DOCSLIB.ORG

News Concerning MOND Laws

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
News Concerning MOND Laws News concerning MOND laws Astro Seminar November 2016 MOND basic tenets • A theory of dynamics (gravity/inertia) involving a new constant a0 (beside G; :::) • Standard limit (a0 ! 0): The Newtonian limit • Scale invariance: (t; r) ! λ(t; r) MOND limit : a0 ! 1; A0 ≡ Ga0 fixed (G ! 0): a0 is analog to c in relativity or ~ in QM 1 Scale invariance X ma = F;F = mMG=r2 2 2 V ma =a0 = F; F = mMG=r , 1=2 or ma = F; F / m(MGa0) =r 2 MOND laws of galactic dynamics • Essentially follow from only the basic tenets of MOND • Are independent as phenomenological lawse.g., if interpreted as eects of DM (just as the BB spectrum, the photo electric eect, H spectrum, superconduc- tivity, etc. are independent in QM) • Pertain separately to properties of the DM alone (e.g., asymptotic atness, universal Σ), of the baryons alone (e.g., M − σ, maximum Σ), relations between the two (e.g., M − V ) • Revolve around a0 in dierent roles 3 Phenomenological lows derived from basic tenets alone In QM, many laws were derived before the Schr. equation: BB spectrum, photoelecic eect, H-like atomic spectra, specic heat of solids, Induced and spontaneous emission/absorption. All involve ~. In pre GR: equivalence principle ) gravitational redshift, light bending (c). 4 MOND: Baryonic density ) dynamical one (not in DM) r ) g r ) r ≡ − −1r~ · g . ρb( ) M ( ) ρD( ) (4πG) M 5 Some of the MOND laws • Asymptotic constancy of orbital velocity: V (r) ! V1 (H) • Light-bending angle becomes asymptotically constant (H) 4 • The velocity mass relation: V1 = MA0 (H-B) 4 • DML virial relation: σ ∼ MA0 2 • Discrepancy appears always at V =R = a0 (H-B) • Isothermal spheres have surface densities Σ¯ . a0=G (B) • The central surface density of dark halos is ≈ a0=2πG (H) • Universal baryonic-dynamical central surface densities relation (H-B). • Full rotation curves from baryon distribution alone (H-B) 6 A universal Halo central surface density? Dashed line [best t log(Σ0) = 2:15 ± 0:2] From Salucci et al. 2012 −2 ΣM ≡ a0=2πG = 138M⊙pc [log(ΣM ) = 2:14] 7 Spiral galaxies (open red circles); dwarf irregulars (full green circles), spirals and ellipticals (weak lensing black squares); Milky Way dSphs (pink triangles); nearby spirals in THINGS (small blue triangles); early-type spirals (full red triangles). 8 A universal Halo central acceleration? a. b. c. d. The parallel lines correspond to gmax(halo) =, 0:2a0 (dashed), 0:3a0 (solid), 0:4a0 (dotted). gmax(halo)=a0 ≈ 0:46ρ0Rc=ΣM 9 From Milgrom and Sanders et al. 2006 10 Maximal Halo acceleration Brada and Milgrom 1999: We have recently discovered that the modied Newtonian dynamics (MOND) implies some universal upper bound on the acceleration that can be produced by a dark halo, which, in a Newtonian analysis, is assumed to account for the eects of MOND. Not surprisingly, the limit is on the order of the acceleration constant of the theory. gH=a0 = ν(y)y − y; y = gN =a0 . ν(y ≫ 1) ≈ 1; ν(y ≪ 1) ≈ y−1=2 11 MOND prediction ΣM is a universal accumulation value of ΣH, for high-surface density galaxies. 1=2 For low-surface-density systems ΣH ≈ 2:4(ΣbΣM ) , Σb = ρR. R 1 −1r~ · g − g ΣH = 2 0 (4πG) ( N )dr = R 1 −2 @ f 2 − g ΣM 0 r @r r y[ν(y) 1] dr: y(r) ≡ gN (r)=a0. 12 Baryonic and dynamical central Surface densities Milgrom 2016, data: Lelli et al. 2016. `Scatter largely driven by obs. uncertainties'. `virtually no intrinsic scatter'. 13 Nonrelativistic theories Nonlinear Poisson equation: r~ · [µ(jr~ ϕj=a0)r~ ϕ] = 4πGρ The deep-MOND limit is conformally invariant Quaslinear MOND (QUMOND): ∆ϕN = 4πGρ, ∆ϕ = r~ · [ν(jr~ ϕN j=a0)r~ ϕN ] Derivable from actions Limits of relativistic theories (TeVeS, BIMOND, Einstein Aether) 14 central-surface-densities relation (CSDR) R 0 0 , ≡ , y 0 0 ΣD = ΣM S(ΣB=ΣM ) ΣM a0=2πG S(y) = 0 ν(y )dy Asymptotes: 0 0 for 0 ≫ , ΣD = ΣB ΣB ΣM 0 0 1=2 for 0 ≪ ΣD = (4ΣM ΣB) ΣB ΣM Quite unrelated to the mass-asymptotic-speed relation. 15 How is 0 measured? ΣD Toomre (1963): R 2 0 1 1 V (r) ΣT = 2πG 0 r2 dr 16 Discrepancy-acceleration correlation for rotationally-supported systems Scale invariance ) V (r ! 1) ! V1. 4 MOND acceleration ) V1 = MGa0. 2 2 1=2 1=2 On the asymptote g(r) = V (r)=r = (a0MG=r ) = (a0gN ) . Elsewhere on the rotation curves of any galaxy? Modied inertia ) g = gN ν(gN =a0) at all radii. ν(y) is universal. ν(y ≫ 1) ≈ 1. ν(y ≪ 1) ≈ y−1=2 (scale invariance). Also true in modied gravity for spherical systems. Predicted by MOND, Approximately, in general. 17 Discrepancy-acceleration correlation for rotationally-supported systems η ≡ g=gN vs. gN for 73 disc galaxies (points with δV=V ≤ 0:05) McGaugh (2015). −2 η ! λη, gN ! λ gN 18 Discrepancy-acceleration correlation for rotationally-supported systems 19 Discrepancy-acceleration correlation for pressure-supported systems g vs. gN , Scarpa (2006) 20 DM? The unexpected diversity of dwarf galaxy rotation curves Oman, Kyle A.; Navarro, Julio F.; Fattahi, Azadeh; Frenk, Carlos S.; Sawala, Till; White, Simon D. M.; Bower, Richard; Crain, Robert A.; Furlong, Michelle; Schaller, Matthieu; Schaye, Joop; Theuns, Tom: (2015) "...The shape of the circular velocity proles of simulated galaxies varies systematically as a function of galaxy mass, but shows remarkably little variation at xed maximum circular velocity. This is especially true for low-mass dark-matter-dominated systems, ... This is at odds with observed dwarf galaxies, which show a large diversity of rotation curve shapes, even at xed maximum rotation speed..." "...We conclude that one or more of the following statements must be true: (i) the dark matter is more complex than envisaged by any current model; (ii) current simulations fail to reproduce the diversity in the eects of baryons on the inner regions of dwarf galaxies; and/or (iii) ... data are incorrect..." Moti: "And, despite the diversity, they all sit on very tight "baryon-DM" relations." 21 Mass-asymptotic-speed relation McGaugh (2011) V (M) from scale invariance. Power 4 from acceleration 22 23 Galaxy-galaxy lensing Data from Brimioulle et al. 2013, analysis from Milgrom 2013. 24 Crater II: Discovery The feeble giant. Discovery of a large and diuse Milky Way dwarf galaxy in the constellation of Crater G. Torrealba, S. E. Koposov, V. Belokurov, M. Irwin (Submitted on 26 Jan 2016 (v1), last revised 1 Aug 2016 (this version, v4)) We announce the discovery of the Crater 2 dwarf galaxy, identied in imaging data of the VST ATLAS survey. Given its half-light radius of 1100 pc, Crater 2 is the fourth largest dwarf in the Milky Way, surpassed only by the LMC, SMC and the Sgr dwarf. With a total luminosity of MV -8, this satellite galaxy is also one of the lowest surface brightness dwarfs. Falling under the nominal detection boundary of 30 mag arcsec−2, it compares in nebulosity to the recently discovered Tuc 2 and Tuc IV and UMa II. Crater 2 is located ∼ 120 kpc from the Sun and appears to be aligned in 3-D with the enigmatic globular cluster Crater, the pair of ultra-faint dwarfs Leo IV and Leo V and the classical dwarf Leo II. We argue that such arrangement is probably not accidental and, in fact, can be viewed as the evidence for the accretion of the Crater-Leo group. 25 The velocity dispersion of Crater II: MOND prediction MOND Prediction for the Velocity Dispersion of the `Feeble Giant' Crater II (McGAugh arXiv:1610.06189) Abstract: Crater II is an unusual object among the dwarf satellite galaxies of the Local Group in that it has a very large size for its small luminosity. This provides a strong test of MOND, as Crater II should be in the deep MOND regime 2 −2 −1 2 −2 −1 (gin ≈ 34 km s kpc ≪ a0 = 3700 km s kpc ). Despite its great distance (≈ 120 kpc) from the Milky Way, the external eld of the host 2 −2 −1 (gex ≈ 282 km s kpc ) comfortably exceeds the internal eld. Consequently, Crater II should be subject to the external eld eect, a feature unique to MOND. This leads to the prediction of a very low velocity dispersion: +0:9 −1. σefe = 2:1−0:6 km s 26 The velocity dispersion of Crater II: recent measurement Nordita workshop on Dark Matter Distribution in the Era of Gaia From Twitter: Walker: Very diuse MW satellite Crater 2 has very, very cold velocity dispersion of 2.5 km/s. Implies very low dynamical density Walker: Crater 2's low velocity dispersion is also right where MOND predicts it. Boylan-Kolchin: Crater 2's velocity dispersion is pretty much exactly what DudeDarkmatter (McGaugh) predicted recently using MOND McGaugh: The MOND prediction was 2 km/s. Low because of EFE. Very hard to understand why this would happen in LCDM. 27.
Load more

Recommended publications
  • Building Blocks That Fall from the Sky
    Building blocks that fall from the sky How did life on Earth begin? Scientists from the “Heidelberg Initiative for the Origin of Life” have set about answering this truly existential question. Indeed, they are going one step further and examining the conditions under which life can emerge. The initiative was founded by Thomas Henning, Director at the Max Planck Institute for Astronomy in Heidelberg, and brings together researchers from chemistry, physics and the geological and biological sciences. 18 MaxPlanckResearch 3 | 18 FOCUS_The Origin of Life TEXT THOMAS BUEHRKE he great questions of our exis- However, recent developments are The initiative was triggered by the dis- tence are the ones that fasci- forcing researchers to break down this covery of an ever greater number of nate us the most: how did the specialization and combine different rocky planets orbiting around stars oth- universe evolve, and how did disciplines. “That’s what we’re trying er than the Sun. “We now know that Earth form and life begin? to do with the Heidelberg Initiative terrestrial planets of this kind are more DoesT life exist anywhere else, or are we for the Origins of Life, which was commonplace than the Jupiter-like gas alone in the vastness of space? By ap- founded three years ago,” says Thom- giants we identified initially,” says Hen- proaching these puzzles from various as Henning. HIFOL, as the initiative’s ning. Accordingly, our Milky Way alone angles, scientists can answer different as- name is abbreviated, not only incor- is home to billions of rocky planets, pects of this question.
    [Show full text]
  • The Feeble Giant. Discovery of a Large and Diffuse Milky Way Dwarf Galaxy in the Constellation of Crater
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Apollo MNRAS 459, 2370–2378 (2016) doi:10.1093/mnras/stw733 Advance Access publication 2016 April 13 The feeble giant. Discovery of a large and diffuse Milky Way dwarf galaxy in the constellation of Crater G. Torrealba,‹ S. E. Koposov, V. Belokurov and M. Irwin Institute of Astronomy, Madingley Rd, Cambridge CB3 0HA, UK Downloaded from https://academic.oup.com/mnras/article-abstract/459/3/2370/2595158 by University of Cambridge user on 24 July 2019 Accepted 2016 March 24. Received 2016 March 24; in original form 2016 January 26 ABSTRACT We announce the discovery of the Crater 2 dwarf galaxy, identified in imaging data of the VLT Survey Telescope ATLAS survey. Given its half-light radius of ∼1100 pc, Crater 2 is the fourth largest satellite of the Milky Way, surpassed only by the Large Magellanic Cloud, Small Magellanic Cloud and the Sgr dwarf. With a total luminosity of MV ≈−8, this galaxy is also one of the lowest surface brightness dwarfs. Falling under the nominal detection boundary of 30 mag arcsec−2, it compares in nebulosity to the recently discovered Tuc 2 and Tuc IV and UMa II. Crater 2 is located ∼120 kpc from the Sun and appears to be aligned in 3D with the enigmatic globular cluster Crater, the pair of ultrafaint dwarfs Leo IV and Leo V and the classical dwarf Leo II. We argue that such arrangement is probably not accidental and, in fact, can be viewed as the evidence for the accretion of the Crater-Leo group.
    [Show full text]
  • 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.
    [Show full text]
  • March 21–25, 2016
    FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk,
    [Show full text]
  • Abstracts of the 50Th DDA Meeting (Boulder, CO)
    Abstracts of the 50th DDA Meeting (Boulder, CO) American Astronomical Society June, 2019 100 — Dynamics on Asteroids break-up event around a Lagrange point. 100.01 — Simulations of a Synthetic Eurybates 100.02 — High-Fidelity Testing of Binary Asteroid Collisional Family Formation with Applications to 1999 KW4 Timothy Holt1; David Nesvorny2; Jonathan Horner1; Alex B. Davis1; Daniel Scheeres1 Rachel King1; Brad Carter1; Leigh Brookshaw1 1 Aerospace Engineering Sciences, University of Colorado Boulder 1 Centre for Astrophysics, University of Southern Queensland (Boulder, Colorado, United States) (Longmont, Colorado, United States) 2 Southwest Research Institute (Boulder, Connecticut, United The commonly accepted formation process for asym- States) metric binary asteroids is the spin up and eventual fission of rubble pile asteroids as proposed by Walsh, Of the six recognized collisional families in the Jo- Richardson and Michel (Walsh et al., Nature 2008) vian Trojan swarms, the Eurybates family is the and Scheeres (Scheeres, Icarus 2007). In this theory largest, with over 200 recognized members. Located a rubble pile asteroid is spun up by YORP until it around the Jovian L4 Lagrange point, librations of reaches a critical spin rate and experiences a mass the members make this family an interesting study shedding event forming a close, low-eccentricity in orbital dynamics. The Jovian Trojans are thought satellite. Further work by Jacobson and Scheeres to have been captured during an early period of in- used a planar, two-ellipsoid model to analyze the stability in the Solar system. The parent body of the evolutionary pathways of such a formation event family, 3548 Eurybates is one of the targets for the from the moment the bodies initially fission (Jacob- LUCY spacecraft, and our work will provide a dy- son and Scheeres, Icarus 2011).
    [Show full text]
  • Open Batalha-Dissertation.Pdf
    The Pennsylvania State University The Graduate School Eberly College of Science A SYNERGISTIC APPROACH TO INTERPRETING PLANETARY ATMOSPHERES A Dissertation in Astronomy and Astrophysics by Natasha E. Batalha © 2017 Natasha E. Batalha Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2017 The dissertation of Natasha E. Batalha was reviewed and approved∗ by the following: Steinn Sigurdsson Professor of Astronomy and Astrophysics Dissertation Co-Advisor, Co-Chair of Committee James Kasting Professor of Geosciences Dissertation Co-Advisor, Co-Chair of Committee Jason Wright Professor of Astronomy and Astrophysics Eric Ford Professor of Astronomy and Astrophysics Chris Forest Professor of Meteorology Avi Mandell NASA Goddard Space Flight Center, Research Scientist Special Signatory Michael Eracleous Professor of Astronomy and Astrophysics Graduate Program Chair ∗Signatures are on file in the Graduate School. ii Abstract We will soon have the technological capability to measure the atmospheric compo- sition of temperate Earth-sized planets orbiting nearby stars. Interpreting these atmospheric signals poses a new challenge to planetary science. In contrast to jovian-like atmospheres, whose bulk compositions consist of hydrogen and helium, terrestrial planet atmospheres are likely comprised of high mean molecular weight secondary atmospheres, which have gone through a high degree of evolution. For example, present-day Mars has a frozen surface with a thin tenuous atmosphere, but 4 billion years ago it may have been warmed by a thick greenhouse atmosphere. Several processes contribute to a planet’s atmospheric evolution: stellar evolution, geological processes, atmospheric escape, biology, etc. Each of these individual processes affects the planetary system as a whole and therefore they all must be considered in the modeling of terrestrial planets.
    [Show full text]
  • Planets and Exoplanets
    NASE Publications Planets and exoplanets Planets and exoplanets Rosa M. Ros, Hans Deeg International Astronomical Union, Technical University of Catalonia (Spain), Instituto de Astrofísica de Canarias and University of La Laguna (Spain) Summary This workshop provides a series of activities to compare the many observed properties (such as size, distances, orbital speeds and escape velocities) of the planets in our Solar System. Each section provides context to various planetary data tables by providing demonstrations or calculations to contrast the properties of the planets, giving the students a concrete sense for what the data mean. At present, several methods are used to find exoplanets, more or less indirectly. It has been possible to detect nearly 4000 planets, and about 500 systems with multiple planets. Objetives - Understand what the numerical values in the Solar Sytem summary data table mean. - Understand the main characteristics of extrasolar planetary systems by comparing their properties to the orbital system of Jupiter and its Galilean satellites. The Solar System By creating scale models of the Solar System, the students will compare the different planetary parameters. To perform these activities, we will use the data in Table 1. Planets Diameter (km) Distance to Sun (km) Sun 1 392 000 Mercury 4 878 57.9 106 Venus 12 180 108.3 106 Earth 12 756 149.7 106 Marte 6 760 228.1 106 Jupiter 142 800 778.7 106 Saturn 120 000 1 430.1 106 Uranus 50 000 2 876.5 106 Neptune 49 000 4 506.6 106 Table 1: Data of the Solar System bodies In all cases, the main goal of the model is to make the data understandable.
    [Show full text]
  • May 2016 Vol
    May 2016 Vol. 47, No. 5 The Warren Astronomical Society President: Diane Hall [email protected] First Vice President: Ralph DeCew [email protected] Founded: 1961 Second Vice President: Jeff MacLeod [email protected] Treasurer: Joe Tocco [email protected] P.O. BOX 1505 Secretary: Dennis David [email protected] WARREN, MICHIGAN 48090-1505 Publications: Dale Thieme [email protected] Outreach: Bob Trembley [email protected] http://www.warrenastro.org Entire Board [email protected] President’s Field of View the Perfect Club” put on by John Goss, current president of the Astronomical League. We wanted pointers on how to keep the W.A.S. in good run- ning shape when it comes to recruitment, volun- teering, and administration. Over the course of the workshop, it became appar- ent that the W.A.S. is such a vibrant club and fun place to be because we— you— already have many “best practices” in place and as part of our club A Love Letter traditions. To be certain, we’ve had major successful projects: renovating Stargate On April 9th of this year, I was able to attend the and making the Kalinowski-Khula Telescope its Northeast Astronomy Forum (NEAF), the tremen- central gem, updating the by-laws and re- dous astronomy and space expo put on by the attaining 501[c]3 status, transitioning the Rockland Astronomy Club in New York State. W.A.S.P. from print to digital. But the social ritual NEAF is a must-do for any amateur astronomer of snack time matters. Greeting potential new with the means to get there, a fabulous place to members with handouts matters (thank you, Jon browse telescopes and eyepieces you’ll never take Blum!).
    [Show full text]
  • DARE MIGHTY THINGS Recent Science Achievements from NASA
    DARE MIGHTY THINGS Recent Science Achievements From NASA Jason Hyon With Contributions from NASA HQ, Renyu Hu, Tiffany Kataria, Christof Sotin, Kevin Hand, Ashwin Vasavada, Lisa Storry-Lombardi Jet Propulsion Laboratory California Institute of Technology NASA Centers Transferred with NACA July 1960 • Langley Research Center, VA • Marshall Space Flight Center, AL, • Ames Research Center, CA transferred from the US Army • Lewis (now Glenn) Research Center, July 1961 OH • Manned Spacecraft Center, TX, • (now Armstrong) Flight Research established – renamed Johnson Space Center, CA Center in 1973 December 1958 October 1961 • Jet Propulsion Laboratory, CA, • Mississippi Test Facility established – transferred from the US Army renamed Stennis Space Center in 1988 May 1959 March 1962 • Parts of the Naval Research Laboratory • Launch Operations Center, now transfer to NASA – becomes the Kennedy Space Center, FL, established Goddard Space Flight Center, MD Aeronautics Research NASA is with you when you fly. Human Exploration International Space Station Off the Earth, for the Earth. Earth Your planet is changing. We’re on it. Mars Join us on the journey. Mars Join us on the journey. Solar System and Beyond NASA… We’re out there. Solar System and Beyond NASA… We’re out there. NASA Technology Technology drives exploration. Partnership Opportunities • International Agency • Small Business • Aerospace • Universities • Postdoc and visiting scientists • Outreach • Space Act • Patent Formation of Universe https://civitashumana.files.wordpress.com/2014/05/multiverse-graph.jpg
    [Show full text]
  • Astronomy Magazine 2011 Index Subject Index
    Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63
    [Show full text]
  • Features the Work of Leading Researchers in the Field Of
    February 2015 Remembering AIAA’s Jim Harford/page 4 FLEET ON YOUR Page 28 BILLION$ on no fault found $AVE BILLION$ time and parts ON YOUR FLEET Stop wasting Stop wasting time and parts on no fault found USAF’s Otto on ISR planes/24 Small sats, big plans/40 A PUBLICATION OF THE AMERICAN INSTITUTE OF AERONAUTICS AND ASTRONAUTICS AIAA Progress in Astronautics and Aeronautics AIAA’s popular book series Progress in Astronautics and Aeronautics features books that present a particular, well- defi ned subject refl ecting advances in the fi elds of aerospace science, engineering, and/or technology. POPULAR TITLES Tactical and Strategic Missile Guidance, Sixth Edition Paul Zarchan 1026 pages This best-selling title provides an in-depth look at tactical and strategic missile guidance using common language, notation, and perspective. The sixth edition includes six new chapters on topics related to improving missile guidance system performance and understanding key design concepts and tradeoffs. ISBN: 978-1-60086-894-8 List Price: $134.95 “AIAA Best Seller” AIAA Member Price: $104.95 Morphing Aerospace Vehicles and Structures John Valasek 286 pages Morphing Aerospace Vehicles and Structures is a synthesis of the relevant disciplines and applications involved in the morphing of fi xed wing fl ight vehicles. The book is organized into three major sections: Bio-Inspiration; Control and Dynamics; and Smart Materials and Structures. Most chapters are both tutorial and research-oriented in nature, covering elementary concepts through advanced – and in many cases
    [Show full text]
  • Abstract Book
    ESA SCI Science Workshop #12 12–14 November 2019 Aranjuez, Spain Abstracts Organising Committee: Alba Alcol, Rune Floberghagen, Michael Küppers, Erik Kuulkers, Tanya Lim, Gabriele Matzeu, Jennifer Ngo-Anh, Mylène Riemens, Jan Tauber, Joe Zender. Space Science Workshop #12 12-14 November 2019, Aranjuez, Spain Scientific Programme Tuesday 12 November 13:00 – Lunch Poster Setup 15:00 Session Chair: Nuria Álvarez 1 15:00 Welcome Arvind Parmar 15:10 Black holes: No hairs, no mercy (Invited) Richard Saxton 15:40 Modelling black hole variability with XMM Michael Parker 16:00 Solving the X-ray Broadband emission in the NLS1 TON Gabriele Matzeu S180 16:20 An upper limit on the mass of a central black hole in the Nora Luetzgendorf large magellanic cloud 16:40 Coffee Break Poster Setup for stragglers Session Chair: Héctor Canovas 2 17:00 Further Investigations of Massive Stars Found Outside Tony Marston Prominent Star Clusters 17:20 Polluting in time and space Guido de Marchi 17:40 Dynamical histories of nearby star-forming regions Catarina Alves de Oliveira 18:00 New RFs and YGTs introduction Jan-Uwe Ness/Ana Heras 18:30 End of Oral Session 18:45 Poster Session + Icebreaker All Poster first authors – Poster room 20:00 End of Sessions 20:15 Buffet Dinner Wednesday 13 November Session Chair:Georgina Graham 3 09:00 Radar Interferometry of Volcanoes (Invited) Julia Kubanek 09:30 Unbuckling the Van Allen Belts: History and Physics Lionel Métrailler 09:50 Radiation health risk assessment and mitigation beyond Low Anna Fogtman Earth Orbit. 10:10 Discovering their Universe - consulting the public on Voyage Karen O’Flaherty 2050 10:30 Coffee Break / Posters Poster room Session Chair: Anezina Solomonidou 4 10:50 Unlocking the Secrets of a Previously Unopened Apollo 17 Francesca McDonald Core Sample 11:10 Constraints on the origin of the sources of lunar magnetic Joana S.
    [Show full text]