The Capabilities and Performance of the Automated Planet Finder Telescope with the Implementation of a Dynamic Scheduler
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Breakthrough Propulsion Study Assessing Interstellar Flight Challenges and Prospects
Breakthrough Propulsion Study Assessing Interstellar Flight Challenges and Prospects NASA Grant No. NNX17AE81G First Year Report Prepared by: Marc G. Millis, Jeff Greason, Rhonda Stevenson Tau Zero Foundation Business Office: 1053 East Third Avenue Broomfield, CO 80020 Prepared for: NASA Headquarters, Space Technology Mission Directorate (STMD) and NASA Innovative Advanced Concepts (NIAC) Washington, DC 20546 June 2018 Millis 2018 Grant NNX17AE81G_for_CR.docx pg 1 of 69 ABSTRACT Progress toward developing an evaluation process for interstellar propulsion and power options is described. The goal is to contrast the challenges, mission choices, and emerging prospects for propulsion and power, to identify which prospects might be more advantageous and under what circumstances, and to identify which technology details might have greater impacts. Unlike prior studies, the infrastructure expenses and prospects for breakthrough advances are included. This first year's focus is on determining the key questions to enable the analysis. Accordingly, a work breakdown structure to organize the information and associated list of variables is offered. A flow diagram of the basic analysis is presented, as well as more detailed methods to convert the performance measures of disparate propulsion methods into common measures of energy, mass, time, and power. Other methods for equitable comparisons include evaluating the prospects under the same assumptions of payload, mission trajectory, and available energy. Missions are divided into three eras of readiness (precursors, era of infrastructure, and era of breakthroughs) as a first step before proceeding to include comparisons of technology advancement rates. Final evaluation "figures of merit" are offered. Preliminary lists of mission architectures and propulsion prospects are provided. -
236. “Stelle E Costellazioni Del Cielo”
Progetto RaPHAEL (www.raphaelproject.com ) - Incontro nº 236 del 10/07/2005 - Colore Grigio verde 236. “Stelle e costellazioni del cielo” Una parte della natura umana è terrestre , ma un’altra parte è cosmica e stellare , volendo riscoprire la totalità della nostra vera natura è molto importante ritrovare la risonanza con le dimensioni trans-terrestri, facendo anche riemergere memorie di vite passate dove non avevamo un corpo umano e dove l’esistenza si svolgeva su altri continuum spazio-temporali. Abbiamo già visto come la Fantascienza sappia risvegliare questa risonanza (ved. incontro n° 212 ) e come ci permetta di concretizzare a livello mentale esperienze che qualcuno potrebbe aver difficoltà anche solo a concepire, adesso focalizziamo un attimo l’attenzione sull’incredibile fascino che ispirano le stelle ad ogni essere umano di animo sensibile... interiormente una parte di noi sa di originare dalle stelle ed è là che aspira a tornare! Una buona parte del nostro DNA origina da altri sistemi stellari, le leggende comparate delle varie tribù native americane raccontano che ben 12 razze galattiche hanno contribuito a creare il DNA dell’Homo sapiens. Ebbene noi suggeriamo di lasciarvi guidare dalla meditazione e dal ricordo immaginativo per recuperare i “circuiti” atemporali legati al piano cosmico , attraverso esercizi rilassati di rimpatrio energetico ed esperenziale (ed un respiro consapevole) molte esperienze possono riemergere… I nomi sotto riportati, con la posizione relativa rispetto alla costellazione di appartenenza (alfa= 1, -
Starshade Rendezvous Probe
Starshade Rendezvous Probe Starshade Rendezvous Probe Study Report Imaging and Spectra of Exoplanets Orbiting our Nearest Sunlike Star Neighbors with a Starshade in the 2020s February 2019 TEAM MEMBERS Principal Investigators Sara Seager, Massachusetts Institute of Technology N. Jeremy Kasdin, Princeton University Co-Investigators Jeff Booth, NASA Jet Propulsion Laboratory Matt Greenhouse, NASA Goddard Space Flight Center Doug Lisman, NASA Jet Propulsion Laboratory Bruce Macintosh, Stanford University Stuart Shaklan, NASA Jet Propulsion Laboratory Melissa Vess, NASA Goddard Space Flight Center Steve Warwick, Northrop Grumman Corporation David Webb, NASA Jet Propulsion Laboratory Study Team Andrew Romero-Wolf, NASA Jet Propulsion Laboratory John Ziemer, NASA Jet Propulsion Laboratory Andrew Gray, NASA Jet Propulsion Laboratory Michael Hughes, NASA Jet Propulsion Laboratory Greg Agnes, NASA Jet Propulsion Laboratory Jon Arenberg, Northrop Grumman Corporation Samuel (Case) Bradford, NASA Jet Propulsion Laboratory Michael Fong, NASA Jet Propulsion Laboratory Jennifer Gregory, NASA Jet Propulsion Laboratory Steve Matousek, NASA Jet Propulsion Laboratory Jonathan Murphy, NASA Jet Propulsion Laboratory Jason Rhodes, NASA Jet Propulsion Laboratory Dan Scharf, NASA Jet Propulsion Laboratory Phil Willems, NASA Jet Propulsion Laboratory Science Team Simone D'Amico, Stanford University John Debes, Space Telescope Science Institute Shawn Domagal-Goldman, NASA Goddard Space Flight Center Sergi Hildebrandt, NASA Jet Propulsion Laboratory Renyu Hu, NASA -
GLIESE 687 B—A NEPTUNE-MASS PLANET ORBITING a NEARBY RED DWARF
The Astrophysical Journal, 789:114 (14pp), 2014 July 10 doi:10.1088/0004-637X/789/2/114 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE LICK–CARNEGIE EXOPLANET SURVEY: GLIESE 687 b—A NEPTUNE-MASS PLANET ORBITING A NEARBY RED DWARF Jennifer Burt1, Steven S. Vogt1, R. Paul Butler2, Russell Hanson1, Stefano Meschiari3, Eugenio J. Rivera1, Gregory W. Henry4, and Gregory Laughlin1 1 UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA 2 Department of Terrestrial Magnetism, Carnegie Institute of Washington, Washington, DC 20015, USA 3 McDonald Observatory, University of Texas at Austin, Austin, TX 78752, USA 4 Center of Excellence in Information Systems, Tennessee State University, Nashville, TN 37209, USA Received 2014 February 24; accepted 2014 May 8; published 2014 June 20 ABSTRACT Precision radial velocities from the Automated Planet Finder (APF) and Keck/HIRES reveal an M sin(i) = 18 ± 2 M⊕ planet orbiting the nearby M3V star GJ 687. This planet has an orbital period P = 38.14 days and a low orbital eccentricity. Our Stromgren¨ b and y photometry of the host star suggests a stellar rotation signature with a period of P = 60 days. The star is somewhat chromospherically active, with a spot filling factor estimated to be several percent. The rotationally induced 60 day signal, however, is well separated from the period of the radial velocity variations, instilling confidence in the interpretation of a Keplerian origin for the observed velocity variations. Although GJ 687 b produces relatively little specific interest in connection with its individual properties, a compelling case can be argued that it is worthy of remark as an eminently typical, yet at a distance of 4.52 pc, a very nearby representative of the galactic planetary census. -
Data Release #3 Stuart Shaklan, Mario Damiano, Stefan Martin, Renyu Hu June 16, 2021
Starshade Exoplanet Data Challenge: Data Release #3 Stuart Shaklan, Mario Damiano, Stefan Martin, Renyu Hu June 16, 2021 © 2021 All rights reserved. Government sponsorship acknowledged. CL # 21-2781 Data provided • For RST: • Simulated spectra of scenes with the starshade blocking the target star. • Simulated spectra of the stars (starshade moved away from the scene). • Line spread and dispersion function with 1 nm, 5 mas resolution. • For HabEX: • Simulated IFS spectra of scenes with the starshade blocking the target star. • Simulated IFS spectra of the stars (starshade moved away from the scene). • Mapping arrays from lenslet positions to image plane positions with a wavelength resolution of 1 nm. RST Spectroscopy Modeling Methodology • Follows the same approach that GSFC (N. Zimmerman) took for CGI: • Use a ray trace model of the prisms and lenses. Map Image plane (x,y,lambda) to output plane (x’,y’,lambda). • But for speed, we use a 3rd order approximation to the distortion map, which has < 0.5 mas error. • Treat the slit as a simple field stop: ignore diffraction since the slit is wide compared to the PSF • Input image plane is computed with a 5 mas pixel pitch • Highly oversamples PSF • Highly oversampled compared to final CGI pixel pitch of 21.8 mas/pixel • Map from input to output with 5 mas resolution • Bin to 21.8 mas resolution using Matlab ‘imresize’ routine. • Absolute position of spectra in image plane are not tracked, but relative position of spectra in the simulations are all consistent with the scenes. Line Spread Function and Dispersion • The dispersion is calculated every nm, and on a 5 mas pixel grid (compared to 21.8 mas pixels in the camera). -
Planet Searching from Ground and Space
Planet Searching from Ground and Space Olivier Guyon Japanese Astrobiology Center, National Institutes for Natural Sciences (NINS) Subaru Telescope, National Astronomical Observatory of Japan (NINS) University of Arizona Breakthrough Watch committee chair June 8, 2017 Perspectives on O/IR Astronomy in the Mid-2020s Outline 1. Current status of exoplanet research 2. Finding the nearest habitable planets 3. Characterizing exoplanets 4. Breakthrough Watch and Starshot initiatives 5. Subaru Telescope instrumentation, Japan/US collaboration toward TMT 6. Recommendations 1. Current Status of Exoplanet Research 1. Current Status of Exoplanet Research 3,500 confirmed planets (as of June 2017) Most identified by Jupiter two techniques: Radial Velocity with Earth ground-based telescopes Transit (most with NASA Kepler mission) Strong observational bias towards short period and high mass (lower right corner) 1. Current Status of Exoplanet Research Key statistical findings Hot Jupiters, P < 10 day, M > 0.1 Jupiter Planetary systems are common occurrence rate ~1% 23 systems with > 5 planets Most frequent around F, G stars (no analog in our solar system) credits: NASA/CXC/M. Weiss 7-planet Trappist-1 system, credit: NASA-JPL Earth-size rocky planets are ~10% of Sun-like stars and ~50% abundant of M-type stars have potentially habitable planets credits: NASA Ames/SETI Institute/JPL-Caltech Dressing & Charbonneau 2013 1. Current Status of Exoplanet Research Spectacular discoveries around M stars Trappist-1 system 7 planets ~3 in hab zone likely rocky 40 ly away Proxima Cen b planet Possibly habitable Closest star to our solar system Faint red M-type star 1. Current Status of Exoplanet Research Spectroscopic characterization limited to Giant young planets or close-in planets For most planets, only Mass, radius and orbit are constrained HR 8799 d planet (direct imaging) Currie, Burrows et al. -
Overview and Reassessment of Noise Budget of Starshade Exoplanet Imaging
Overview and Reassessment of Noise Budget of Starshade Exoplanet Imaging Renyu Hua,b,*, Doug Lismana, Stuart Shaklana, Stefan Martina, Phil Willemsa, Kendra Shorta aJet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA bDivision of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA Abstract. High-contrast imaging enabled by a starshade in formation flight with a space telescope can provide a near-term pathway to search for and characterize temperate and small planets of nearby stars. NASA’s Starshade Technology Development Activity to TRL5 (S5) is rapidly maturing the required technologies to the point at which starshades could be integrated into potential future missions. Here we reappraise the noise budget of starshade-enabled exoplanet imaging to incorporate the experimentally demonstrated optical performance of the starshade and its optical edge. Our analyses of stray light sources – including the leakage through micrometeoroid damage and the reflection of bright celestial bodies – indicate that sunlight scattered by the optical edge (i.e., the solar glint) is by far the dominant stray light. With telescope and observation parameters that approximately correspond to Starshade Rendezvous with Roman and HabEx, we find that the dominating noise source would be exozodiacal light for characterizing a temperate and Earth-sized planet around Sun-like and earlier stars and the solar glint for later-type stars. Further reducing the brightness of solar glint by a factor of 10 with a coating would prevent it from becoming the dominant noise for both Roman and HabEx. With an instrument contrast of 10−10, the residual starlight is not a dominant noise; and increasing the contrast level by a factor 10 would not lead to any appreciable change in the expected science performance. -
Milestone Goto-Bino Series .Cdr
Kson MilestoneK Standard Alt/Az GOTO Mount INSTRUCTIONS CONTENT FOR KSON STANDARD ALT/AZ GOTO USER INTRODUCTION.................................................................................1 ACCESSORIES..................................................................................2 ASSEMBLY INSTRUCTIONS.............................................................3 FEATURES.........................................................................5 OPERATION MANUAL FOR SKYTOUCH CONTROLLER............... 6 KEY DESCRIPTION.................................................................................6 STATUS DESCRIPTION...........................................................................6 OPERATION PROCESS...........................................................................7 POWER ON......................................................................................7 WARNING........................................................................................7 ALIGNMENT STATUS........................................................................7 CHANGE THE DATE..................................................................7 CHANGE THE TIME...................................................................8 CHANGE THE SITE...................................................................8 ALIGNMENT.............................................................................9 NAVIGATION STATUS.....................................................................11 MENU STATUS................................................................................11 -
Scientific American
Medicine Climate Science Electronics How to Find the The Last Great Hacking the Best Treatments Global Warming Power Grid Winner of the 2011 National Magazine Award for General Excellence July 2011 ScientificAmerican.com PhysicsTHE IntellıgenceOF Evolution has packed 100 billion neurons into our three-pound brain. CAN WE GET ANY SMARTER? www.diako.ir© 2011 Scientific American www.diako.ir SCIENTIFIC AMERICAN_FP_ Hashim_23april11.indd 1 4/19/11 4:18 PM ON THE COVER Various lines of research suggest that most conceivable ways of improving brainpower would face fundamental limits similar to those that affect computer chips. Has evolution made us nearly as smart as the laws of physics will allow? Brain photographed by Adam Voorhes at the Department of Psychology, Institute for Neuroscience, University of Texas at Austin. Graphic element by 2FAKE. July 2011 Volume 305, Number 1 46 FEATURES ENGINEERING NEUROSCIENCE 46 Underground Railroad 20 The Limits of Intelligence A peek inside New York City’s subway line of the future. The laws of physics may prevent the human brain from By Anna Kuchment evolving into an ever more powerful thinking machine. BIOLOGY By Douglas Fox 48 Evolution of the Eye ASTROPHYSICS Scientists now have a clear view of how our notoriously complex eye came to be. By Trevor D. Lamb 28 The Periodic Table of the Cosmos CYBERSECURITY A simple diagram, which celebrates its centennial this 54 Hacking the Lights Out year, continues to serve as the most essential conceptual A powerful computer virus has taken out well-guarded tool in stellar astrophysics. By Ken Croswell industrial control systems. -
1455189355674.Pdf
THE STORYTeller’S THESAURUS FANTASY, HISTORY, AND HORROR JAMES M. WARD AND ANNE K. BROWN Cover by: Peter Bradley LEGAL PAGE: Every effort has been made not to make use of proprietary or copyrighted materi- al. Any mention of actual commercial products in this book does not constitute an endorsement. www.trolllord.com www.chenaultandgraypublishing.com Email:[email protected] Printed in U.S.A © 2013 Chenault & Gray Publishing, LLC. All Rights Reserved. Storyteller’s Thesaurus Trademark of Cheanult & Gray Publishing. All Rights Reserved. Chenault & Gray Publishing, Troll Lord Games logos are Trademark of Chenault & Gray Publishing. All Rights Reserved. TABLE OF CONTENTS THE STORYTeller’S THESAURUS 1 FANTASY, HISTORY, AND HORROR 1 JAMES M. WARD AND ANNE K. BROWN 1 INTRODUCTION 8 WHAT MAKES THIS BOOK DIFFERENT 8 THE STORYTeller’s RESPONSIBILITY: RESEARCH 9 WHAT THIS BOOK DOES NOT CONTAIN 9 A WHISPER OF ENCOURAGEMENT 10 CHAPTER 1: CHARACTER BUILDING 11 GENDER 11 AGE 11 PHYSICAL AttRIBUTES 11 SIZE AND BODY TYPE 11 FACIAL FEATURES 12 HAIR 13 SPECIES 13 PERSONALITY 14 PHOBIAS 15 OCCUPATIONS 17 ADVENTURERS 17 CIVILIANS 18 ORGANIZATIONS 21 CHAPTER 2: CLOTHING 22 STYLES OF DRESS 22 CLOTHING PIECES 22 CLOTHING CONSTRUCTION 24 CHAPTER 3: ARCHITECTURE AND PROPERTY 25 ARCHITECTURAL STYLES AND ELEMENTS 25 BUILDING MATERIALS 26 PROPERTY TYPES 26 SPECIALTY ANATOMY 29 CHAPTER 4: FURNISHINGS 30 CHAPTER 5: EQUIPMENT AND TOOLS 31 ADVENTurer’S GEAR 31 GENERAL EQUIPMENT AND TOOLS 31 2 THE STORYTeller’s Thesaurus KITCHEN EQUIPMENT 35 LINENS 36 MUSICAL INSTRUMENTS -
Extrasolar Planets and Their Host Stars
Kaspar von Braun & Tabetha S. Boyajian Extrasolar Planets and Their Host Stars July 25, 2017 arXiv:1707.07405v1 [astro-ph.EP] 24 Jul 2017 Springer Preface In astronomy or indeed any collaborative environment, it pays to figure out with whom one can work well. From existing projects or simply conversations, research ideas appear, are developed, take shape, sometimes take a detour into some un- expected directions, often need to be refocused, are sometimes divided up and/or distributed among collaborators, and are (hopefully) published. After a number of these cycles repeat, something bigger may be born, all of which one then tries to simultaneously fit into one’s head for what feels like a challenging amount of time. That was certainly the case a long time ago when writing a PhD dissertation. Since then, there have been postdoctoral fellowships and appointments, permanent and adjunct positions, and former, current, and future collaborators. And yet, con- versations spawn research ideas, which take many different turns and may divide up into a multitude of approaches or related or perhaps unrelated subjects. Again, one had better figure out with whom one likes to work. And again, in the process of writing this Brief, one needs create something bigger by focusing the relevant pieces of work into one (hopefully) coherent manuscript. It is an honor, a privi- lege, an amazing experience, and simply a lot of fun to be and have been working with all the people who have had an influence on our work and thereby on this book. To quote the late and great Jim Croce: ”If you dig it, do it. -
44 Closest Stars and How They Compare to Our Sun
44 CLOSEST STARS AND HOW THEY COMPARE TO OUR SUN R = Solar radius (a unit of distance to express the size of stars relative to the sun) L = Solar luminosity (a unit of radiant flux used SUN System/constellation to compare the luminosity of stars, galaxies, Solar System Potential planets and other celestial objects in terms of the sunʼs output) 8 Distance From Earth 8.317 light-minutes EARTH 1R (432,288 miles) s) -year (light Proxima Centauri TH EAR Alpha Centauri OM E FR 1 ANC DIST 4.244 light-years 0.001 0.01 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 10 25 0.1542R 0.00005L L <=0.0001 α Centauri A (Rigil Kentaurus) 1 Alpha Centauri L 4.365 light-years 1.223R 1.519 L α Centauri B (Toliman) 5 Alpha Centauri light-years 4.37 light-years 0.863R 0.5002L Bernard’s Star Ophiuchus 1 5.957 light-years 0.196R 0.0035L Wolf 359 (CN Leonis) Leo 2 7.856 light-years 0.16R 0.0014L Lalande 21185 Ursa Major 1 8.307 light-years 0.393R 0.026L Sirius A Canis Major Luyten 726-8A 8.659 light-years Cetus 1.711 R 25.4L 8.791 light-years 0.14R 0.00004L Sirius B Canis Major 8.659 light-years Luyten 726-8B 0.0084R 0.056L Cetus 8.791 light-years 0.14R 0.00004L Ross 154 Sagittarius 9.7035 light-years 0.24R 0.0038L 10 light-years Epsilon Eridani Eridanus Ross 248 2 Andromeda 10.446 light-years 10.2903 light-years 0.735R 0.34L 0.16R 0.0018L Lacaille 9352 Piscis Austrinus 3 10.7211 light-years Ross 128 0.47R 0.0367L Virgo 1 EZ Aquarii A 11 light-years Aquarius 61 Cygni A 0.1967R 0.00362L 11.1 light-years Cygnus 0.175R 0.000087L 3 (part of triple star system) 11.4 light-years