Celebrating the Centennial of a Celestial Yardstick
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Sky Notes - April 2012
North Devon Astronomical Society www.northdevonastronomy.co.uk Sky Notes - April 2012 THE MOON New Moon 21s t April First Quarter 29th April Full Moon 6th April Last Quarter 13th April THE PLANETS Mercury A morning object, Mercury is visible before sunrise by the middle of the month. The planet will reach greatest western elongation on the 18th, when it will be around 27 degrees from the Sun. Venus Now moving closer to the Sun once again following greatest elongation last month, but blazing away at magnitude -4.4, Venus still dominates the western evening sky. In the eyepiece, the planet presents a 25 arcsecond disc which is just under half illuminated. Mars Following last month’s opposition, The Red Planet remains fairly close to the bright star Regulus, in the constellation Leo. Though the apparent diameter of the planet will shrink slightly throughout the month, Mars remains worthy of observation and is visible for most of the night. Jupiter Though still visible low in the west after sunset, Jupiter will soon become lost in the evening twilight. Saturn R eaching opposition on the 15th, Saturn is observable all night in the constellation Virgo, close to the first magnitude star Spica, (Alpha Virginis). A magnificent object, Saturn’s rings and it’s largest satellite Titan are readily apparent in small telescopes, while larger instruments will show atmospheric bands and some of the smaller moons. Uranus Ur anus is too close to the Sun to be observable this month. Neptune A morning object, Neptune can be found among the stars of the constellation Aquarius. -
Resolved Astrometric Binary Stars Brian D. Mason
Resolved Astrometric Binary Stars Brian D. Mason 9/12/2012 U.S. Naval Observatory 1 Background Astrometric contributions of Friedrich Bessel (1784-1846) •Parallax of 61 Cygni (1838) U.S. Naval Observatory Background Astrometric contributions of Friedrich Bessel (1784-1846) •Parallax of 61 Cygni (1838) •Non-linear proper motion of Sirius and Procyon (1844) Image: http://vega.lpl.arizona.edu/sirius/A5.html U.S. Naval Observatory Background Astrometric contributions of Friedrich Bessel (1784-1846) •Parallax of 61 Cygni (1838) •Non-linear proper motion of Sirius and Procyon (1844) Due to stellar types (main- sequence and white dwarf) motion affect significant, but Image: http://vega.lpl.arizona.edu/sirius/A5.html companion hard to detect. • Sirius B first resolved in 1862 by Alvan Graham Clark (right) testing 18.5 ” Clark refractor. U.S. Naval Observatory Background Astrometric contributions of Friedrich Bessel (1784-1846) •Parallax of 61 Cygni (1838) •Non-linear proper motion of Sirius and Procyon (1844) Due to stellar types (main- sequence and white dwarf) motion affect significant, but companion hard to detect. • Sirius B first resolved in 1862 by Alvan Graham Clark (right) testing 18.5 ” Clark refractor. • Procyon B first resolved in 1896 by John Martin Schaeberle with Lick 36 ” Clark refractor. U.S. Naval Observatory CurrentCurrent Orbit: Orbit: Procyon Sirius AB AB • Broken line is line of nodes. • Green plus signs and asterisks: micrometry. • Pink asterisks: photography • Blue circles: HST/WFPC2 • Scales on axis are in arcseconds. • Direction of orbital motion at lower right. • Sirius Period = 50.090y. • Procyon Period = 40.82y. U.S. Naval Observatory Orbits • The 6 th Catalog of Orbits of Visual Binary Stars has 2298 orbits of 2187 systems. -
Essays-Mechanics / Electrodynamics/Download/8831
WHAT IF THE GALILEO AFFAIR NEVER HAPPENED? ABSTRACT From the 5th Century A.D. to the advent of Scholastic Aristotelianism, the curriculum in Roman Catholic universities in Europe taught a Rotating Geocentric Earth. St. Thomas Aquinas (1225 A.D.-1274 A.D.) introduced the writings of Aristotle (384 B.C.-322 B.C.) and of Claudius Ptolemy (100 A.D.-170 A.D.) in the 13th Century A.D., and the curriculum changed to teach a Non-Rotating Geocentric Earth. In this GSJ presentation, an Alternate History is presented. The famous Trial of Galileo never happened and the book by Nicolaus Copernicus was never banned by the Vatican of the Roman Catholic Church. The Roman Catholic Church simply ignored Galileo & his insulting book of 1632 A.D. The Roman Catholic Church Astronomers produced the Gregorian Calendar in 1583 A.D. The Roman Catholic Astronomers had abandoned the Aristotle/Ptolemy Model of Astronomy and had replaced it with the Non-Rotating Tychonian Model. This is NOT Alternate History. Johann Kepler published. That is NOT Alternate History. Isaac Newton published Principia, too. Christian Huygens contributed to the technology of the Mechanical Clock. Mechanical Time and Sundial Time demonstrate two similar but not identical paths. This is NOT Alternate History, either. The writer that is known as Voltaire (1694-1778) campaigned for Newton’s Principia as did Willem Gravesande (1688-1742). Pierre-Simon LaPlace (1748-1827) rescued Newton’s Celestial Mechanics of Universal Gravitation and Kepler’s Elliptical Orbits from disequilibrium issues in 1804A.D. Friedrich Bessel (1784-1846) discovered the first star to exhibit Stellar Parallax in 1838. -
Binocular Universe: Sly Fox September 2010 Phil Harrington
Binocular Universe is available every month on Cloudynights.com Binocular Universe: Sly Fox September 2010 Phil Harrington ast month's Stellafane convention, held atop Breezy Hill outside of Springfield, Vermont, was the best in recent memory. The skies were the Lclearest we've had in years, giving us a chance to enjoy the beauty of the summer Milky Way, which stretched from horizon to horizon. Armed with my trusty 10x50 and 16x70 binoculars, I sat back in my reclining chair and swept the plane of our Galaxy in pursuit of some old friends and new conquests. Above: Summer star map from Star Watch by Phil Harrington Binocular Universe is available every month on Cloudynights.com Above: Finder chart for this month's Binocular Universe. Chart adapted from Touring the Universe through Binoculars Atlas (TUBA), www.philharrington.net/tuba.htm Binocular Universe is available every month on Cloudynights.com Here are a few gems I bumped into along the way as I viewed the tiny constellation of Vulpecula the Fox. Vulpecula is a faint summertime constellation wedged between Cygnus (the Swan) to the north and Sagitta (the Arrow) to the south. None of Vulpecula’s stars shine brighter than magnitude 4.5, so seeing a fox here is a tall order indeed. But the sly Fox holds many binocular treasures for those who the time to seek them out. Vulpecula was created in 1687 by the Polish astronomer Johannes Hevelius. His original drawing showed a small fox carrying a hapless goose in its mouth. He called the combination Vulpecula et Anser ("the little fox and the goose"). -
A Hot Subdwarf-White Dwarf Super-Chandrasekhar Candidate
A hot subdwarf–white dwarf super-Chandrasekhar candidate supernova Ia progenitor Ingrid Pelisoli1,2*, P. Neunteufel3, S. Geier1, T. Kupfer4,5, U. Heber6, A. Irrgang6, D. Schneider6, A. Bastian1, J. van Roestel7, V. Schaffenroth1, and B. N. Barlow8 1Institut fur¨ Physik und Astronomie, Universitat¨ Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam-Golm, Germany 2Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 3Max Planck Institut fur¨ Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching bei Munchen¨ 4Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA 5Texas Tech University, Department of Physics & Astronomy, Box 41051, 79409, Lubbock, TX, USA 6Dr. Karl Remeis-Observatory & ECAP, Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg (FAU), Sternwartstr. 7, 96049 Bamberg, Germany 7Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 8Department of Physics and Astronomy, High Point University, High Point, NC 27268, USA *[email protected] ABSTRACT Supernova Ia are bright explosive events that can be used to estimate cosmological distances, allowing us to study the expansion of the Universe. They are understood to result from a thermonuclear detonation in a white dwarf that formed from the exhausted core of a star more massive than the Sun. However, the possible progenitor channels leading to an explosion are a long-standing debate, limiting the precision and accuracy of supernova Ia as distance indicators. Here we present HD 265435, a binary system with an orbital period of less than a hundred minutes, consisting of a white dwarf and a hot subdwarf — a stripped core-helium burning star. -
Plotting Variable Stars on the H-R Diagram Activity
Pulsating Variable Stars and the Hertzsprung-Russell Diagram The Hertzsprung-Russell (H-R) Diagram: The H-R diagram is an important astronomical tool for understanding how stars evolve over time. Stellar evolution can not be studied by observing individual stars as most changes occur over millions and billions of years. Astrophysicists observe numerous stars at various stages in their evolutionary history to determine their changing properties and probable evolutionary tracks across the H-R diagram. The H-R diagram is a scatter graph of stars. When the absolute magnitude (MV) – intrinsic brightness – of stars is plotted against their surface temperature (stellar classification) the stars are not randomly distributed on the graph but are mostly restricted to a few well-defined regions. The stars within the same regions share a common set of characteristics. As the physical characteristics of a star change over its evolutionary history, its position on the H-R diagram The H-R Diagram changes also – so the H-R diagram can also be thought of as a graphical plot of stellar evolution. From the location of a star on the diagram, its luminosity, spectral type, color, temperature, mass, age, chemical composition and evolutionary history are known. Most stars are classified by surface temperature (spectral type) from hottest to coolest as follows: O B A F G K M. These categories are further subdivided into subclasses from hottest (0) to coolest (9). The hottest B stars are B0 and the coolest are B9, followed by spectral type A0. Each major spectral classification is characterized by its own unique spectra. -
The Impact of the Astro2010 Recommendations on Variable Star Science
The Impact of the Astro2010 Recommendations on Variable Star Science Corresponding Authors Lucianne M. Walkowicz Department of Astronomy, University of California Berkeley [email protected] phone: (510) 642–6931 Andrew C. Becker Department of Astronomy, University of Washington [email protected] phone: (206) 685–0542 Authors Scott F. Anderson, Department of Astronomy, University of Washington Joshua S. Bloom, Department of Astronomy, University of California Berkeley Leonid Georgiev, Universidad Autonoma de Mexico Josh Grindlay, Harvard–Smithsonian Center for Astrophysics Steve Howell, National Optical Astronomy Observatory Knox Long, Space Telescope Science Institute Anjum Mukadam, Department of Astronomy, University of Washington Andrej Prsa,ˇ Villanova University Joshua Pepper, Villanova University Arne Rau, California Institute of Technology Branimir Sesar, Department of Astronomy, University of Washington Nicole Silvestri, Department of Astronomy, University of Washington Nathan Smith, Department of Astronomy, University of California Berkeley Keivan Stassun, Vanderbilt University Paula Szkody, Department of Astronomy, University of Washington Science Frontier Panels: Stars and Stellar Evolution (SSE) February 16, 2009 Abstract The next decade of survey astronomy has the potential to transform our knowledge of variable stars. Stellar variability underpins our knowledge of the cosmological distance ladder, and provides direct tests of stellar formation and evolution theory. Variable stars can also be used to probe the fundamental physics of gravity and degenerate material in ways that are otherwise impossible in the laboratory. The computational and engineering advances of the past decade have made large–scale, time–domain surveys an immediate reality. Some surveys proposed for the next decade promise to gather more data than in the prior cumulative history of astronomy. -
Distances and Magnitudes Distance Measurements the Cosmic Distance
Distances and Magnitudes Prof Andy Lawrence Astronomy 1G 2011-12 Distance Measurements Astronomy 1G 2011-12 The cosmic distance ladder • Distance measurements in astronomy are a chain, with each type of measurement relative to the one before • The bottom rung is the Astronomical Unit (AU), the (mean) distance between the Earth and the Sun • Many distance estimates rely on the idea of a "standard candle" or "standard yardstick" Astronomy 1G 2011-12 Distances in the solar system • relative distances to planets given by periods + Keplers law (see Lecture-2) • distance to Venus measured by radar • Sun-Earth = 1 A.U. (average) • Sun-Jupiter = 5 A.U. (average) • Sun-Neptune = 30 A.U. (average) • Sun- Oort cloud (comets) ~ 50,000 A.U. • 1 A.U. = 1.496 x 1011 m Astronomy 1G 2011-12 Distances to nearest stars • parallax against more distant non- moving stars • 1 parsec (pc) is defined as distance where parallax = 1 second of arc in standard units D = a/✓ (radians, metres) in AU and arcsec D(AU) = 1/✓rad = 206, 265/✓00 in parsec and arcsec D(pc) = 1/✓00 nearest star Proxima Centauri 1.30pc Very hard to measure less than 0.1" 1pc = 206,265 AU = 3.086 x 1016m so only good for stars a few parsecs away... until launch of GAIA mission in 2014..... Astronomy 1G 2011-12 More distant stars : standard candle technique If a star has luminosity L (total energy emitted per sec) then at L distance D we will observe flux density F (i.e. energy per second F = 2 per sq.m. -
The Extragalactic Distance Scale
The Extragalactic Distance Scale Published in "Stellar astrophysics for the local group" : VIII Canary Islands Winter School of Astrophysics. Edited by A. Aparicio, A. Herrero, and F. Sanchez. Cambridge ; New York : Cambridge University Press, 1998 Calibration of the Extragalactic Distance Scale By BARRY F. MADORE1, WENDY L. FREEDMAN2 1NASA/IPAC Extragalactic Database, Infrared Processing & Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA 2Observatories, Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena CA 91101, USA The calibration and use of Cepheids as primary distance indicators is reviewed in the context of the extragalactic distance scale. Comparison is made with the independently calibrated Population II distance scale and found to be consistent at the 10% level. The combined use of ground-based facilities and the Hubble Space Telescope now allow for the application of the Cepheid Period-Luminosity relation out to distances in excess of 20 Mpc. Calibration of secondary distance indicators and the direct determination of distances to galaxies in the field as well as in the Virgo and Fornax clusters allows for multiple paths to the determination of the absolute rate of the expansion of the Universe parameterized by the Hubble constant. At this point in the reduction and analysis of Key Project galaxies H0 = 72km/ sec/Mpc ± 2 (random) ± 12 [systematic]. Table of Contents INTRODUCTION TO THE LECTURES CEPHEIDS BRIEF SUMMARY OF THE OBSERVED PROPERTIES OF CEPHEID -
Not Surprising That the Method Begins to Break Down at This Point
152 ASTRONOMY: W. S. ADAMS hanced lines in the early F stars are normally so prominent that it is not surprising that the method begins to break down at this point. To illustrate the use of the formulae and curves we may select as il- lustrations a few stars of different spectral types and magnitudes. These are collected in Table II. The classification is from Mount Wilson determinations. TABLE H ~A M PARAIuAX srTATYP_________________ (a) I(b) (C) (a) (b) c) Mean Comp. Ob. Pi 10U96.... 7.6F5 -0.7 +0.7 +3.0 +6.5 4.7 5.8 5.7 +0#04 +0.04 Sun........ GO -0.5 +0.5 +3.0 +5.6 4.3 5.8 5.2 Lal. 38287.. 7.2 G5 -1.8 +1.5 +3.5 +7.4 +6.3 +6.2 7.3 +0.10 +0.09 a Arietis... 2.2K0O +2.5 -2.4 +0.2 +1.0 1.3 +0.2 0.8 +0.05 +0.09 aTauri.... 1.1K5 +3.0 -2.0 +0.5 -0.4 +1.9 +0.5 0.7 +0.08 +0.07 61' Cygni...6.3K8 -1.8 +5.8 +7.7 +8.2 9.3 8.9 8.8 +0.32 +0.31 Groom. 34..8.2 Ma -2.2 +6.8 +9.2 +10.2 10.5 10.4 10.4 +0.28 +0.28 The parallaxes are computed from the absolute magnitudes by the formula, to which reference has already been made, 5 logr = M - m - 5. The results are given in the next to the last column of the table, and the measured parallaxes in the final column. -
The Kinematic Signature of the Galactic Warp in Gaia DR1-I. the Hipparcos Subsample
Astronomy & Astrophysics manuscript no. WarpGaia c ESO 2021 September 26, 2021 The kinematic signature of the Galactic warp in Gaia DR1 I. The Hipparcos sub-sample E. Poggio1; 2, R. Drimmel2, R. L. Smart2; 3, A. Spagna2, and M. G. Lattanzi2 1 Università di Torino, Dipartimento di Fisica, via P. Giuria 1, 10125 Torino, Italy 2 Osservatorio Astrofisico di Torino, Istituto Nazionale di Astrofisica (INAF), Strada Osservatorio 20, 10025 Pino Torinese, Italy 3 School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK ABSTRACT Context. The mechanism responsible for the warp of our Galaxy, as well as its dynamical nature, continues to remain unknown. With the advent of high precision astrometry, new horizons have been opened for detecting the kinematics associated with the warp and constraining possible warp formation scenarios for the Milky Way. Aims. The aim of this contribution is to establish whether the first Gaia data release (DR1) shows significant evidence of the kinematic signature expected from a long-lived Galactic warp in the kinematics of distant OB stars. As the first paper in a series, we present our approach for analyzing the proper motions and apply it to the sub-sample of Hipparcos stars. Methods. We select a sample of 989 distant spectroscopically-identified OB stars from the New Reduction of Hipparcos (van Leeuwen 2008), of which 758 are also in the first Gaia data release (DR1), covering distances from 0.5 to 3 kpc from the Sun. We develop a model of the spatial distribution and kinematics of the OB stars from which we produce the probability distribution functions of the proper motions, with and without the systematic motions expected from a long-lived warp. -
Binocular Double Star Logbook
Astronomical League Binocular Double Star Club Logbook 1 Table of Contents Alpha Cassiopeiae 3 14 Canis Minoris Sh 251 (Oph) Psi 1 Piscium* F Hydrae Psi 1 & 2 Draconis* 37 Ceti Iota Cancri* 10 Σ2273 (Dra) Phi Cassiopeiae 27 Hydrae 40 & 41 Draconis* 93 (Rho) & 94 Piscium Tau 1 Hydrae 67 Ophiuchi 17 Chi Ceti 35 & 36 (Zeta) Leonis 39 Draconis 56 Andromedae 4 42 Leonis Minoris Epsilon 1 & 2 Lyrae* (U) 14 Arietis Σ1474 (Hya) Zeta 1 & 2 Lyrae* 59 Andromedae Alpha Ursae Majoris 11 Beta Lyrae* 15 Trianguli Delta Leonis Delta 1 & 2 Lyrae 33 Arietis 83 Leonis Theta Serpentis* 18 19 Tauri Tau Leonis 15 Aquilae 21 & 22 Tauri 5 93 Leonis OΣΣ178 (Aql) Eta Tauri 65 Ursae Majoris 28 Aquilae Phi Tauri 67 Ursae Majoris 12 6 (Alpha) & 8 Vul 62 Tauri 12 Comae Berenices Beta Cygni* Kappa 1 & 2 Tauri 17 Comae Berenices Epsilon Sagittae 19 Theta 1 & 2 Tauri 5 (Kappa) & 6 Draconis 54 Sagittarii 57 Persei 6 32 Camelopardalis* 16 Cygni 88 Tauri Σ1740 (Vir) 57 Aquilae Sigma 1 & 2 Tauri 79 (Zeta) & 80 Ursae Maj* 13 15 Sagittae Tau Tauri 70 Virginis Theta Sagittae 62 Eridani Iota Bootis* O1 (30 & 31) Cyg* 20 Beta Camelopardalis Σ1850 (Boo) 29 Cygni 11 & 12 Camelopardalis 7 Alpha Librae* Alpha 1 & 2 Capricorni* Delta Orionis* Delta Bootis* Beta 1 & 2 Capricorni* 42 & 45 Orionis Mu 1 & 2 Bootis* 14 75 Draconis Theta 2 Orionis* Omega 1 & 2 Scorpii Rho Capricorni Gamma Leporis* Kappa Herculis Omicron Capricorni 21 35 Camelopardalis ?? Nu Scorpii S 752 (Delphinus) 5 Lyncis 8 Nu 1 & 2 Coronae Borealis 48 Cygni Nu Geminorum Rho Ophiuchi 61 Cygni* 20 Geminorum 16 & 17 Draconis* 15 5 (Gamma) & 6 Equulei Zeta Geminorum 36 & 37 Herculis 79 Cygni h 3945 (CMa) Mu 1 & 2 Scorpii Mu Cygni 22 19 Lyncis* Zeta 1 & 2 Scorpii Epsilon Pegasi* Eta Canis Majoris 9 Σ133 (Her) Pi 1 & 2 Pegasi Δ 47 (CMa) 36 Ophiuchi* 33 Pegasi 64 & 65 Geminorum Nu 1 & 2 Draconis* 16 35 Pegasi Knt 4 (Pup) 53 Ophiuchi Delta Cephei* (U) The 28 stars with asterisks are also required for the regular AL Double Star Club.