insurance Rate Map Two-Dimension FMA – Flood Mitigation Assistance STWAVE – Steady-State Spectral Wave Model FMAG – Fire Management Assistance Grant TNC – The Nature Conservancy HAZUS – Hazards US USACE – U.S. Army Corps of Engineers HEC-HMS – Hydrologic -
Vol. 47, No. 2 June 2018 a New Star Appears in Europe Page 14 Journal
Online PDF: ISSN 233333-9063 Vol. 47, No. 2 June 2018 Journal of the International Planetarium Society A New Star Appears in Europe Page 14 Reach for the stars... and beyond. ZEISS powerdome IV // INSPIRATION MADE BY ZEISS True Hybrid with brilliant stars and perfect renderings from a single source ZEISS powerdome IV brings many new features to your star theater: an integrated planetarium for earthbound and extraterrestrial astronomy with seamless transitions between optical and digital star fields (True Hybrid) | The universe from Earth via the solar system and Milky Way galaxy to the very edge of the observable space | Stereo projection | 8k performance | 10 bit color depth for smooth gradients | HEVC codec for efficient video renderings free of artifacts | All constellation figures, individually and in groups without any mutual overlapping | Telescope function for deep-sky imagery applying Astronomy Visualization Metadata | Complete image set of all Messier objects | Customizable polar lights, comets with gas and dust tails, and shooting stars with a great variety of parameters for location, brightness, colors and appearance | Simulation of day and night with dusk and dawn coloring of sky and panorama images | Customizable weather effects such as clouds, rain, fog, snow, rainbow, halos, air and light pollution effects | Digital rights management to secure your productions | Remote service for quick help, and much more from the only company serving planetariums for nearly a century. www.zeiss.com/planetariums zeiss-ad_pdIV_letter_x3.indd -
The Solar System
5 The Solar System R. Lynne Jones, Steven R. Chesley, Paul A. Abell, Michael E. Brown, Josef Durech,ˇ Yanga R. Fern´andez,Alan W. Harris, Matt J. Holman, Zeljkoˇ Ivezi´c,R. Jedicke, Mikko Kaasalainen, Nathan A. Kaib, Zoran Kneˇzevi´c,Andrea Milani, Alex Parker, Stephen T. Ridgway, David E. Trilling, Bojan Vrˇsnak LSST will provide huge advances in our knowledge of millions of astronomical objects “close to home’”– the small bodies in our Solar System. Previous studies of these small bodies have led to dramatic changes in our understanding of the process of planet formation and evolution, and the relationship between our Solar System and other systems. Beyond providing asteroid targets for space missions or igniting popular interest in observing a new comet or learning about a new distant icy dwarf planet, these small bodies also serve as large populations of “test particles,” recording the dynamical history of the giant planets, revealing the nature of the Solar System impactor population over time, and illustrating the size distributions of planetesimals, which were the building blocks of planets. In this chapter, a brief introduction to the different populations of small bodies in the Solar System (§ 5.1) is followed by a summary of the number of objects of each population that LSST is expected to find (§ 5.2). Some of the Solar System science that LSST will address is presented through the rest of the chapter, starting with the insights into planetary formation and evolution gained through the small body population orbital distributions (§ 5.3). The effects of collisional evolution in the Main Belt and Kuiper Belt are discussed in the next two sections, along with the implications for the determination of the size distribution in the Main Belt (§ 5.4) and possibilities for identifying wide binaries and understanding the environment in the early outer Solar System in § 5.5. -
Abstracts Connecting to the Boston University Network
20th Cambridge Workshop: Cool Stars, Stellar Systems, and the Sun July 29 - Aug 3, 2018 Boston / Cambridge, USA Abstracts Connecting to the Boston University Network 1. Select network ”BU Guest (unencrypted)” 2. Once connected, open a web browser and try to navigate to a website. You should be redirected to https://safeconnect.bu.edu:9443 for registration. If the page does not automatically redirect, go to bu.edu to be brought to the login page. 3. Enter the login information: Guest Username: CoolStars20 Password: CoolStars20 Click to accept the conditions then log in. ii Foreword Our story starts on January 31, 1980 when a small group of about 50 astronomers came to- gether, organized by Andrea Dupree, to discuss the results from the new high-energy satel- lites IUE and Einstein. Called “Cool Stars, Stellar Systems, and the Sun,” the meeting empha- sized the solar stellar connection and focused discussion on “several topics … in which the similarity is manifest: the structures of chromospheres and coronae, stellar activity, and the phenomena of mass loss,” according to the preface of the resulting, “Special Report of the Smithsonian Astrophysical Observatory.” We could easily have chosen the same topics for this meeting. Over the summer of 1980, the group met again in Bonas, France and then back in Cambridge in 1981. Nearly 40 years on, I am comfortable saying these workshops have evolved to be the premier conference series for cool star research. Cool Stars has been held largely biennially, alternating between North America and Europe. Over that time, the field of stellar astro- physics has been upended several times, first by results from Hubble, then ROSAT, then Keck and other large aperture ground-based adaptive optics telescopes. -
Monday, November 13, 2017 WHAT DOES IT MEAN to BE HABITABLE? 8:15 A.M. MHRGC Salons ABCD 8:15 A.M. Jang-Condell H. * Welcome C
Monday, November 13, 2017 WHAT DOES IT MEAN TO BE HABITABLE? 8:15 a.m. MHRGC Salons ABCD 8:15 a.m. Jang-Condell H. * Welcome Chair: Stephen Kane 8:30 a.m. Forget F. * Turbet M. Selsis F. Leconte J. Definition and Characterization of the Habitable Zone [#4057] We review the concept of habitable zone (HZ), why it is useful, and how to characterize it. The HZ could be nicknamed the “Hunting Zone” because its primary objective is now to help astronomers plan observations. This has interesting consequences. 9:00 a.m. Rushby A. J. Johnson M. Mills B. J. W. Watson A. J. Claire M. W. Long Term Planetary Habitability and the Carbonate-Silicate Cycle [#4026] We develop a coupled carbonate-silicate and stellar evolution model to investigate the effect of planet size on the operation of the long-term carbon cycle, and determine that larger planets are generally warmer for a given incident flux. 9:20 a.m. Dong C. F. * Huang Z. G. Jin M. Lingam M. Ma Y. J. Toth G. van der Holst B. Airapetian V. Cohen O. Gombosi T. Are “Habitable” Exoplanets Really Habitable? A Perspective from Atmospheric Loss [#4021] We will discuss the impact of exoplanetary space weather on the climate and habitability, which offers fresh insights concerning the habitability of exoplanets, especially those orbiting M-dwarfs, such as Proxima b and the TRAPPIST-1 system. 9:40 a.m. Fisher T. M. * Walker S. I. Desch S. J. Hartnett H. E. Glaser S. Limitations of Primary Productivity on “Aqua Planets:” Implications for Detectability [#4109] While ocean-covered planets have been considered a strong candidate for the search for life, the lack of surface weathering may lead to phosphorus scarcity and low primary productivity, making aqua planet biospheres difficult to detect. -
A Comparative Analysis of the Cobb-Douglas Habitability Score (CDHS) with the Earth Similarity Index (ESI)
A Comparative Analysis of the Cobb-Douglas Habitability Score (CDHS) with the Earth Similarity Index (ESI) Surbhi Agrawal1, Suryoday Basak1, Snehanshu Saha1, Kakoli Bora2 and Jayant Murthy3 I. Introduction and Methods is 1.27 EU, the radius is R = M 0.5 ≡ 1.12 EU1. Accordingly, the escape velocity was calculated by V = p2GM/R ≡ 1.065 (EU), and the density by A sequence of recent explorations by Saha et al. [4] e the usual D = 3M/4πR3 ≡ 0.904 (EU) formula. expanding previous work by Bora et al. [1] on using The manuscript, [4] consists of three related Machine Learning algorithm to construct and test analyses: (i) computation and comparison of ESI planetary habitability functions with exoplanet data and CDHS habitability scores for Proxima-b and raises important questions. The 2018 paper analyzed the Trappist-1 system, (ii) some considerations the elasticity of their Cobb-Douglas Habitability on the computational methods for computing the Score (CDHS) and compared its performance with CDHS score, and (iii) a machine learning exercise other machine learning algorithms. They demon- to estimate temperature-based habitability classes. strated the robustness of their methods to identify The analysis is carefully conducted in each case, potentially habitable planets from exoplanet dataset. and the depth of the contribution to the literature Given our little knowledge on exoplanets and habit- helped unfold the differences and approaches to ability, these results and methods provide one impor- CDHS and ESI. tant step toward automatically identifying objects of interest from large datasets by future ground and Several important characteristics were introduced space observatories. -
A Day in the Life of Your Data
A Day in the Life of Your Data A Father-Daughter Day at the Playground April, 2021 “I believe people are smart and some people want to share more data than other people do. Ask them. Ask them every time. Make them tell you to stop asking them if they get tired of your asking them. Let them know precisely what you’re going to do with their data.” Steve Jobs All Things Digital Conference, 2010 Over the past decade, a large and opaque industry has been amassing increasing amounts of personal data.1,2 A complex ecosystem of websites, apps, social media companies, data brokers, and ad tech firms track users online and offline, harvesting their personal data. This data is pieced together, shared, aggregated, and used in real-time auctions, fueling a $227 billion-a-year industry.1 This occurs every day, as people go about their daily lives, often without their knowledge or permission.3,4 Let’s take a look at what this industry is able to learn about a father and daughter during an otherwise pleasant day at the park. Did you know? Trackers are embedded in Trackers are often embedded Data brokers collect and sell, apps you use every day: the in third-party code that helps license, or otherwise disclose average app has 6 trackers.3 developers build their apps. to third parties the personal The majority of popular Android By including trackers, developers information of particular individ- and iOS apps have embedded also allow third parties to collect uals with whom they do not have trackers.5,6,7 and link data you have shared a direct relationship.3 with them across different apps and with other data that has been collected about you.