DOCSLIB.ORG

© in This Web Service Cambridge University

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Cambridge University Press 978-1-107-06885-8 - The New Cosmos: Answering Astronomy’s Big Questions David J. Eicher Index More information Index 1992QB1,11 Alpha Centauri B, 115 2010 TK7,92 Alpha Centauri Bb, 115 2060 Chiron, 89 Alpha Centauri C, 115 2MASS Survey, 135 Alpha-Proxima Centauri, 15, 115 3753 Cruithne, 92 Alpha Regio, 81 3C 48, 206 Alpher, Ralph, 146 3C 273, 206–207 aluminum, 53, 85 47 Tucanae, 125, 165 Alvarez, Luis, 44 51 Pegasi, 11, 104, 106, 113 Alvarez, Walter, 44 55 Cancri e, 108, 112 Amazonis Planitia, 71 61 Cygni, 162 American Astronomical Society, ix 70 Ophiuchi, 103 Ames Research Center, 44 amino acids, 36, 227 aa (lava), 84 ammonia, 35, 99, 232 accelerating universe, 191, 215 amphibians, 228 accretion disk, 207 amphibole, 85 Acheron, 94 Anaxagoras, 49 Acrux, 164 Andromeda Galaxy, 5, 12, 128, 132, 136–137, active galactic nuclei, 208 140, 165, 172, 208 adaptation, 35 Andromeda I, 135 Africa, 46, 83, 134 Andromeda II, 135 age of the universe, 13 angular momentum, 51, 53, 137, 179 AGN, 208 anisotropies, 193 Aino Planitia, 83 Annual Review of Astronomy and albedo, 98 Astrophysics,39 albedo features, 97 anorthosite, 57 Aldebaran, 163 Antarctica, 35 Alfonso X of Castile, v Antares, 164 ALH 84001, 35 antimatter, 45, 153 Allen Telescope Array, 237 antimuons, 152, 179 Alpha and Proxima Centauri, 160 antiparticles, 153 Alpha Centauri, 18, 162, 164 anti-tau particles, 179 Alpha Centauri A, 115 “An Unbound Universe,” 188 264 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-06885-8 - The New Cosmos: Answering Astronomy’s Big Questions David J. Eicher Index More information Index Aphrodite Terra, 82–83, 85 Beehive Cluster, 163 Apollo program, 8, 32, 48, 50, 53, 57 Beer, Wilhelm, 49 Arches cluster, 127 Bekenstein, Jacob, 210 Arcturus, 164 Belbruno, Edward, 59 Ares Vallis, 71 Bell Laboratories, 146 Argyre, 9, 70 Bell Regio, 81 Aristarchus of Samos, 49, 159 Bender, Ralf, 136 Aristotle, 33, 49, 225 Benjamin, Robert A., xvii, 129 Artemis Chasma, 86 Bennett, Charles L., 193 arthropods, 228 Bern, Switzerland, 6 Asteria, 82 Beta (venusian tessera), 82 asteroids, 11, 32, 35, 44–45, 53–54, 61, 73, 159– Beta Pictoris Moving Group, 57 160, 229 Beta Regio, 86 asteroids, Hilda group, 93 Betelgeuse, 46, 164 astrometry, 105–106 Betz, Eric, xviii astronomical unit, 92, 159 BICEP2, 154, 194 Astronomy magazine, xii, xvii–xviii, 14, 91, Big Bang nucleosynthesis, 195 198 Big Bang theory, xv, 13–14, 145, 148–149, 153, astrophysical jets, 207, 210 157, 168–169, 175–176, 187, 192, 194, 213, astrophysics, xv 221 Atalanta Planitia, 83 Big Crunch, 221 Athens, Greece, 33 Big Dipper, 124 Atla Regio, 84–86 Big Freeze, 219 atomic hydrogen, 127 Big Rip, 218, 221 Auriga, 113 binary stars, 104 Austin, Texas, 118 Binzel, Richard, 97 Australia, 8, 16, 32, 37, 43, 80, 83, 189, 226 biochemistry, 35 Australopithecus africanus, 134 birds, 38 axions, 183 Birr Castle, 5 bismuth, 53 B-mode polarization, 154, 194 Black Hole Era, 220 Baade, Walter, 146, 172, 201 black holes, ix, xiv, 14, 24–25, 45, 123, 127, bacteria, 8, 37 136, 140, 143, 148, 162, 183, 185, 198, 201– Bailey, Karyn, xvii 202, 205, 211, 214, 219, 221 Bakich, Michael, xvii Blanco Telescope, 197 Balick, Bruce, xvii Blinking Planetary, 164 bar (galactic), 122, 162 blueshift, 106 Barnard’s Galaxy, 132 Blumenthal, George, 178 Barnard’s Star, 103, 162 bolometric magnitude, 39 barred spiral galaxies, 12, 118, 127, 131 Bondi, Hermann, 145 Barringer Meteor Crater, 229 Bonneville Crater, 71 baryon acoustic oscillations, 197 Boötes, 164 baryonic matter, 146, 153, 171, 194, 213, 220 bosons, 179 baryons, 148, 176, 179 Boulder, Colorado, 51 Bath, England, 5 Brahe, Tycho, 159 BBC Radio, 145 Breakthrough Prize in Fundamental Physics, Beagle 2, 62 192 265 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-06885-8 - The New Cosmos: Answering Astronomy’s Big Questions David J. Eicher Index More information Index Brown, Mike, 90 Castor, 164 Brown University, xviii CCD (charge-coupled devices), 78 Bruno, Giordano, 103 cD galaxy, 132 Buie, Marc W., 94, 97 CDM (cold dark matter), 178, 180–181 Bullet Cluster, 174 Centaurus, 162 Burns formation, 72 Centaurus A, 140, 166 Butler, Paul, 104 Centaurus A/M83 Group, 166 central bar (Milky Way), 129 calcium carbonate, 42 central bulge (Milky Way), 122, 126 Caldeira, Ken, 39 Central, “Bulgy” Bar (Milky Way), 119 Caldwell, Robert, 218 Cepheid variable stars, 5, 12, 132, 169 California, 104 Cepheus, 162 California Institute of Technology, 56, 171, Ceres, 51, 90 206 Cerro Tololo Inter-American Observatory, Callisto, 47, 231 197 Caloris Basin, 55 Chandra X-ray Telescope, 136 Cambrian explosion, 228 Chandrasekhar, Subrahmanyan, 23, 201 Cambrian period, 37 Chandrasekhar limit, 201–202 Cameron, Alistair G. W., 51 CHaracterizing ExOPlanets Satellite Campbell, William W., 186 (CHEOPS), 110 Canada, 80 Charon, 47, 94, 97, 99 Canada-France-Hawaii Telescope, 208 Chelyabinsk, Russia, 45 Canary Islands, 79, 119 chemistry, 34 Cancer, 163 Chicago, Illinois, 12, 137 Canis Major, 163 Chicxulub crater, 44 Canis Major Dwarf, 166 Chile, 197 Canis Minor, 162 chondrite meteorites, 53 Canopus, 164 Christy, James W., 94 Canup, Robin M., 51, 59, 100 chromium, 53 Capella, 18 Chryse Planitia, 61, 65–66, 70–71 capture (origin of Moon idea), 50 Churchwell, Ed, 129 carbohydrates, 34 civilizations, 16, 115 carbon, 18, 25, 27, 34, 42, 112 CL J1449þ0856, 168 carbon dioxide, 8, 37, 39, 42, 46, 64, 68, 73–74, clusters of galaxies, 171 76, 78, 235 co-accretion (Moon), 50 carbon monoxide, 28, 35, 95, 98, 124 Coalsack, 164 carbonaceous chondrite meteorites, 20, 52 COBE spacecraft, 129, 175, 193 Carboniferous period, 38, 228 Cocconi, Giuseppe, 237 Carina, 174 cold dark matter, 178 Carina Nebula, 164 color-magnitude diagrams, 21, 125, 137, 169 Carina-Sagittarius Arm (Milky Way), 131 Columbia Hills, 69, 71 Carl Sagan Memorial Station, 61 Columbia River Basalt Group, 85 Carnegie Institution of Washington, 56, 173 Columbia University, 52 Carson, Johnny, xi Coma Berenices, 163 Cassini–Huygens mission, 231 Coma Cluster of galaxies, 132 Cassiopeia, 117, 135 Coma Star Cluster, 163 Cassiopeia Dwarf Galaxy, 135 Comet 103P/Hartley, 108 266 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-06885-8 - The New Cosmos: Answering Astronomy’s Big Questions David J. Eicher Index More information Index Comet Wild 2, 36 dark matter, ix–x, xvi, 13, 122, 137, 144, 146, comets, 15, 32, 35–36, 44, 54, 160, 229, 231 165, 170–171, 176, 187, 193–194, 213, 221 constellations, 46 dark matter fluctuations, 175 Contact, 237 dark nebulae, 123, 164 Convection, 78 Dartmouth College, 218 COnvection ROtation et Transits Planétaires Darwin, Charles, 53 (COROT), 108 Darwin, George, 53 Copernicus, Nicolaus, 4, 159 Darwinian evolution, 33, 226, 228, 235 corals, 228 Davis, Donald R., 51 Cornell University, xi, 237 de Sitter, Willem, 185 coronae (venusian features), 79, 82, 86 de Vaucouleurs, Gérard, 118, 135 Cosmic Background Explorer (COBE), 13, Deccan Flats, 85 148, 175 Deep Impact, 58 cosmic dark ages, 148 Deep Sky, xii, 91 Cosmic Discovery, 195 Deep Sky Monthly,xi cosmic distance scale, xv, 15, 117, 158 Degenerate Era, 219 cosmic inflation, 194, 212 degenerate stars, 201 cosmic microwave background radiation, xv, Deimos, 61 13, 146, 148, 175, 192, 213 Deneb, 164 cosmic rays, 127, 201 density fluctuations, 177 cosmological constant, 182, 186, 188, 190, 192, deoxyribonucleic acid (DNA), 34 215, 217 deuterium, 78, 151 Cosmos,xi Deuteronilus Mensae, 71 Cox, T. J., 137 Devonian period, 37, 228 craters, 10, 79, 81 diapir, 86 Cretaceous period, 38, 228 Diffuse Infrared Background Experiment, Cretaceous-Paleogene, 229 129 Cretaceous-Paleogene Extinction Event, 44 dinosaurs, 228 Cretaceous-Paleogene Impact, 38 “Discovery of a Supernova Explosion at Half critical density, 187 the Age of the Universe and its Crux, 163–164 Cosmological Implications,” 191 cryosphere, 64, 68, 74 disk scale radius, 135 cryovolcanism, 232 Disney, Walt, 89 cryovolcanoes, 231 DNA, 34, 36, 226–227 Curiosity (Mars rover), 62, 72 Donato, Leonardo, 2 Curtis, Heber D., 5 Doppler effect, 106 curvature of space, 213 Doppler shifts, 28, 129, 204 cyanobacteria, 32, 43, 226, 228 Doppler technique, 105–106, 114 Cygnus, 11, 109, 112, 114, 117, 162–164 Double Cluster, 163 Cygnus X-1, 14, 198, 204 double planet, 52 double stars, 29, 31 dark energy, ix–x, xvi, 13–14, 146, 171, 181, down quarks, 179 183–184, 191, 193–195, 213–214, 216–217, Drake, Frank, 236–237 219, 221 Drake Equation, 236 dark energy density, 194 Dressler, Alan, 208 Dark Energy Survey, 197 Dumbbell Nebula, 26, 164 Dark Era, 221 dunes, 81 267 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-06885-8 - The New Cosmos: Answering Astronomy’s Big Questions David J. Eicher Index More information Index dunkle Materie, 171 end Triassic, 45 dwarf galaxies, 132 Endurance crater, 72 dwarf planets, 11, 51, 89, 94, 229 enstatite chondrite meteorites, 53 dwarf stars, 16–17 entropy, 153 Dzigai Vallis, 70 EPOXI, 108 Epsilon Eridani, 162, 237 E ¼ mc2, 148, 184 Epsilon Indi, 162 Eagle crater, 72 era of equal densities, 148 Eagle Nebula, 164 ergosphere, 203 Earth, x, xv–xvi, 7–8, 16, 25, 32, 39, 43–44, Eris, 90, 94, 101, 159, 161 46–47, 53, 75, 78, 84, 90, 92, 94, 97, 100, 123, Erosion, 80 131, 152, 159, 170, 211, 224, 226, 228–229, Eskimo Nebula, 164 231, 234–235 ethane, 35, 231 Earth Trojan asteroid, 92 eukaryotes, 37, 228 earthlike planets,
Recommended publications
  • Photometric Study of Two Near-Earth Asteroids in the Sloan Digital Sky Survey Moving Objects Catalog

    Photometric Study of Two Near-Earth Asteroids in the Sloan Digital Sky Survey Moving Objects Catalog

    University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2020 Photometric Study Of Two Near-Earth Asteroids In The Sloan Digital Sky Survey Moving Objects Catalog Christopher James Miko Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Miko, Christopher James, "Photometric Study Of Two Near-Earth Asteroids In The Sloan Digital Sky Survey Moving Objects Catalog" (2020). Theses and Dissertations. 3287. https://commons.und.edu/theses/3287 This Thesis is brought to you for free and open access by the Theses, Dissertations, and Senior Projects at UND Scholarly Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. PHOTOMETRIC STUDY OF TWO NEAR-EARTH ASTEROIDS IN THE SLOAN DIGITAL SKY SURVEY MOVING OBJECTS CATALOG by Christopher James Miko Bachelor of Science, Valparaiso University, 2013 A Thesis Submitted to the Graduate Faculty of the University of North Dakota in partial fulfillment of the requirements for the degree of Master of Science Grand Forks, North Dakota August 2020 Copyright 2020 Christopher J. Miko ii Christopher J. Miko Name: Degree: Master of Science This document, submitted in partial fulfillment of the requirements for the degree from the University of North Dakota, has been read by the Faculty Advisory Committee under whom the work has been done and is hereby approved. ____________________________________ Dr. Ronald Fevig ____________________________________ Dr. Michael Gaffey ____________________________________ Dr. Wayne Barkhouse ____________________________________ Dr. Vishnu Reddy ____________________________________ ____________________________________ This document is being submitted by the appointed advisory committee as having met all the requirements of the School of Graduate Studies at the University of North Dakota and is hereby approved.
  • Planets Transiting Non-Eclipsing Binaries

    Planets Transiting Non-Eclipsing Binaries

    A&A 570, A91 (2014) Astronomy DOI: 10.1051/0004-6361/201323112 & c ESO 2014 Astrophysics Planets transiting non-eclipsing binaries David V. Martin1 and Amaury H. M. J. Triaud2;? 1 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, CH-1290 Sauverny, Switzerland e-mail: [email protected] 2 Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA Received 22 November 2013 / Accepted 28 August 2014 ABSTRACT The majority of binary stars do not eclipse. Current searches for transiting circumbinary planets concentrate on eclipsing binaries, and are therefore restricted to a small fraction of potential hosts. We investigate the concept of finding planets transiting non-eclipsing binaries, whose geometry would require mutually inclined planes. Using an N-body code we explore how the number and sequence of transits vary as functions of observing time and orbital parameters. The concept is then generalised thanks to a suite of simulated circumbinary systems. Binaries are constructed from radial-velocity surveys of the solar neighbourhood. They are then populated with orbiting gas giants, drawn from a range of distributions. The binary population is shown to be compatible with the Kepler eclipsing binary catalogue, indicating that the properties of binaries may be as universal as the initial mass function. These synthetic systems produce transiting circumbinary planets occurring on both eclipsing and non-eclipsing binaries. Simulated planets transiting eclipsing binaries are compared with published Kepler detections. We find 1) that planets transiting non-eclipsing binaries are probably present in the Kepler data; 2) that observational biases alone cannot account for the observed over-density of circumbinary planets near the stability limit, which implies a physical pile-up; and 3) that the distributions of gas giants orbiting single and binary stars are likely different.
  • Science in the Urantia Papers

    Science in the Urantia Papers

    Science ¾ Scientific Validation of the UB z By Denver Pearson z By Phil Calabrese ¾ Seraphic Velocities ¾ Astronomy The Scientific Integrity of the Urantia Book by Denver Pearson As scientifically minded readers first peruse the Urantia Book, it soon occurs to them that many of its statements on the natural sciences conflict with currently held data and theories. In the minds of many this gives rise to doubts about the truthfulness of those statements. Wisdom would lead us to realize that nothing short of perfection is perfect, and anything touched by human hands has fingerprints. This should be our guiding thoughts as we contemplate the accuracy of the scientific content of the Urantia Papers. Several years ago, at the first scientific symposium, it was implied by one of the speakers that the revelation contains errors. This implication is alarming. More recently, at the second symposium held in Oklahoma, an interesting publication named "The Science Content of The Urantia Book" was made available (this document is obtainable from the Brotherhood of Man Library). In this publication is an article entitled "Time Bombs" in which the author suggests that the revelators planted certain inaccurate scientific statements in the book in order to prevent it from becoming a fetish. He states "...the revelators incorporated safeguards in the papers that would form The Urantia Book to diminish the tendency to regard it as an object of worship. What safeguards did they use? Suppose they decided to make sure that mortals reading it understood that some cosmological statements in the book would be found to be inaccurate".
  • Arxiv:0809.1275V2

    Arxiv:0809.1275V2

    How eccentric orbital solutions can hide planetary systems in 2:1 resonant orbits Guillem Anglada-Escud´e1, Mercedes L´opez-Morales1,2, John E. Chambers1 [email protected], [email protected], [email protected] ABSTRACT The Doppler technique measures the reflex radial motion of a star induced by the presence of companions and is the most successful method to detect ex- oplanets. If several planets are present, their signals will appear combined in the radial motion of the star, leading to potential misinterpretations of the data. Specifically, two planets in 2:1 resonant orbits can mimic the signal of a sin- gle planet in an eccentric orbit. We quantify the implications of this statistical degeneracy for a representative sample of the reported single exoplanets with available datasets, finding that 1) around 35% percent of the published eccentric one-planet solutions are statistically indistinguishible from planetary systems in 2:1 orbital resonance, 2) another 40% cannot be statistically distinguished from a circular orbital solution and 3) planets with masses comparable to Earth could be hidden in known orbital solutions of eccentric super-Earths and Neptune mass planets. Subject headings: Exoplanets – Orbital dynamics – Planet detection – Doppler method arXiv:0809.1275v2 [astro-ph] 25 Nov 2009 Introduction Most of the +300 exoplanets found to date have been discovered using the Doppler tech- nique, which measures the reflex motion of the host star induced by the planets (Mayor & Queloz 1995; Marcy & Butler 1996). The diverse characteristics of these exoplanets are somewhat surprising. Many of them are similar in mass to Jupiter, but orbit much closer to their 1Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Rd.
  • 1 Introduction

    1 Introduction

    ASTROPHYSICAL RESEARCH CONSORTIUM Principles of Operation for SDSS-V VERSION: v1.1 Approved by the ARC Board of Governors 1 Introduction Over the past 15 years, the Sloan Digital Sky Survey has carried out some of the most influential surveys in the history of astronomy. Through four prior epochs, called SDSS-I, II, III, and IV, the SDSS has provided world-leading data sets for a vast range of astrophysical research, including the study of extragalactic astrophysics, cosmology, the Milky Way, the solar system, and stars. The current SDSS-IV project is funded to operate through June 30, 2020. At that time, the 2.5-m Sloan Foundation Telescope at Apache Point Observatory (APO) and its instruments will remain a world-leading facility for wide-field spectroscopy, ready to pursue further state-of-the-art investigations of the Universe. The APOGEE South spectrograph recently commissioned for use at the 2.5-m du Pont Telescope at Las Campanas Observatory (LCO) provides a matching state-of-the-art capability in the Southern hemisphere. SDSS-V as currently envisaged is a five-year program to use these facilities at APO and LCO to execute the first-ever all-sky, multi-epoch survey involving both near-infrared and optical spectroscopy, with rapid response target allocation enabled by new fiber-positioning robots. SDSS-V consists of three survey components. The Milky Way Mapper will conduct infrared and optical spectroscopy of millions of stars to chart and interpret our Galaxy’s history, and to understand the astrophysics of stars and their relation to planets. The Black Hole Mapper will monitor quasars and X-ray sources from next-generation X-ray satellites to investigate the physics and evolution of supermassive black holes.
  • And Ecclesiastical Cosmology

    And Ecclesiastical Cosmology

    GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc.
  • A Remarkable Panoramic Space Telescope for the 2020'S

    A Remarkable Panoramic Space Telescope for the 2020'S

    A Remarkable Panoramic Space Telescope for the 2020s Dr. Marc Postman (SB ’81, MIT) Space Telescope Science Institute How are stars and galaxies formed? How does the universe work? Astronomers ask big questions. Are we alone? WFIRST: Wide Field Infrared Survey Telescope Dark Energy, Dark Wide-Field Surveys of the Matter, and the Fate of the Universe Universe ? ? Technology Development for The full distribution of planets around stars Exploration of New Worlds National Academy of Sciences Astronomy & Astrophysics Decadal Survey (2010) DARK MATTER DARK ENERGY 26% 69% STARS, GAS, DUST, ALL WE CAN SEE 5% How do we know there is so much dark matter? And what could dark matter be? How do we know there is so much dark energy? And what is it? Do we need new physics? What new experiments do we need to run? What new observations do we need to make? Basic properties of dark matter… • Dark matter is likely a particle, the way protons and neutrons are particles. • These particles must be abundant. • Dark matter barely interacts, if at all, with other matter (except by gravity). • Dark matter does not emit light. • Dark matter is passing through each of us right now (about 3 x 10-7 micrograms every second)*. *Based on E. Siegel, Forbes We already know dark matter cannot be: • Black holes • Neutrinos • Dwarf planets • Cosmic dust • Squirrels https://xkcd.com/2186/ Cluster of galaxies We can measure the mass in a system by measuring orbital speeds and distances 60 50 Mercury 40 Venus 30 Earth Mars 20 Jupiter Orbital Velocity (km/s) Velocity Orbital 10
  • Cfa in the News ~ Week Ending 3 January 2010

    Cfa in the News ~ Week Ending 3 January 2010

    Wolbach Library: CfA in the News ~ Week ending 3 January 2010 1. New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 2. 2009 in science and medicine, ROGER SCHLUETER, Belleville News Democrat (IL), Sunday, January 3, 2010 3. 'Science, celestial bodies have always inspired humankind', Staff Correspondent, Hindu (India), Tuesday, December 29, 2009 4. Why is Carpenter defending scientists?, The Morning Call, Morning Call (Allentown, PA), FIRST ed, pA25, Sunday, December 27, 2009 5. CORRECTIONS, OPINION BY RYAN FINLEY, ARIZONA DAILY STAR, Arizona Daily Star (AZ), FINAL ed, pA2, Saturday, December 19, 2009 6. We see a 'Super-Earth', TOM BEAL; TOM BEAL, ARIZONA DAILY STAR, Arizona Daily Star, (AZ), FINAL ed, pA1, Thursday, December 17, 2009 Record - 1 DIALOG(R) New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 TEXT: "In this paper we report on testing the 'rolen model' and 'opportunity-structure' hypotheses about the parents whom scientists mentioned as career influencers. According to the role-model hypothesis, the gender match between scientist and influencer is paramount (for example, women scientists would disproportionately often mention their mothers as career influencers)," scientists writing in the journal Social Studies of Science report (see also ). "According to the opportunity-structure hypothesis, the parent's educational level predicts his/her probability of being mentioned as a career influencer (that ism parents with higher educational levels would be more likely to be named). The examination of a sample of American scientists who had received prestigious postdoctoral fellowships resulted in rejecting the role-model hypothesis and corroborating the opportunity-structure hypothesis.
  • The Skyscraper 2009 05.Indd

    The Skyscraper 2009 05.Indd

    THE SKYSCRAPER • MAY 2009 A Better Galaxy Guide: Part 2, Late Spring Craig Cortis Those of you who enjoyed my first field eyepieces. the brighter objects listed and use what installment on this subject (in last Many of my choices here can be you’ve got. In closing, you might find month’s issue) will, I hope, find this seen in a 4-inch telescope and some it advisable to take another look at my second part to be even better. Three are doable in 50mm or larger binocu- article in last month’s issue. The intro- constellations are covered on the lars, but in general, I’d suggest using ductory section explains why I chose accompanying list of recommended telescopes of 6-to-8 inch aperture, at to come up with these observing lists objects and two—Virgo and Coma least for the galaxies. If you don’t own and also how they are planned. I hope Berenices-feature the grandest, richest a scope of that size range, just pick-out you’ll find my notes useful for star- assortment of galaxies bright enough to be seen in small-to-medium aperture Object Type R.A. Dec. Mag. Size Burnham’s instruments of all constellations in the sky, period. This “Virgo-Coma” cluster Virgo of galaxies is so crowded with objects M61 Sp Gx 12h 21.9m +04° 28’ 9.7 6.0x5.6’ v3, p. 2089-91 that trying to “zero-in” on only the best *M84 El Gx 12h 25.1m +12° 53’ 9.2 5.1x4.3’ v3, p.
  • Mètodes De Detecció I Anàlisi D'exoplanetes

    Mètodes De Detecció I Anàlisi D'exoplanetes

    MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits
  • From Monitoring Survey of Variable Red Giant Stars to the Evolution of the Galaxy: Andromeda Vii

    From Monitoring Survey of Variable Red Giant Stars to the Evolution of the Galaxy: Andromeda Vii

    Stars and their variability observed from space C. Neiner, W. W. Weiss, D. Baade, R. E. Griffin, C. C. Lovekin, A. F. J. Moffat (eds) FROM MONITORING SURVEY OF VARIABLE RED GIANT STARS TO THE EVOLUTION OF THE GALAXY: ANDROMEDA VII M. Navabi1, M. Noori2, E. Saremi1, A. Javadi1, J. van Loon3 and H. Khosroshahi1 Abstract. We have observed the Andromeda VII dwarf galaxy (And VII) using optical multi-epochs with the Isaac Newton Telescope (INT), in order to identify AGB stars. Among AGB stars, we concentrated on long-period variable stars (LPVs) with the largest amplitudes at optical wavelengths. Because these stars are cool at the end of their evolution and their luminosities reach maxima, their birth mass is directly related to luminosity by employing theoretical evolutionary tracks. Since the periods of LPVs are months to years, we have taken t10 epochs from And VII during the period 2015 − 2017, spaced by a month or more in the i- and V -bands, plus one epoch in the I-band, to find these variable stars. As a result, a catalogue of 10; 000 stars and 48 LPVs was identified within two halflight radii of And VII. The i−band amplitude of variability for our LPV stars ranged from 0:2{1:6 mag. We used the luminosity distribution of those stars to reconstruct their star formation history, employing a method that we have applied in the cases of other Local Group galaxies. By using as well the Spitzer catalogues at mid-IR wavelengths, we constructed a detailed map of the mass feedback into the interstellar medium (ISM).
  • Jahresbericht 2010 Mitteilungen Der Astronomischen Gesellschaft 94 (2013), 583–627

    Jahresbericht 2010 Mitteilungen Der Astronomischen Gesellschaft 94 (2013), 583–627

    Jahresbericht 2010 Mitteilungen der Astronomischen Gesellschaft 94 (2013), 583–627 Potsdam Leibniz-Institut für Astrophysik Potsdam (AIP) An der Sternwarte 16, D-14482 Potsdam Tel. 03317499-0, Telefax: 03317499-267 E-Mail: [email protected] WWW: http://www.aip.de Beobachtungseinrichtungen Robotisches Observatorium STELLA Observatorio del Teide, Izaña E-38205 La Laguna, Teneriffa, Spanien Tel. +34 922 329 138 bzw. 03317499-633 LOFAR-Station DE604 Potsdam-Bornim D-14469 Potsdam Tel. 03317499-291, Telefax: 03317499-352 Observatorium für Solare Radioastronomie Tremsdorf D-14552 Tremsdorf Tel. 03317499-291, Telefax: 03317499-352 Sonnenobservatorium Einsteinturm Telegrafenberg, D-14473 Potsdam Tel. 0331288-2303/-2304, Telefax: 03317499-524 0 Allgemeines Das Leibniz-Institut für Astrophysik Potsdam (AIP) ist eine Stiftung bürgerlichen Rechts zum Zweck der wissenschaftlichen Forschung auf dem Gebiet der Astrophysik. Als außer- universitäre Forschungseinrichtung ist es Mitglied der Leibniz-Gemeinschaft. Seinen For- schungsauftrag führt das AIP im Rahmen von nationalen und internationalen Kooperatio- nen aus. Die Beteiligung am Large Binocular Telescope auf dem Mt Graham in Arizona, dem größten optischen Teleskop der Welt, verdient hierbei besondere Erwähnung. Neben seinen Forschungsarbeiten profiliert sich das Institut zunehmend als Kompetenzzentrum im Bereich der Entwicklung von Forschungstechnologie. Vier gemeinsame Berufungen mit der Universität Potsdam und mehrere außerplanmäßige Professuren und Privatdozenturen an Universitäten in der Region und