DOCSLIB.ORG

AS1001:Extra-Galactic Astronomy

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
AS1001:Extra-Galactic Astronomy AS1001:Extra-Galactic Astronomy Lecture 6: Galaxy Orientation, Black Holes & Quasars Simon Driver Theatre B [email protected] http://www-star.st-and.ac.uk/~spd3 Galaxy Inclination FACE-ON EDGE-ON o o Inclination=0 Inclination=90 b=Minor Axis Majority of galaxies are somewhere in between a=Major Axis Calculating the Inclination • Assuming galaxies are circular: b cos(i) = • Inclination, i, is given by: a b i a • a=b, i=0o • b=0, i=90o NB: a is always measurable Line-of-sight velocity When we measure the rotational velocity from a spectral line we need to correct for inclination. i vobs Line-of-sight velocity i v rot Hence if, i=90 , V = V obs rot VOBS VROT = i=0 , Vobs = 0 sin(i) Example A long slit spectrum aligned along a galaxy’s major axis indicates a variation in the OII line of 5A, The midpoint of the OII line is observed to be at 3900A and the major-to-minor axis ratio is 3. What is the rotational velocity of the outermost stars ? i = cos!1(1/ 3) = 70.50 Note: 5/2 A "# 2.5 V = c = !3!105 =192km / s OBS # 3900 V Note: λ=3900 V = OBS = 204km / s ROT sin(i) and not 3727 Black Holes Gravity is the curvature of space-time by matter. If sufficient mass exists in a small enough volume space- time is distorted such that even light cannot escape The Schwarzschild Radius • The radius at which even light cannot escape is known as the event horizon or Schwarzschild radius. • For a non-rotating black hole this is simply when the Kinetic Energy = Gravitational Energy for a photon 1 GMm mv2 = 2 r 1 GMm mc2 = 2 rS 2GM rS = 2 rs c Types of Black Hole • Normal – Formed from massive stars going supernovae MBH ~ 10M! • Super-massive – Formed in galaxy cores during initial collapse 7"9 MBH ~ 10 M! • Most galaxies are believed to harbour a super-massive black-hole in their cores Evidence for SMBHs • We find that stars have velocities of >110km/s within 2.5pc of the core of M31 Super-massive BH in M31 • IF they are in circular orbits we can use the Virial theorem to calculate the mass inside r v2r (110#103 )2 # 2.5#3#1016 M = = CORE G 6.67#10"11 37 6 MCORE =1.4#10 kg = 6.8#10 M! • In our Milky Way galaxy – Velocities > 1000 km/s inside 0.01 pc! 6 • => 2 x 10 Msun SMBH Quasars • Quasi-Stellar Objects (aka QSOs) • For many years “stars” with unknown spectral features were found but their nature unknown ! • In 1963 Martin Schmidt took a closer look and noticed these bright stellar-like objects have features consistent with very large redshifts (>> galaxies) ? • Hence QSOs are extra-galactic objects but: – Appear star-like (i.e., not extended but point-like) – Are more intrinsically luminous than galaxies (up to 105 more luminous; M ~ -26 mags) – Exhibit very broad emission line features (Δv ~ 10000 km/s) – Emit strongly in the X-ray (Synchrotron Radiation) A Quasars Energy Output • Unlike most astronomical objects QSOs show non-thermal spectra (thermal=Blackbody). • This is consistent with Synchrotron Radiation, this is produced by relativistic particles spiralling along magnetic field lines. The QSO Model SUPER-MASSIVE POLAR OUTFLOWS BLACK HOLE OF RELATIVISTIC PARTICLES ALONG MAGNETIC FIELD LINES (JETS) INFALLING STARS ACCRETION DISK CRUSHED BY OF CRUSHED GRAVITY FIELD STARS AND GAS Types of Active Galactic Nuclei • Very deep HST images show that QSOs are normally embedded in the cores of galaxies. • These cores are called Active Galactic Nuclei (AGN) – If the AGN outshines the host galaxy = Quasar – If the AGN has radio lobes = Radio Galaxy – If the AGN luminosity equals host galaxy = Seyfert Galaxy – If the core shows high variability = Blazar WHY ? AGN Unification Current theory suggests all these AGN are due to the same process viewed from different orientations: Sees a BLAZAR Sees a Sees a RADIO QUASAR GALAXY Quasars in the Universe • Redshift surveys indicate that most quasars have z > 0.3 • In later lectures we’ll see that large redshifts means large distances or large “lookback times,” i.e., we are seeing objects as they looked when the Universe was very young • Nearest quasar is about 250 Mpc or 800 million light years from Earth • Therefore, no new quasars for ~ billion years • Quasars were common in the early Universe, then died out Galaxy Formation • It appears that every galaxy harbours a Super- Massive Black Hole and that when swallowing stars it results in an Active Galactic nucleus. • During a mad feeding frenzy the galaxy will temporarily become a Quasar which outshines the rest of the galaxy by a factor of 1000 or more. • SMBH, AGN activity, and Quasars may represent an integral and key clue to galaxy formation however the exact details remain to be discovered. SMBH Model/Observations MODEL OBSERVATIONS (NGC4261) Tutorial 2, Question 5 Density = Mass/Volume = n * MGal = n * LGal * MGal / LGal = n * LGal * 10 * Msun/Lsun = n * LGal/Lsun * 10 * Msun -0.4(MG-MS) = 10 * n * Msun * 10 Assume all galaxies have same mass and luminosity Mgal = Mass of a galaxy; Lgal = Galaxy luminosity Msun = mass of sun; Lsun =Sun’s luminosity MG = galaxy absolute magnitude MS = Sun’s absolute magnitude, use MS = 5.48 Super-massive BH in M31 • IF they are in circular orbits we can use the Virial theorem to calculate the mass inside r v2r (110#103 )2 # 2.5#3#1016 M = = CORE G 6.67#10"11 37 6 MCORE =1.4#10 kg = 6.8#10 M! • The escape velocity required to leave this region is therefore: 2GM v = r 2!6.67!10"11 !1.4!1037 • => SMBH ? v = 2.5!3!1016 v =160000 = 0.5c! Black Holes Evaporate Annihilation Particle escapes, removing E = mc2 Particle Anti-particle Creation Virtual Pair rs Black Holes Evaporate • Hawking Radiation unites gravity, thermodynamics and quantum dynamics • Black holes radiate with a temperature 3 hG M bh h c k T = 2 2 = 2 4! c rs 16! G M bh 2 4 • Luminosity is Lbh = 4" rs ! T 2 • Energy available is Ebh = M bhc • Black hole evaporates in time Tbh = Ebh / Lbh 15 • Mbh = 10 kg (Everest): Tbh = 15 billion years 62 • Mbh = 5M: Tbh = 10 years.
Load more

Recommended publications
  • ASTR 503 – Galactic Astronomy Spring 2015 COURSE SYLLABUS
    ASTR 503 – Galactic Astronomy Spring 2015 COURSE SYLLABUS WHO I AM Instructor: Dr. Kurtis A. Williams Office Location: Science 145 Office Phone: 903-886-5516 Office Fax: 903-886-5480 Office Hours: TBA University Email Address: [email protected] Course Location and Time: Science 122, TR 11:00-12:15 WHAT THIS COURSE IS ABOUT Course Description: Observations of galaxies provide much of the key evidence supporting the current paradigms of cosmology, from the Big Bang through formation of large-scale structure and the evolution of stellar environments over cosmological history. In this course, we will explore the phenomenology of galaxies, primarily through observational support of underlying astrophysical theory. Student Learning Outcomes: 1. You will calculate properties of galaxies and stellar systems given quantitative observations, and vice-versa. 2. You will be able to categorize galactic systems and their components. 3. You will be able to interpret observations of galaxies within a framework of galactic and stellar evolution. 4. You will prepare written and oral summaries of both current and fundamental peer- reviewed articles on galactic astronomy for your peers. WHAT YOU ABSOLUTELY NEED Materials – Textbooks, Software and Additional Reading: Required: • Galactic Astronomy, Binney & Merrifield 1998 (Princeton University Press: Princeton) • Access to a desktop or laptop computer on which you can install software, read PDF files, compile code, and access the internet. Recommended: • Allen’s Astrophysical Quantities, 4th Edition, Arthur Cox, 2000 (Springer) Course Prerequisites: Advanced undergraduate classical dynamics (equivalent of Phys 411) or Phys 511. HOW THE COURSE WILL WORK Instructional Methods / Activities / Assessments Assigned Readings There is far too much material in the text for us to cover every single topic in class.
    [Show full text]
  • PHYS 1302 Intro to Stellar & Galactic Astronomy
    PHYS 1302: Introduction to Stellar and Galactic Astronomy University of Houston-Downtown Course Prefix, Number, and Title: PHYS 1302: Introduction to Stellar and Galactic Astronomy Credits/Lecture/Lab Hours: 3/2/2 Foundational Component Area: Life and Physical Sciences Prerequisites: Credit or enrollment in MATH 1301 or MATH 1310 Co-requisites: None Course Description: An integrated lecture/laboratory course for non-science majors. This course surveys stellar and galactic systems, the evolution and properties of stars, galaxies, clusters of galaxies, the properties of interstellar matter, cosmology and the effort to find extraterrestrial life. Competing theories that address recent discoveries are discussed. The role of technology in space sciences, the spin-offs and implications of such are presented. Visual observations and laboratory exercises illustrating various techniques in astronomy are integrated into the course. Recent results obtained by NASA and other agencies are introduced. Up to three evening observing sessions are required for this course, one of which will take place off-campus at George Observatory at Brazos Bend State Park. TCCNS Number: N/A Demonstration of Core Objectives within the Course: Assigned Core Learning Outcome Instructional strategy or content Method by which students’ Objective Students will be able to: used to achieve the outcome mastery of this outcome will be evaluated Critical Thinking Utilize scientific Star Property Correlations – They will be instructed to processes to identify students will form and test prioritize these properties in Empirical & questions pertaining to hypotheses to explain the terms of their relevance in Quantitative natural phenomena. correlation between a number of deciding between competing Reasoning properties seen in stars.
    [Show full text]
  • Galactic Astronomy with AO: Nearby Star Clusters and Moving Groups
    Galactic astronomy with AO: Nearby star clusters and moving groups T. J. Davidgea aDominion Astrophysical Observatory, Victoria, BC Canada ABSTRACT Observations of Galactic star clusters and objects in nearby moving groups recorded with Adaptive Optics (AO) systems on Gemini South are discussed. These include observations of open and globular clusters with the GeMS system, and high Strehl L observations of the moving group member Sirius obtained with NICI. The latter data 2 fail to reveal a brown dwarf companion with a mass ≥ 0.02M in an 18 × 18 arcsec area around Sirius A. Potential future directions for AO studies of nearby star clusters and groups with systems on large telescopes are also presented. Keywords: Adaptive optics, Open clusters: individual (Haffner 16, NGC 3105), Globular Clusters: individual (NGC 1851), stars: individual (Sirius) 1. STAR CLUSTERS AND THE GALAXY Deep surveys of star-forming regions have revealed that stars do not form in isolation, but instead form in clusters or loose groups (e.g. Ref. 25). This is a somewhat surprising result given that most stars in the Galaxy and nearby galaxies are not seen to be in obvious clusters (e.g. Ref. 31). This apparent contradiction can be reconciled if clusters tend to be short-lived. In fact, the pace of cluster destruction has been measured to be roughly an order of magnitude per decade in age (Ref. 17), indicating that the vast majority of clusters have lifespans that are only a modest fraction of the dynamical crossing-time of the Galactic disk. Clusters likely disperse in response to sudden changes in mass driven by supernovae and stellar winds (e.g.
    [Show full text]
  • Dwarfs Walking in a Row the filamentary Nature of the NGC 3109 Association
    A&A 559, L11 (2013) Astronomy DOI: 10.1051/0004-6361/201322744 & c ESO 2013 Astrophysics Letter to the Editor Dwarfs walking in a row The filamentary nature of the NGC 3109 association M. Bellazzini1, T. Oosterloo2;3, F. Fraternali4;3, and G. Beccari5 1 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: [email protected] 2 Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands 3 Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands 4 Dipartimento di Fisica e Astronomia - Università degli Studi di Bologna, viale Berti Pichat 6/2, 40127 Bologna, Italy 5 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei Munchen, Germany Received 24 September 2013 / Accepted 22 October 2013 ABSTRACT We re-consider the association of dwarf galaxies around NGC 3109, whose known members were NGC 3109, Antlia, Sextans A, and Sextans B, based on a new updated list of nearby galaxies and the most recent data. We find that the original members of the NGC 3109 association, together with the recently discovered and adjacent dwarf irregular Leo P, form a very tight and elongated configuration in space. All these galaxies lie within ∼100 kpc of a line that is '1070 kpc long, from one extreme (NGC 3109) to the other (Leo P), and they show a gradient in the Local Group standard of rest velocity with a total amplitude of 43 km s−1 Mpc−1, and a rms scatter of just 16.8 km s−1. It is shown that the reported configuration is exceptional given the known dwarf galaxies in the Local Group and its surroundings.
    [Show full text]
  • Galaxies: Outstanding Problems and Instrumental Prospects for the Coming Decade (A Review)* T (Cosmology/History of Astronomy/Quasars/Space) JEREMIAH P
    Proc. Natl. Acad. Sci. USA Vol. 74, No. 5, pp. 1767-1774, May 1977 Astronomy Galaxies: Outstanding problems and instrumental prospects for the coming decade (A Review)* t (cosmology/history of astronomy/quasars/space) JEREMIAH P. OSTRIKER Princeton University Observatory, Peyton Hall, Princeton, New Jersey 08540 Contributed by Jeremiah P. Ostriker, February 3, 1977 ABSTRACT After a review of the discovery of external It is more than a little astonishing that in the early part of this galaxies and the early classification of these enormous aggre- century it was the prevailing scientific view that man lived in gates of stars into visually recognizable types, a new classifi- a universe centered about himself; by 1920 the sun's newly cation scheme is suggested based on a measurable physical quantity, the luminosity of the spheroidal component. It is ar- discovered, slightly off-center position was still controversial. gued that the new one-parameter scheme may correlate well The discovery was, ironically, due to Shapley. both with existing descriptive labels and with underlying A little background to this debate may be useful. The Island physical reality. Universe hypothesis was not new, having been proposed 170 Two particular problems in extragalactic research are isolated years previously by the English astronomer, Thomas Wright as currently most fundamental. (i) A significant fraction of the (2), and developed with remarkably prescience by Emmanuel energy emitted by active galaxies (approximately 1% of all galaxies) is emitted by very small central regions largely in parts Kant, who wrote (see refs. 10 and 23 in ref. 3) in 1755 (in a of the spectrum (microwave, infrared, ultraviolet and x-ray translation from Edwin Hubble).
    [Show full text]
  • Observational Cosmology - 30H Course 218.163.109.230 Et Al
    Observational cosmology - 30h course 218.163.109.230 et al. (2004–2014) PDF generated using the open source mwlib toolkit. See http://code.pediapress.com/ for more information. PDF generated at: Thu, 31 Oct 2013 03:42:03 UTC Contents Articles Observational cosmology 1 Observations: expansion, nucleosynthesis, CMB 5 Redshift 5 Hubble's law 19 Metric expansion of space 29 Big Bang nucleosynthesis 41 Cosmic microwave background 47 Hot big bang model 58 Friedmann equations 58 Friedmann–Lemaître–Robertson–Walker metric 62 Distance measures (cosmology) 68 Observations: up to 10 Gpc/h 71 Observable universe 71 Structure formation 82 Galaxy formation and evolution 88 Quasar 93 Active galactic nucleus 99 Galaxy filament 106 Phenomenological model: LambdaCDM + MOND 111 Lambda-CDM model 111 Inflation (cosmology) 116 Modified Newtonian dynamics 129 Towards a physical model 137 Shape of the universe 137 Inhomogeneous cosmology 143 Back-reaction 144 References Article Sources and Contributors 145 Image Sources, Licenses and Contributors 148 Article Licenses License 150 Observational cosmology 1 Observational cosmology Observational cosmology is the study of the structure, the evolution and the origin of the universe through observation, using instruments such as telescopes and cosmic ray detectors. Early observations The science of physical cosmology as it is practiced today had its subject material defined in the years following the Shapley-Curtis debate when it was determined that the universe had a larger scale than the Milky Way galaxy. This was precipitated by observations that established the size and the dynamics of the cosmos that could be explained by Einstein's General Theory of Relativity.
    [Show full text]
  • Astronomy (ASTR) 1
    Astronomy (ASTR) 1 Astronomy (ASTR) ASTR 1000. Introduction to the Universe. 3 Hours. A survey of the universe, examining the historical origins of astronomy; the motions and physical properties of the Sun, Moon, and planets; the formation, evolution, and death of stars; and the structure of galaxies and the expansion of the Universe. ASTR 1010K. Astronomy of the Solar System. 4 Hours. Astronomy from early ideas of the cosmos to modern observational techniques. The solar system planets, satellites, and minor bodies. The origin and evolution of the solar system. Three lectures and one night laboratory session per week. ASTR 1020K. Stellar and Galactic Astronomy. 4 Hours. The study of the Sun and stars, their physical properties and evolution, interstellar matter, star clusters, our Galaxy and other galaxies, the origin and evolution of the Universe. Three lectures and one night laboratory session per week. ASTR 2010. Tools of Astronomy. 1 Hour. An introduction to observational techniques for the beginning astronomy major. Completion of this course will enable the student to use the campus observatory without direct supervision. The student will be given instruction in the use of the observatory and its associated equipment. Includes laboratory safety, research methods, exploration of resources (library and Internet), and an outline of the discipline. ASTR 2020. The Planetarium. 1 Hour. Prerequisites: ASTR 1000, ASTR 1010K, ASTR 1020K, or permission of instructor. Instruction in the operation of the campus planetarium and delivery of planetarium programs. Completion of this course will qualify the student to prepare and give planetarium programs to visiting groups. ASTR 2950. Directed Study.
    [Show full text]
  • AS203 – Introduction to Stellar and Galactic Astronomy
    AS 203 – Introduction to Stellar and Galactic Astronomy Syllabus – Spring 2008 Instructor Prof. Elizabeth Blanton Room: CAS 519 Email: [email protected] Phone: 617-353-2633 Office hours: M 12:00 – 1:30 pm, W 1:00 – 2:30 pm, or by appointment Teaching Assistant Teaching Assistant Day Labs Night Labs Nicholas Lee Michael Pavel Room: CAS 524 Room: CAS 524 Email: [email protected] Email: [email protected] Phone: 617-353-6554 Phone: 617-358-0566 Office hours: T 1:30 – 3:00 pm M, T 10:00 – 11:00 am Th 11:00 am – 12:30 pm W 4:00 – 5:00 pm Class Hours and Location Lectures (A1 and HP): MWF 11:00 am – 12:00 pm; CAS 502 Labs: You must sign up for one section; indoor labs are in CAS 521 A2 Mon. 5:00 – 6:30 pm A3 Tues. 5:00 – 6:30 pm A4 Wed. 5:00 – 6:30 pm Observing Labs: CAS rooftop telescopes Observing (night) labs will be held immediately after the indoor (day) labs. You should go to observing labs on the same day that you go to your indoor labs. There will be two periods for each observing lab, 6:30 – 7:30 pm and 7:30 – 8:30 pm. This is to avoid having too many people share the telescopes at the same time. Later in the semester, the 6:30 – 7:30 pm section will move to 8:30 – 9:30 pm, since the sun will be setting later. In case of poor weather, observing labs will not be held.
    [Show full text]
  • Quasars & Black Holes
    The Odd Couple: Quasars & Black Holes Scott Tremaine Abstract: Quasars emit more energy than any other object in the universe, yet are not much bigger than our solar system. Quasars are powered by giant black holes of up to ten billion (1010) times the mass of the sun. Their enormous luminosities are the result of frictional forces acting upon matter as it spirals toward the black hole, heating the gas until it glows. We also believe that black holes of one million to ten billion solar masses–dead quasars–are present at the centers of most galaxies, includ ing our own. The mass of the central black hole appears to be closely related to other properties of its host galaxy, such as the total mass in stars, but the origin of this relation and the role that black holes play in the formation of galaxies are still mysteries. Black holes are among the most alien predictions of Einstein’s general theory of relativity: regions of space-time in which gravity is so strong that nothing –not even light–can escape. More precisely, a black hole is a singularity in space-time surrounded by an SCOTT TREMAINE, a Foreign Hon - event horizon, a surface that acts as a perfect one-way orary Member of the American membrane: matter and radiation can enter the event Acad emy since 1992, is the Richard horizon, but, once inside, can never escape. Although Black Professor in the School of black holes are an inevitable consequence of Ein- Nat ural Sciences at the Institute for stein’s theory, their main properties were only under - Advanced Study and the Charles A.
    [Show full text]
  • Amy Reines Wandering Massive Black Holes in Dwarf Galaxies
    Wandering Massive Black Holes in Dwarf Galaxies Amy Reines Montana State University Image credit: NRAO/Sophia Dagnello (illustration) eXtreme Gravity Institute (XGI) Giant elliptical galaxy Messier 87 Normally, massive black holes are found in the centers of giant galaxies. We don’t know how these black holes form! 6.5 billion solar mass black hole (EHT Collaboration) How massive were the first black hole seeds? Giant galaxies with > billion solar-mass BHs growth via accretion and mergers Black hole mass Dwarf galaxies with < hundred thousand solar-mass BHs Galaxy mass Theory: Possible black hole seed formation mechanisms Remnants from first Direct collapse of dense gas generation of massive stars 5 6 • MBH ~100 Msun • MBH ~10 -10 Msun • abundant • rare for reviews, see e.g., Volonteri (2010); Natarajan (2014); Johnson & Haardt (2016); Latif & Ferrara (2016) Models of BH growth in a cosmological context predict that the observational signatures indicative of seed formation are strongest in dwarf galaxies predictions at z=0 Direct Stellar Direct collapse collapse remnants Stellar remnants BH occupation fraction MBH-host galaxy relations Volonteri et al. (2008); van Wassenhove et al. (2010); also see Ricarte & Natarajan (2018) Observations: The smallest BHs in dwarf galaxies place the most concrete limits on the masses of BH seeds. RGG 118: Dwarf galaxy with MBH ~50,000 Msun Baldassare, Reines, Gallo & Greene (2015, 2017) The focus of my research is to search for and study massive black holes in dwarf galaxies. This is currently our best observational probe of the origin of massive black holes. Optical Searches Radio Searches •Lots of progress in recent years •Potential for new discoveries For example: > 100 dwarfs with massive black holes (Reines et al.
    [Show full text]
  • A Sequoia in the Garden: a Dwarf Galaxy Or a Giant Globular Cluster Hidden in the Bulge?
    A sequoia in the garden: a dwarf galaxy or a giant globular cluster hidden in the bulge? Rodolfo H. Barbá Universidad de La Serena Chile Modern Cosmography: Playing the game of big panchromatic all-sky surveys Cosmography is the science that maps the general features of the cosmos or universe, describing both heaven and Earth. In Astrophysics, the term is beginning to be used to describe attempts to determine the large-scale matter distribution and kinematics of the observable universe (Wikipedia) In collaboration with: Dante Minniti (UNAB) Doug Geisler (ULS-UdeC) Javier Alonso-García (UA) Maren Hempel (UNAB) Antonela Monachesi (ULS) Julia Arias (ULS) Facundo Gómez (ULS) Motivation ● Large multi-frequency, synoptic, and all-sky surveys are opening new horizons in the heaven exploration. ● For Galactic Astronomy, relevant are: VVV, UKIDDS, Glimpse, WISE, DECaPS, SkyMapper, PANSTARRS, Herschel, etc. ● Gaia DR2 is opening a Pandora’s Box, and transforming our knowledge about the Milky Way structure. ● Tens of large scale new structures discovered. DECaPS ● Dark Energy Camera Galactic Plane Survey http://decaps.skymaps.info ● DECAM: 520 mpix, 4-m Blanco Telescope, CTIO (Chile) ● Southern GP, 1000 sq-deg (|b| < 4º). ● Very deep, limits g~23.7, r~22.8, i~22.2, z~21.8, and Y~21.0 ● Details in Schlafly et al. 2018. �������� ������������ /*" &!�J��� ��� ���������� � � ������������ /*" &!J1��$%�� ������ �!�"��������� � � /*" &!J-+!* � �� ����#�������������� � � /*" &!J-+!* ����� ���$$$�% ���& 01"�KF=G 9��:? �"-�A:> 01"�KFF? �"-�A:: � � VVV Window – Minniti et al 2018, A&A, 616, A26 ........., o.O 1 Q) '"d 0 L......J ..Q - 1 E(J -Ks ) 2 ........., o.O 1 Q) '"d 0 L......J ..Q - 1 - 2 35 0 345 34 0 335 33 0 325 1 [ deg] 3 1.44 0 2.5 1.20 ........., 2 0.96 o.O ---~ U) Q) U) '"d ::.::: L......J ~ 1.5 0.72 ~ '----" ..Q - 0.5 ~ 1 0.48 0.5 0.24 0 0.00 - 1 348.5 348 347 346.5 VVV Window – Minniti et al 2018, A&A, 616, A26 ------ .,,,,..
    [Show full text]
  • Szegedi Tudományegyetem Természettudományi És
    Szegedi Tudom´anyegyetem Term´eszettudom´anyi ´es Informatikai Kar K´ıs´erleti Fizika Tansz´ek A k¨oz´episkolai ,,k´ıs´erleti” fizika tank¨onyvsorozat elemz´ese csillag´asz szemmel An astronomers’ view on the secondary level ’experimental’ schoolbooks of physics Szakdolgozat k´esz´ıtette: Dr. Egedyn´eBakos Judit fizikatan´ar MSc levelez¨ohallgat´o t´emavezet¨o: Dr. Szatm´ary K´aroly egyetemi tan´ar 2017 Dorcinak. Tartalomjegyz´ek 1 Bevezet˝o 1 1.1 Aszakdolgozatmotiv´aci´oja . .... 1 1.2 Atank¨onyvcsal´adh´attere . .... 2 1.2.1 A k´ıs´erleti tank¨onyvek koncepci´oja . ....... 3 1.2.2 A k´ıs´erleti tank¨onyvek szerkezete . ...... 4 1.3 Aszakdolgozatc´elja . .. .. 4 2 A 9. oszt´alyos tank¨onyv csillag´aszati tartalmai 6 2.1 T´aj´ekoz´od´as ´egen-f¨old¨on . ......... 6 2.1.1 A t´er ´es az id˝otartom´anyai (Fizika 9/8.) . ....... 9 2.1.2 A t´avols´agok ´es az id˝om´er´ese . ..... 17 2.1.3 Helymeghat´aroz´as (Fizika 9/17.) . .... 18 2.2 Mozg´asokaNaprendszerben . .. 21 2.2.1 A Naprendszer modelljei (Fizika 9./78) . .... 21 2.2.2 Kepler t¨orv´enyek - Fizika 9./83. .... 28 2.2.3 A F¨old, a Hold ´es a Nap m´er´ese - Fizika 9./87. ...... 30 2.3 Altal´abanaFizika9.´ tank¨onyvr˝ol . .... 30 3 A 11. oszt´alyos tank¨onyv csillag´aszati tartalmai 32 3.1 A f´eny term´eszete. Hogyan l´atunk? . ...... 32 3.1.1 Hogyan m˝uk¨odik? A nagyat´ot´ol a t´avcs˝oig (Fizika11./23) .
    [Show full text]