Deep Space Transport (DST) and Mars Mission Architecture
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Modelling and the Transit of Venus
Modelling and the transit of Venus Dave Quinn University of Queensland <[email protected]> Ron Berry University of Queensland <[email protected]> Introduction enior secondary mathematics students could justifiably question the rele- Svance of subject matter they are being required to understand. One response to this is to place the learning experience within a context that clearly demonstrates a non-trivial application of the material, and which thereby provides a definite purpose for the mathematical tools under consid- eration. This neatly complements a requirement of mathematics syllabi (for example, Queensland Board of Senior Secondary School Studies, 2001), which are placing increasing emphasis on the ability of students to apply mathematical thinking to the task of modelling real situations. Success in this endeavour requires that a process for developing a mathematical model be taught explicitly (Galbraith & Clatworthy, 1991), and that sufficient opportu- nities are provided to students to engage them in that process so that when they are confronted by an apparently complex situation they have the think- ing and operational skills, as well as the disposition, to enable them to proceed. The modelling process can be seen as an iterative sequence of stages (not ) necessarily distinctly delineated) that convert a physical situation into a math- 1 ( ematical formulation that allows relationships to be defined, variables to be 0 2 l manipulated, and results to be obtained, which can then be interpreted and a n r verified as to their accuracy (Galbraith & Clatworthy, 1991; Mason & Davis, u o J 1991). The process is iterative because often, at this point, limitations, inac- s c i t curacies and/or invalid assumptions are identified which necessitate a m refinement of the model, or perhaps even a reassessment of the question for e h t which we are seeking an answer. -
KENNEDY SPACE CENTER – APOLLO to MULTI-USER SPACEPORT Philip J
THE 2ND GROUND-BASED SPACE FACILITIES SYMPOSIUM 17-19 October 2017, Toulouse, France KENNEDY SPACE CENTER – APOLLO TO MULTI-USER SPACEPORT Philip J. Weber (1), Howard S. Kanner, PhD, CSEP (2) (1) National Aeronautics and Space Administration MS LX, Kennedy Space Center, FL, 32899, USA, [email protected] (2) All Points Logistics, LLC MS LX-C-LCC, Kennedy Space Center, FL, 32899, USA, [email protected] ABSTRACT NASA Kennedy Space Center (KSC) was established as the gateway to exploring beyond earth. Since the establishment of KSC in December 1963, the Center has been critical in the execution of the United States of America’s bold mission to send astronauts beyond the grasp of the terra firma. On May 25, 1961, a few weeks after a Soviet cosmonaut became the first person to fly in space, President John F. Kennedy laid out the ambitious goal “of landing a man on the moon and returning him safely to the Earth” by the end of the decade. The resultant Apollo program was massive endeavor, driven by the Cold War Space Race, and supported with a robust budget. The Apollo program consisted of 18 launches from newly developed infrastructure, including 12 manned missions and six lunar landings, ending with Apollo 17 that launched on December 7, 1972. Continuing to use this infrastructure, the Skylab program launched four missions. During the Skylab program, KSC infrastructure was redesigned to meet the needs of the Space Shuttle program, which launched its first vehicle (STS-1) on April 12, 1981. The Space Shuttle required significant modifications to the Apollo launch pads and assembly facilities, as well as new infrastructure, such as Orbiter and Payload Processing Facilities, as well as the Shuttle Landing Facility. -
Predictable Patterns in Planetary Transit Timing Variations and Transit Duration Variations Due to Exomoons
Astronomy & Astrophysics manuscript no. ms c ESO 2016 June 21, 2016 Predictable patterns in planetary transit timing variations and transit duration variations due to exomoons René Heller1, Michael Hippke2, Ben Placek3, Daniel Angerhausen4, 5, and Eric Agol6, 7 1 Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany; [email protected] 2 Luiter Straße 21b, 47506 Neukirchen-Vluyn, Germany; [email protected] 3 Center for Science and Technology, Schenectady County Community College, Schenectady, NY 12305, USA; [email protected] 4 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; [email protected] 5 USRA NASA Postdoctoral Program Fellow, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA 6 Astronomy Department, University of Washington, Seattle, WA 98195, USA; [email protected] 7 NASA Astrobiology Institute’s Virtual Planetary Laboratory, Seattle, WA 98195, USA Received 22 March 2016; Accepted 12 April 2016 ABSTRACT We present new ways to identify single and multiple moons around extrasolar planets using planetary transit timing variations (TTVs) and transit duration variations (TDVs). For planets with one moon, measurements from successive transits exhibit a hitherto unde- scribed pattern in the TTV-TDV diagram, originating from the stroboscopic sampling of the planet’s orbit around the planet–moon barycenter. This pattern is fully determined and analytically predictable after three consecutive transits. The more measurements become available, the more the TTV-TDV diagram approaches an ellipse. For planets with multi-moons in orbital mean motion reso- nance (MMR), like the Galilean moon system, the pattern is much more complex and addressed numerically in this report. -
A Disintegrating Minor Planet Transiting a White Dwarf!
A Disintegrating Minor Planet Transiting a White Dwarf! Andrew Vanderburg1, John Asher Johnson1, Saul Rappaport2, Allyson Bieryla1, Jonathan Irwin1, John Arban Lewis1, David Kipping1,3, Warren R. Brown1, Patrick Dufour4, David R. Ciardi5, Ruth Angus1,6, Laura Schaefer1, David W. Latham1, David Charbonneau1, Charles Beichman5, Jason Eastman1, Nate McCrady7, Robert A. Wittenmyer8, & Jason T. Wright9,10. ! White dwarfs are the end state of most stars, including We initiated follow-up ground-based photometry to the Sun, after they exhaust their nuclear fuel. Between better time-resolve the transits seen in the K2 data (Figure 1/4 and 1/2 of white dwarfs have elements heavier than S1). We observed WD 1145+017 frequently over the course helium in their atmospheres1,2, even though these of about a month with the 1.2-meter telescope at the Fred L. elements should rapidly settle into the stellar interiors Whipple Observatory (FLWO) on Mt. Hopkins, Arizona; unless they are occasionally replenished3–5. The one of the 0.7-meter MINERVA telescopes, also at FLWO; abundance ratios of heavy elements in white dwarf and four of the eight 0.4-meter telescopes that compose the atmospheres are similar to rocky bodies in the Solar MEarth-South Array at Cerro Tololo Inter-American system6,7. This and the existence of warm dusty debris Observatory in Chile. Most of these data showed no disks8–13 around about 4% of white dwarfs14–16 suggest interesting or significant signals, but on two nights we that rocky debris from white dwarf progenitors’ observed deep (up to 40%), short-duration (5 minutes), planetary systems occasionally pollute the stars’ asymmetric transits separated by the dominant 4.5 hour atmospheres17. -
NASA's Lunar Orbital Platform-Gatway
The Space Congress® Proceedings 2018 (45th) The Next Great Steps Feb 28th, 9:00 AM NASA's Lunar Orbital Platform-Gatway Tracy Gill NASA/KSC Technology Strategy Manager Follow this and additional works at: https://commons.erau.edu/space-congress-proceedings Scholarly Commons Citation Gill, Tracy, "NASA's Lunar Orbital Platform-Gatway" (2018). The Space Congress® Proceedings. 17. https://commons.erau.edu/space-congress-proceedings/proceedings-2018-45th/presentations/17 This Event is brought to you for free and open access by the Conferences at Scholarly Commons. It has been accepted for inclusion in The Space Congress® Proceedings by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. National Aeronautics and Space Administration NASA’s Lunar Orbital Platform- Gateway Tracy Gill NASA/Kennedy Space Center Exploration Research & Technology Programs February 28, 2018 45th Space Congress Space Policy Directive-1 “Lead an innovative and sustainable program of exploration with commercial and international partners to enable human expansion across the solar system and to bring back to Earth new knowledge and opportunities. Beginning with missions beyond low-Earth orbit, the United States will lead the return of humans to the Moon for long-term exploration and utilization, followed by human missions to Mars and other destinations.” 2 LUNAR EXPLORATION CAMPAIGN 3 4 STRATEGIC PRINCIPLES FOR SUSTAINABLE EXPLORATION • FISCAL REALISM • ECONOMIC OPPORTUNITY Implementable in the near-term with the buying -
Contents JUPITER Transits
1 Contents JUPITER Transits..........................................................................................................5 JUPITER Conjunct Sun..............................................................................................6 JUPITER Opposite Sun............................................................................................10 JUPITER Sextile Sun...............................................................................................14 JUPITER Square Sun...............................................................................................17 JUPITER Trine Sun..................................................................................................20 JUPITER Conjunct Moon.........................................................................................23 JUPITER Opposite Moon.........................................................................................28 JUPITER Sextile Moon.............................................................................................32 JUPITER Square Moon............................................................................................36 JUPITER Trine Moon................................................................................................40 JUPITER Conjunct Mercury.....................................................................................45 JUPITER Opposite Mercury.....................................................................................48 JUPITER Sextile Mercury........................................................................................51 -
A Warm Terrestrial Planet with Half the Mass of Venus Transiting a Nearby Star∗
Astronomy & Astrophysics manuscript no. toi175 c ESO 2021 July 13, 2021 A warm terrestrial planet with half the mass of Venus transiting a nearby star∗ y Olivier D. S. Demangeon1; 2 , M. R. Zapatero Osorio10, Y. Alibert6, S. C. C. Barros1; 2, V. Adibekyan1; 2, H. M. Tabernero10; 1, A. Antoniadis-Karnavas1; 2, J. D. Camacho1; 2, A. Suárez Mascareño7; 8, M. Oshagh7; 8, G. Micela15, S. G. Sousa1, C. Lovis5, F. A. Pepe5, R. Rebolo7; 8; 9, S. Cristiani11, N. C. Santos1; 2, R. Allart19; 5, C. Allende Prieto7; 8, D. Bossini1, F. Bouchy5, A. Cabral3; 4, M. Damasso12, P. Di Marcantonio11, V. D’Odorico11; 16, D. Ehrenreich5, J. Faria1; 2, P. Figueira17; 1, R. Génova Santos7; 8, J. Haldemann6, N. Hara5, J. I. González Hernández7; 8, B. Lavie5, J. Lillo-Box10, G. Lo Curto18, C. J. A. P. Martins1, D. Mégevand5, A. Mehner17, P. Molaro11; 16, N. J. Nunes3, E. Pallé7; 8, L. Pasquini18, E. Poretti13; 14, A. Sozzetti12, and S. Udry5 1 Instituto de Astrofísica e Ciências do Espaço, CAUP, Universidade do Porto, Rua das Estrelas, 4150-762, Porto, Portugal 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua Campo Alegre, 4169-007, Porto, Portugal 3 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências da Universidade de Lisboa, Campo Grande, PT1749-016 Lisboa, Portugal 4 Departamento de Física da Faculdade de Ciências da Universidade de Lisboa, Edifício C8, 1749-016 Lisboa, Portugal 5 Observatoire de Genève, Université de Genève, Chemin Pegasi, 51, 1290 Sauverny, Switzerland 6 Physics Institute, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland 7 Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain 8 Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain 9 Consejo Superior de Investigaciones Cientícas, Spain 10 Centro de Astrobiología (CSIC-INTA), Crta. -
Correlations Between Planetary Transit Timing Variations, Transit Duration Variations and Brightness fluctuations Due to Exomoons
Correlations between planetary transit timing variations, transit duration variations and brightness fluctuations due to exomoons April 4, 2017 K:E:Naydenkin1 and D:S:Kaparulin2 1 Academic Lyceum of Tomsk, High school of Physics and Math, Vavilova 8 [email protected] 2 Tomsk State University, Physics Faculty, Lenina av. 50 [email protected] Abstract Modern theoretical estimates show that with the help of real equipment we are able to detect large satellites of exoplanets (about the size of the Ganymede), although, numerical attempts of direct exomoon detection were unsuccessful. Lots of methods for finding the satellites of exoplanets for various reasons have not yielded results. Some of the proposed methods are oriented on a more accurate telescopes than those exist today. In this work, we propose a method based on relationship between the transit tim- ing variation (TTV) and the brightness fluctuations (BF) before and after the planetary transit. With the help of a numerical simulation of the Earth- Moon system transits, we have constructed data on the BF and the TTV for arXiv:1704.00202v1 [astro-ph.IM] 1 Apr 2017 any configuration of an individual transit. The experimental charts obtained indicate an easily detectable near linear dependence. Even with an artificial increase in orbital speed of the Moon and high-level errors in measurements the patterns suggest an accurate correlation. A significant advantage of the method is its convenience for multiple moons systems due to an additive properties of the TTV and the BF. Its also important that mean motion res- onance (MMR) in system have no affect on ability of satellites detection. -
Detection of Exoplanets Using the Transit Method
Detection of Exoplanets Using the Transit Method De nnis A fanase v , T h e Geo rg e W a s h i n g t o n Un i vers i t y *, Washington, DC 20052 [email protected] Abstract I conducted differential photometry on a star GSC 3281-0800, a known host to exoplanet HAT-P-32b, using analysis software AstroImageJ. I plotted the measurements from a series of images taken during the transit, via ADU count given from an earth-based digital CCD camera. I was able to establish a definite light curve and learn more about the properties of this exoplanet. * Columbian College of Arts and Sciences, 2020 Introduction Exoplanets are the planets found outside of the solar system. Since the first exoplanet was discovered in 1992, a number of methods for detection have been established. Specific to this paper, I will be evaluating the star known as HAT-P-32 (also catalogued as GSC 3281- 0800) and its exoplanet HAT-P-32b using the transit method. Figure 1. Light curve when planet passes in front of a star. When a planet passes in front of a star, the brightness of that star as Transit Method observed by us becomes dimmer; which I have conducted my research on depends on the size of the planet. The detecting exoplanets with the transit data we observe will show a dip in flux method. This method relies on taking if a planet is transiting the star we are the light flux of the target star and observing, as shown in Fig. -
Fast Transit: Mars & Beyond
Fast Transit: mars & beyond final Report Space Studies Program 2019 Team Project Final Report Fast Transit: mars & beyond final Report Internationali l Space Universityi i Space Studies Program 2019 © International Space University. All Rights Reserved. i International Space University Fast Transit: Mars & Beyond Cover images of Mars, Earth, and Moon courtesy of NASA. Spacecraft render designed and produced using CAD. While all care has been taken in the preparation of this report, ISU does not take any responsibility for the accuracy of its content. The 2019 Space Studies Program of the International Space University was hosted by the International Space University, Strasbourg, France. Electronic copies of the Final Report and the Executive Summary can be downloaded from the ISU Library website at http://isulibrary.isunet.edu/ International Space University Strasbourg Central Campus Parc d’Innovation 1 rue Jean-Dominique Cassini 67400 Illkirch-Graffenstaden France Tel +33 (0)3 88 65 54 30 Fax +33 (0)3 88 65 54 47 e-mail: [email protected] website: www.isunet.edu ii Space Studies Program 2019 ACKNOWLEDGEMENTS Our Team Project (TP) has been an international, interdisciplinary and intercultural journey which would not have been possible without the following people: Geoff Steeves, our chair, and Jaroslaw “JJ” Jaworski, our associate chair, provided guidance and motivation throughout our TP and helped us maintain our sanity. Øystein Borgersen and Pablo Melendres Claros, our teaching associates, worked hard with us through many long days and late nights. Our staff editors: on-site editor Ryan Clement, remote editor Merryl Azriel, and graphics editor Andrée-Anne Parent, helped us better communicate our ideas. -
When Extrasolar Planets Transit Their Parent Stars 701
Charbonneau et al.: When Extrasolar Planets Transit Their Parent Stars 701 When Extrasolar Planets Transit Their Parent Stars David Charbonneau Harvard-Smithsonian Center for Astrophysics Timothy M. Brown High Altitude Observatory Adam Burrows University of Arizona Greg Laughlin University of California, Santa Cruz When extrasolar planets are observed to transit their parent stars, we are granted unprece- dented access to their physical properties. It is only for transiting planets that we are permitted direct estimates of the planetary masses and radii, which provide the fundamental constraints on models of their physical structure. In particular, precise determination of the radius may indicate the presence (or absence) of a core of solid material, which in turn would speak to the canonical formation model of gas accretion onto a core of ice and rock embedded in a proto- planetary disk. Furthermore, the radii of planets in close proximity to their stars are affected by tidal effects and the intense stellar radiation. As a result, some of these “hot Jupiters” are significantly larger than Jupiter in radius. Precision follow-up studies of such objects (notably with the spacebased platforms of the Hubble and Spitzer Space Telescopes) have enabled direct observation of their transmission spectra and emitted radiation. These data provide the first observational constraints on atmospheric models of these extrasolar gas giants, and permit a direct comparison with the gas giants of the solar system. Despite significant observational challenges, numerous transit surveys and quick-look radial velocity surveys are active, and promise to deliver an ever-increasing number of these precious objects. The detection of tran- sits of short-period Neptune-sized objects, whose existence was recently uncovered by the radial- velocity surveys, is eagerly anticipated. -
The Orion Spacecraft As a Key Element in a Deep Space Gateway
The Orion Spacecraft as a Key Element in a Deep Space Gateway A Technical Paper Presented by: Timothy Cichan Lockheed Martin Space [email protected] Kerry Timmons Lockheed Martin Space [email protected] Kathleen Coderre Lockheed Martin Space [email protected] Willian D. Pratt Lockheed Martin Space [email protected] July 2017 © 2014 Lockheed Martin Corporation Abstract With the Orion exploration vehicle and Space Launch System (SLS) approaching operational status, NASA and the international community are developing the next generation of habitats to serve as a deep space platform that will be the first of its kind, a cislunar Deep Space Gateway (DSG). The DSG is evolvable, flexible, and modular. It would be positioned in the vicinity of the Moon and allow astronauts to demonstrate they can operate for months at a time well beyond Low Earth Orbit. Orion is the next generation human exploration spacecraft being developed by NASA. It is designed to perform deep space exploration missions, and is capable of carrying a crew of 4 astronauts on independent free-flight missions up to 21 days, limited only by consumables. Because Orion meets the strict requirements for deep space flight environments (reentry conditions, deep-space communications, safety, radiation, and life support for example) it is a key element in a DSG and is more than just a transportation system. Orion has the capability to act as the command deck of any deep space piloted vehicle. To increase affordability and reduce the complexity and number of subsystem functions the early DSG must be responsible for, the DSG can leverage these unique deep space qualifications of Orion.