DOCSLIB.ORG

Relativistic, 140 Abundance

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Relativistic, 140 Abundance 523 Index aberration – radio galaxies, 174 – of starlight, 224 – Seyfert galaxies, 174 – relativistic, 140 – unified model of, 175 abundance adiabatic – 4He, 53, 60, 64 – expansion, 7, 10, 40 – 7Li, 66 – perturbations, 89, 103, 104, 127, – cosmic, 36, 43 499 – deuterium, 52, 59, 64 affine – hydrogen, 66 – connection, 303, 342, 361 – neutron, 54, 56 – geometry, 334 – of lightest elements, 62 – manifold, 342 – primordial, 49, 61, 63, 195 – parameter, 305, 373, 505 accretion, 171, 177 – space, 334 – characteristic temperature, 179 Aharonov–Bohm effect, 330 – disk, 180 Alfven´ wave, 172 – magnetohydrodynamic instabil- annihilation ity, 180 – electron–positron, 44 – viscous torque, 183 – gluon–gluon, 193 acoustic – particle–antiparticle, 10, 20, 42, – damping, 131 221 – oscillations, 12, 118, 129, 135, antenna 487, 503 – beam solid angle, 151 – peak at 150 Mpc, 105, 118 – collecting area, 151 – peaks, 130, 145 – effective aperture, 151 – waves, 88, 104, 144 – feedhorn, 153 action integral, 267, 273 – main beam, 150 active galactic nuclei, 79, 171 – power pattern, 150 – blazars, 173 – side lobes, 150 – – BL Lacertae, 174 – temperature, 152 – quasars, 172 antimatter Relativity, Astrophysics and Cosmology Radoje Beluseviˇ c´ Copyright c 2008 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim ISBN: 978-3-527-40764-4 524 Index – presence in the universe, 21, 43, – – ergosphere, 172 198 – – frame dragging, 172 astronomical unit (AU), 421 – supermassive, 170–172, 182, 187, atomic 190 – clock, 214, 250, 252 black-hole era, 198 – energy levels bolometer, 14, 153 – – conjectured by Boltzmann, 2 Boltzmann – – in cyanogen, 16 – constant, 8 – equation, 73, 504 baryon, 29, 37 – – for photons, 508, 509 – bulk velocity, 508 – factor, 50 – density, 22, 128 BOOMERANG telescope, 13, 148 – density parameter, 38 Bose–Einstein – loading, 512 – distribution, 508 baryon-number conservation, 198 boson, 21, 42 baryon-photon fluid, 512 – star, 192 baryon-to-photon density ratio, brightness 510 – distribution of the sky, 157 baryon-to-photon ratio, 66 – function, 508 basis – of blackbody radiation, 133 – anholonomic, 375 – temperature, 152 – coordinate, 336, 407 – dyad, 338 Cartan – holonomic, 380 – calculus, 342, 361 – one-form, 335 – formula, 364 – orthonormal, 380 – formulation of Newtonian grav- – tensors, 338 ity, 31 – vectors, 334 – structural equations, 377, 407 Bianchi identity, 300, 306, 313, 352 Cassini spacecraft, 183 – contracted, 315, 317 CBI telescope array, 15, 148, 153, – first, 374, 378 159 – second, 374, 379 CCD array, 416 Big Bang, 4, 28, 192 celestial binding energy – coordinates, 141 – 4He, 52 – equator, 160, 424 – deuterium, 51, 53 – sphere, 148, 165, 424, 475 – gravitational, 247 Cepheids, see stars – of lightest nuclei, 60 chemical Birkhoff’s theorem, 24, 257 – equilibrium, 38, 44 black hole, 163, 171, 198 – potential, 21, 42 – accretion, 182, 187 Cherenkov – rotating (Kerr) – radiation, 228 Index 525 Christoffel symbol, 275, 278, 293, conformal 295, 303, 376, 495 – mapping, 459 CMB, 4, 82 – time, 458 – angular power spectrum, 15, congruence of geodesics, 372 130, 137, 146 – connecting vector, 372 – dipole anisotropy, 121, 141 connection – discovery of, 10, 195 – coefficients, 294, 367, 368, 371 – energy density, 18, 36 – Koszul, 365 – foregrounds, 146, 147 – one-form, 376, 407 – lensing, 445, 478 continuity equation, 25, 85, 87, – map, 15, 149 122, 305, 324, 353 – multipole expansion, 135 contravariant – observational techniques, 146 – basis vectors, 270 – photons, 90 – components, 277, 296 – polarimeter, 485 – transformation rule, 277, 288 – polarization, 14, 81, 485, 489 convolution theorem, 158 – – (E,B)-type patterns, 487 coordinate transformations – – anisotropy, 478, 487 – Bardeen variables, 494 – – power spectrum, 480, 488 – gauge freedom, 491 – – WMAP measurement, 487 coordinates – primary anisotropies, 127 – Cartesian, 32, 89, 265, 278, 280, – secondary anisotropies, 131, 146 299, 347 – spectrum, 13 – celestial, 141 – temperature, 8, 12 – curvilinear, 240, 280 – – anisotropy, 142, 149, 157, 487 – galactic, 141 – – power spectrum, 15, 130, 137, – generalized, 265 143, 488 – spherical, 240 CMBFAST code, 105, 114 – system of, 334 co-moving Coriolis force, 282 – coordinates, 387, 458 correlation function, 107, 137 – distance, 412 cosmic – frame, 86, 387 – baryons, 67 – observer, 387, 390, 505 – dark age, 481 – wavevector, 88, 502 – energy density, 29 COBE telescope, 13, 148 – fluid, 130, 387, 395, 398, 489 collision rate, 37 – lens, 461 color index, 417 – photosphere, 11, 106, 195 Compton – rays, 213 – scattering, 12 – shear, 468, 471 – – inverse, 132, 436 – time, 6, 9, 30, 387, 439 configuration space, 265 – variance, 138, 139, 488 526 Index cosmic expansion covariant – accelerated, 27, 196, 398, 402, 443 – basis vectors, 269 – decelerated, 395, 443 – components, 270, 271, 277, 296 – deceleration parameter, 391 – derivative, 296, 308, 366 – scale parameter, 7 – formulation, 232 cosmic inflation, 514 – tensor, 290 – chaotic, 517 – transformation rule, 277, 288 – density perturbations, 517 Crab Nebula, 207 – quantum fluctuations, 514 critical density, 29, 396 – reheating, 516 curvature – scalar field φ, 514 – extrinsic, 311 – slow-roll approximation, 516 – forms, 361 cosmic microwave background, – intrinsic, 302, 307, 311, 330 see CMB – of manifold, 331 cosmological – of spacetime, 35, 111, 253, 319, – constant, 27, 30, 104, 142, 401, 396 402, 440, 515 – parameter, 27, 30 – fluctuations – perturbations, 489, 494, 518 – – acoustic dynamics, 509, 511 – radius of, 397 – – adiabatic, 499 – scalar, 496 – – dust-dominated universe, 501 – tensor, 369 – – Einstein equations, 495 cyanogen excitation, 17 – – gauge transformation, 491 cyclotron frequency, 234 – – Newtonian theory, 82 – – radiation-dominated universe, d’Alembertian, 299 503 dark energy, 30, 196, 402 – – relativistic theory, 489 dark halo, 77, 101 – – scalar, 491 dark matter, 29, 77, 92, 96, 103, – – tensor, 491 104, 162 – – tight-coupling limit, 510 dark-sky paradox, 17 ––vector,491 DASI telescope array, 14, 148, 159, – hypothesis, 4, 82, 86 485 – parameters, 142 de Broglie Coulomb – wavelength, 9 – barrier, 52 Debye – force, 21 – length, 23 – potential, 23 – shielding, 21 – scattering, 235 degenerate covariance – era, 198 – matrix, 158 density – of tensors, 288 – contrast, 87, 106 – energy, 39 Index 527 – fluctuations, 106 – tensor, 316, 382, 406, 496 – number, 39 Einstein, Albert, 316 – parameter, 29 Einstein–de Sitter model, 89, 123 – phase-space, 55 electromagnetic detailed balance, 54, 74 – four-potential, 272 differential forms, 342 electromagnetic field – coderivative operator, 354 – tensor, 273 – exterior derivative, 343, 349 electroweak – Hodge star operator, 347 – symmetry, 192 – inner product, 358 ellipse, 465 – interior product, 363 ensemble – one-form, 333, 342 – average, 108, 137, 138, 487 – two-form, 343, 377, 408 – average power, 109 – wedge product, 344 entropy differential geometry, 331 – conservation of, 7, 42 Dirac – density, 22, 40, 41 – delta function, 109 equinox, 423 – monopole, 330 equivalence principle, 247 directional derivative, 332 – strong, 247 distance modulus, 415, 424, 427, – weak, 247 440 ergodic hypothesis, 108, 138 distribution function, 38, 45, 508 ether, 204, 215, 228, 229 Doppler effect, 97, 129, 134, 140, Euclidean 220, 221, 226, 249, 262 – geometry, 394 dual field tensor, 306, 353 – space, 25, 27, 31, 239, 299, 333 Euler’s equation, 25, 85, 87, 324 ecliptic Euler–Lagrange equations, 265 – coordinates, 456 extragalactic distance – definition of, 424 – angular-diameter distance, 413, – latitude, 223 449 – plane of, 224, 423 – co-moving distance, 412 Eddington – distance ladder, 420 – limit, 178 – expanding photosphere method, Einstein 434 – field equations, 320, 496 – fundamental plane relation, 432 – – conservation laws, 319 – fundamental rung, 427 – – coordinate transformations, – luminosity distance, 412, 419, 317 440 – – for empty space, 316 – primary indicator, 435 – – from variational principle, 324 – proper distance, 389 – – weak-field limit, 320 – summation convention, 239, 271 528 Index – secondary indicator, 426, 427, – winds, 188 432, 438 galaxy – to Large Magellanic Cloud, 426 – Andromeda, 28, 165 – Tully–Fisher relation, 123, 430 – biasing, 119 – classification, 168 Fermat’s principle, 253, 269 – correlation function, 105, 107 fermion, 21, 42 – dwarf, 98, 159 Feynman – elliptical, 98, 159, 169, 188 – path integral approach, 325 – irregular, 170 first stars, 77, 195 – lenticular, 169 Fizeau’s experiment, 229 – Local Group, 141, 165 flux – Magellanic Clouds, 165 – definition of, 413 – Milky Way, 121, 160, 189 – of angular momentum, 184 – morphological evolution, 187 flux density, 399, 413 – nonlinear evolution, 119 – incident on antenna, 150 – peculiar motion, 121 – of starlight, 414 – redshift distortions, 121 Foucault pendulum, 302 – – finger-of-God effect, 126 Fourier – rotation curve, 97 – decomposition, 135 – Sombrero, 170 – modes, 108, 110 – spiral, 97, 168, 188 – series, 88 – spiral arms, 160, 168 – space, 108 – starburst, 188 – transform, 109, 157 – Whirlpool, 170 Fresnel drag coefficient, 229 galaxy cluster, 98, 195 Friedmann–Lemaˆıtre – Abell 2029, 99 – equations, 27, 387, 395, 406, 410, – Centaurus, 141 500 – Coma, 165 – – derivation of, 402 – Virgo, 124, 165 – model, 4, 82, 459, 475 galaxy redshift survey – universe, 27, 395, 407, 440, 472 – 2MASS, 167 fusion – 2dFGRS, 83, 115 – Gamow – CfA, 116 – – condition, 37 – DEEP2, 116 – SDSS, 115 galactic Galilean relativity, 203 – bulge, 160 Galilei, Galileo, 162 – center, 160 gamma-ray – disk,
Load more

Recommended publications
  • Multiwavelength Observations of Accretion in Low-Mass X-Ray Binary Systems Robert I
    1 Multiwavelength Observations of Accretion in Low-Mass X-ray Binary Systems Robert I. Hynesa Abstract This work is intended to provide an introduction to multiwavelength observations of low-mass X-ray binaries and the techniques used to ana- lyze and interpret their data. The focus will primarily be on ultraviolet, optical, and infrared observations and their connections to other wave- lengths. The topics covered include: outbursts of soft X-ray transients, accretion disk spectral energy distributions, orbital lightcurves in lumi- nous and quiescent states, super-orbital and sub-orbital variability, line spectra, system parameter determinations, and echo-mapping and other rapid correlated variability. 1.1 Introduction The first X-ray binary to be observed and identified as such was Scorpius X-1 (Giacconi et al., 1962), although several other systems were known as optical stars or novae before this. Within a few years, optical and radio counterparts to Sco X-1 were discovered (Sandage et al., 1966; Andrew and Purton, 1968), and the topic has remained multiwavelength in nature since then. This work is intended to provide an introduction to some of the obser- vational characteristics of X-ray binaries suitable for a graduate student or an advanced undergraduate. My aim was to produce a primer for someone relatively new to the field rather than a comprehensive review. Where appropriate I will also discuss techniques for analysis and inter- a Louisiana State University, Department of Physics and Astronomy, 202 arXiv:1010.5770v1 [astro-ph.HE] 27 Oct 2010 Nicholson Hall, Tower Drive, Baton Rouge, LA 70803, USA 2 R.
    [Show full text]
  • Star Maps: Where Are the Black Holes?
    BLACK HOLE FAQ’s 1. What is a black hole? A black hole is a region of space that has so much mass concentrated in it that there is no way for a nearby object to escape its gravitational pull. There are three kinds of black hole that we have strong evidence for: a. Stellar-mass black holes are the remaining cores of massive stars after they die in a supernova explosion. b. Mid-mass black hole in the centers of dense star clusters Credit : ESA, NASA, and F. Mirabel c. Supermassive black hole are found in the centers of many (and maybe all) galaxies. 2. Can a black hole appear anywhere? No, you need an amount of matter more than 3 times the mass of the Sun before it can collapse to create a black hole. 3. If a star dies, does it always turn into a black hole? No, smaller stars like our Sun end their lives as dense hot stars called white dwarfs. Much more massive stars end their lives in a supernova explosion. The remaining cores of only the most massive stars will form black holes. 4. Will black holes suck up all the matter in the universe? No. A black hole has a very small region around it from which you can't escape, called the “event horizon”. If you (or other matter) cross the horizon, you will be pulled in. But as long as you stay outside of the horizon, you can avoid getting pulled in if you are orbiting fast enough. 5. What happens when a spaceship you are riding in falls into a black hole? Your spaceship, along with you, would be squeezed and stretched until it was torn completely apart as it approached the center of the black hole.
    [Show full text]
  • The Nova-Like Nebular Optical Spectrum of V404 Cygni at The
    MNRAS 000, i–xvi (2016) Preprint 4 October 2018 Compiled using MNRAS LATEX style file v3.0 The nova-like nebular optical spectrum of V404 Cygni at the beginning of the 2015 outburst decay Farid Rahoui1,2⋆, J. A. Tomsick3, P. Gandhi4, P. Casella5, F. Furst¨ 6, L. Natalucci7, A. Rossi8, A. W. Shaw4, V. Testa5, and D. J. Walton6 1European Southern Observatory, K. Schwarzschild-Str. 2, 85748 Garching bei Munchen,¨ Germany 2Department of Astronomy, Harvard University, 60 Garden street, Cambridge, MA 02138, USA 3Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720-7450, USA 4Department of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ, UK 5INAF-OA Roma, Via Frascati 33, I-00078 Monteporzio Catone, Italy 6California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA 7Istituto di Astrofisica e Planetologia Spaziali, INAF, Via Fosso del Cavaliere 100, I-00133 Roma, Italy 8INAF-IASF Bologna, Area della Ricerca CNR, via Gobetti 101, I–40129 Bologna, Italy Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We report on FORS2 optical spectroscopy of the black hole X-ray binary V404 Cygni, performed at the very beginning of its 2015 outburst decay, complemented by quasi- simultaneous Swift X-ray and ultra-violet as well as REM near-infrared observations. Its peculiar spectrum is dominated by a wealth of emission signatures of H i, He i, and higher ionisation species, in particular Fe ii. The spectral features are divided between broad red-shifted and narrow stationary varieties, the latter being emitted in the outer regions.
    [Show full text]
  • Annual Report 2016–2017 AAVSO
    AAVSO The American Association of Variable Star Observers Annual Report 2016–2017 AAVSO Annual Report 2012 –2013 The American Association of Variable Star Observers AAVSO Annual Report 2016–2017 The American Association of Variable Star Observers 49 Bay State Road Cambridge, MA 02138-1203 USA Telephone: 617-354-0484 Fax: 617-354-0665 email: [email protected] website: https://www.aavso.org Annual Report Website: https://www.aavso.org/annual-report On the cover... At the 2017 AAVSO Annual Meeting.(clockwise from upper left) Knicole Colon, Koji Mukai, Dennis Conti, Kristine Larsen, Joey Rodriguez; Rachid El Hamri, Andy Block, Jane Glanzer, Erin Aadland, Jamin Welch, Stella Kafka; and (clockwise from upper left) Joey Rodriguez, Knicole Colon, Koji Mukai, Frans-Josef “Josch” Hambsch, Chandler Barnes. Picture credits In additon to images from the AAVSO and its archives, the editors gratefully acknowledge the following for their image contributions: Glenn Chaple, Shawn Dvorak, Mary Glennon, Bill Goff, Barbara Harris, Mario Motta, NASA, Gary Poyner, Msgr. Ronald Royer, the Mary Lea Shane Archives of the Lick Observatory, Chris Stephan, and Wheatley, et al. 2003, MNRAS, 345, 49. Table of Contents 1. About the AAVSO Vision and Mission Statement 1 About the AAVSO 1 What We Do 2 What Are Variable Stars? 3 Why Observe Variable Stars? 3 The AAVSO International Database 4 Observing Variable Stars 6 Services to Astronomy 7 Education and Outreach 9 2. The Year in Review Introduction 11 The 106th AAVSO Spring Membership Meeting, Ontario, California 11 The
    [Show full text]
  • Repetitive Patterns in Rapid Optical Variations in the Nearby Black-Hole Binary V404 Cygni
    Repetitive Patterns in Rapid Optical Variations in the Nearby Black-hole Binary V404 Cygni Mariko Kimura1, Keisuke Isogai1, Taichi Kato1, Yoshihiro Ueda1, Satoshi Nakahira2, Megumi Shidatsu3, Teruaki Enoto1,4, Takafumi Hori1, Daisaku Nogami1, Colin Littlefield5, Ryoko Ishioka6, Ying-Tung Chen6, Sun-Kun King6, Chih-Yi Wen6, Shiang-Yu Wang6, Matthew J. Lehner6,7,8, Megan E. Schwamb6, Jen-Hung Wang6, Zhi-Wei Zhang6, Charles Alcock8, Tim Axelrod9, Federica B. Bianco10, Yong-Ik Byun11, Wen-Ping Chen12, Kem H. Cook6, Dae-Won Kim13, Typhoon Lee6, Stuart L. Marshall14, Elena P. Pavlenko15, Oksana I. Antonyuk15, Kirill A. Antonyuk15, Nikolai V. Pit15, Aleksei A. Sosnovskij15, Julia V. Babina15, Aleksei V. Baklanov15, Alexei S. Pozanenko16,17, Elena D. Mazaeva16, Sergei E. Schmalz18, Inna V. Reva19, Sergei P. Belan15, Raguli Ya. Inasaridze20, Namkhai Tungalag21, Alina A. Volnova16, Igor E. Molotov22, Enrique de Miguel23,24, Kiyoshi Kasai25, William Stein26, Pavol A. Dubovsky27, Seiichiro Kiyota28, Ian Miller29, Michael Richmond30, William Goff31, Maksim V. Andreev32,33, Hiromitsu Takahashi34, Naoto Kojiguchi35, Yuki Sugiura35, Nao Takeda35, Eiji Yamada35, Katsura Matsumoto35, Nick James36, Roger D. Pickard37,38, Tamás Tordai39, Yutaka Maeda40, Javier Ruiz41,42,43, Atsushi Miyashita44, Lewis M. Cook45, Akira Imada46 & Makoto Uemura47 1Department of Astronomy, Graduate School of Science, Kyoto University, Oiwakecho, Kitashirakawa, Sakyo-ku, Kyoto 606-8502, Japan! 2JEM Mission Operations and Integration Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan 3MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan 4The Hakubi Center for Advanced Research, Kyoto University, Kyoto 606-8302, Japan 5Astronomy Department, Wesleyan University, Middletown, CT 06459 USA !6Institute of Astronomy and Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU.
    [Show full text]
  • To Read Notes on Black Holes
    Required reading Why are we so sure that black holes are real, and that we have found them? “Extraordinary claims require extraordinary evidence.” – Attributed to Carl Sagan (1) “We know that neutron stars exist, and black holes are pretty close!” This isn’t a strong argument. Just because it’s plausible doesn’t mean it must exist. Horses are almost unicorns, and we know that horses exist, but this doesn’t imply that unicorns must exist. (2) To hold up against collapse, a neutron star with a mass of greater than 3 Suns would have to be made of material that’s infinitely strong. Indeed, nuclear theory predicts how strong neutron star material should be: a realistic neutron star should collapse, if it had a mass greater than 2.7 + 0.3 Suns. Can we find a compact object with a mass we can prove is greater than 3 Suns? We measure mass of stars (and black holes) with Kepler’s Third Law, from the strength of gravity as they orbit each other. From Kepler’s third law, m = a3/P2 (m = mass in Suns; a = semi-major axis or orbital separation in AU; P = orbital period in years). This is done by getting spectra of the binary star system all around the orbit, and measuring how much the stars’ gravity pull each other around by measuring the Doppler shift. This is similar to how we detect planets around other stars, by measuring how their gravity pulls their parent stars around. The compact star in the binary star system Cygnus X-1 for many years (from 1971 to 1992) was hailed as the most likely black hole candidate, but the case wasn’t decisive.
    [Show full text]
  • Postępy Astronomii Nr 4/2015
    DODATEK DLA PRENUMERATORÓW: KOLOROWA BROSZURA ESO 4/2015 (778) lipiec–sierpień Tom LXXXVI ukazuje się od 1920 r. Cena 12,90 zł w tym 5% VAT www.urania.edu.pl Którędy do czarnej dziury? Tajemniczy świat Plutona ISSN 1689-6009 indeks 401323 Komu potrzebne 4/2015 ciemneUrania niebo? 1 URANIA – NASZA MUZA dla szkół, uczelni oraz miłośników astronomii i amatorów nocnego nieba (PL ISSN 1689-6009) Dwumiesięcznik poświęcony upowszech- oniec lata. Pracowitego lata. Do pocztu najpracowitszych kolegów na świecie, nianiu wiedzy astronomicznej. Czasopismo powstałe w roku 1998 z połączenia „Uranii” oprócz opisywanych niedawno twórców obserwatoriów w Truszczynach (ISSN 0042-0794) — dotychczasowego i Rzepienniku, muszę dołączyć Karola Wenerskiego, miłośnika astronomii miesięcznika Polskiego Towarzystwa Mi- z Bydgoszczy, twórcę i budowniczego, jeśli nie największego — lustro łośników Astronomii, ukazującego się od 1920 r. i „Postępów Astronomii” (ISSN Kszczecińskiej SOWY jest chyba identyczne, 63 cm — to na pewno najpiękniejszego, 0032-5414) — dotychczasowego kwartal- amatorskiego teleskopu w Polsce. Ktoś ze wspólnych przyjaciół z Pałucko-Pomorskiego nika Polskiego Towarzystwa Astronomicz- Stowarzyszenie Astronomiczno-Ekologicznego po minimalnej stawce policzył nego, wychodzącego od 1953 r. Zachowana zostaje dotychczasowa numeracja „Uranii”. roboczogodziny Karola spędzającego w Obserwatorium w Niedźwiadach weekend Pismo częściowo finansowane przez: w weekend od kilku lat i wyszedł koszt robocizny sto kilkadziesiąt tysięcy złotych! Na swoje plastyczne i techniczne talenty chyba Karol nie ma żadnych papierów, ale za sprawą jego dzieła nie zdziwiłbym się, gdyby nagle dostał propozycję pracy w NASA! A to jeszcze nic! Pamiętam Karola sprzed ponad już dwudziestu lat jako najbardziej nietuzinkowego Nakład: 3000 egz. wychowawcę młodzieży, jakiego poznałem. Zespół Redakcyjny: Miałem cudowną okazję gościć kilkukrotnie Krzysztof Czart (serwis www, redaktor) grupę jego podopiecznych z bydgoskiego Jan Desselberger (kalendarz astronomiczny) Jacek Drążkowski (red.
    [Show full text]
  • New Type of Black Hole Detected in Massive Collision That Sent Gravitational Waves with a 'Bang'
    New type of black hole detected in massive collision that sent gravitational waves with a 'bang' By Ashley Strickland, CNN Updated 1200 GMT (2000 HKT) September 2, 2020 <img alt="Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image." class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190516104725-ngc-4485-nasa-super-169.jpg"> Photos: Wonders of the universe Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image. Hide Caption 98 of 195 <img alt="Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. " class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190502151952-0502-wonders-of-the-universe-super-169.jpg"> Photos: Wonders of the universe Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. Hide Caption 99 of 195 <img alt="A ground-based telescope's view of the Large Magellanic Cloud, a neighboring galaxy of our Milky Way.
    [Show full text]
  • Black Hole Math Is Designed to Be Used As a Supplement for Teaching Mathematical Topics
    National Aeronautics and Space Administration andSpace Aeronautics National ole M a th B lack H i This collection of activities, updated in February, 2019, is based on a weekly series of space science problems distributed to thousands of teachers during the 2004-2013 school years. They were intended as supplementary problems for students looking for additional challenges in the math and physical science curriculum in grades 10 through 12. The problems are designed to be ‘one-pagers’ consisting of a Student Page, and Teacher’s Answer Key. This compact form was deemed very popular by participating teachers. The topic for this collection is Black Holes, which is a very popular, and mysterious subject among students hearing about astronomy. Students have endless questions about these exciting and exotic objects as many of you may realize! Amazingly enough, many aspects of black holes can be understood by using simple algebra and pre-algebra mathematical skills. This booklet fills the gap by presenting black hole concepts in their simplest mathematical form. General Approach: The activities are organized according to progressive difficulty in mathematics. Students need to be familiar with scientific notation, and it is assumed that they can perform simple algebraic computations involving exponentiation, square-roots, and have some facility with calculators. The assumed level is that of Grade 10-12 Algebra II, although some problems can be worked by Algebra I students. Some of the issues of energy, force, space and time may be appropriate for students taking high school Physics. For more weekly classroom activities about astronomy and space visit the NASA website, http://spacemath.gsfc.nasa.gov Add your email address to our mailing list by contacting Dr.
    [Show full text]
  • Paving the Way to Simultaneous Multi-Wavelength Astronomy
    Paving the way to simultaneous multi-wavelength astronomy M. J. Middleton,∗ P. Casella, P. Gandhi, E. Bozzo, G. Anderson, N. Degenaar, I. Donnarumma, G. Israel, C. Knigge, A. Lohfink, S. Markoff, T. Marsh, N. Rea, S. Tingay, K. Wiersema, D. Altamirano, D. Bhattacharya, W. N. Brandt, S. Carey, P. Charles, M. Diaz Trigo, C. Done, M. Kotze, S. Eikenberry, R. Fender, P. Ferruit, F. Fuerst, J. Greiner, A. Ingram, L. Heil, P. Jonker, S. Komossa, B. Leibundgut, T. Maccarone, J. Malzac, V. McBride, J. Miller-Jones, M. Page, E. M. Rossi, D. M. Russell, T. Shahbaz, G. R. Sivakoff, M. Tanaka, D. J. Thompson, M. Uemura, P. Uttley, G. van Moorsel, M. Van Doesburgh, B. Warner, B. Wilkes, J. Wilms, P. Woudt 1 Introduction Whilst astronomy as a science is historically founded on observations at optical wavelengths, studying the Universe in other bands has yielded remarkable discoveries, from pulsars in the radio, signatures of the Big Bang at submm wavelengths, through to high energy emission from accreting, gravitationally-compact objects and the discovery of gamma-ray bursts. Unsurpris- ingly, the result of combining multiple wavebands leads to an enormous increase in diagnostic power, but powerful insights can be lost when the sources studied vary on timescales shorter than the temporal separation between observations in different bands. In July 2015, the work- shop “Paving the way to simultaneous multi-wavelength astronomy” was held as a concerted effort to address this at the Lorentz Center, Leiden. It was attended by 50 astronomers from diverse fields as well as the directors and staff of observatories and spaced-based missions.
    [Show full text]
  • Download PDF of Abstracts
    15th HEAD Naples, FL – April, 2016 Meeting Program Session Table of Contents 100 – AGN I Analysis Poster Session 206 – Early Results from the Astro-H 101 – Galaxy Clusters 116 – Missions & Instruments Poster Mission 102 – Dissertation Prize Talk: Accretion Session 207 – Stellar Compact II driven outflows across the black hole mass 117 – Solar and Stellar Poster Session 300 – The Physics of Accretion Disks – A scale, Ashley King (KIPAC/Stanford 118 – Supernovae and Supernova Joint HEAD/LAD Session University) Remnants Poster Session 301 – Gravitational Waves 103 – Time Domain Astronomy 119 – WDs & CVs Poster Session 302 – Missions & Instruments 104 – Feedback from Accreting Binaries in 120 – XRBs and Population Surveys Poster 303 – Mid-Career Prize Talk: In the Ring Cosmological Scales Session with Circinus X-1: A Three-Round Struggle 105 – Stellar Compact I 200 – Solar Wind Charge Exchange: to Reveal its Secrets, Sebastian Heinz 106 – AGNs Poster Session Measurements and Models (Univ. of Wisconsin) 107 – Astroparticles, Cosmic Rays, and 201 – TeraGauss, Gigatons, and 304 – Science of X-ray Polarimetry in the Neutrinos Poster Session MegaKelvin: Theory and Observations of 21st Century 108 – Cosmic Backgrounds and Deep Accretion Column Physics 305 – Making the Multimessenger – EM Surveys Poster Session 202 – The Structure of the Inner Accretion Connection 109 – Galactic Black Holes Poster Session Flow of Stellar-Mass and Supermassive 306 – SNR/GRB/Gravitational Waves 110 – Galaxies and ISM Poster Session Black Holes 400 – AGN II 111 – Galaxy
    [Show full text]
  • Black Holes by John Percy, University of Toronto
    www.astrosociety.org/uitc No. 24 - Summer 1993 © 1993, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112. Black Holes by John Percy, University of Toronto Gravity is the midwife and the undertaker of the stars. It gathers clumps of gas and dust from the interstellar clouds, compresses them and, if they are sufficiently massive, ignites thermonuclear reactions in their cores. Then, for millions or billions of years, they produce energy, heat and pressure which can balance the inward pull of gravity. The star is stable, like the Sun. When the star's energy sources are finally exhausted, however, gravity shrinks the star unhindered. Stars like the Sun contract to become white dwarfs -- a million times denser than water, and supported by quantum forces between electrons. If the mass of the collapsing star is more than 1.44 solar masses, gravity overwhelms the quantum forces, and the star collapses further to become a neutron star, millions of times denser than a white dwarf, and supported by quantum forces between neutrons. The energy released in this collapse blows away the outer layers of the star, producing a supernova. If the mass of the collapsing star is more than three solar masses, however, no force can prevent it from collapsing completely to become a black hole. What is a black hole? Mini black holes How can you "see'' a Black Hole? Supermassive black holes Black holes and science fiction Activity #1: Shrinking Activity #2: A Scale Model of a Black Hole Black hole myths For Further Reading About Black Holes What is a black hole? A black hole is a region of space in which the pull of gravity is so strong that nothing can escape.
    [Show full text]