Multi-Color Photometry of the Hot R Coronae Borealis Star, MV Sagittarii
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High Precision Photometry of Transiting Exoplanets
McNair Scholars Research Journal Volume 3 Article 3 2016 High Precision Photometry of Transiting Exoplanets Maurice Wilson Embry-Riddle Aeronautical University and Harvard-Smithsonian Center for Astrophysics Jason Eastman Harvard-Smithsonian Center for Astrophysics John Johnson Harvard-Smithsonian Center for Astrophysics Follow this and additional works at: https://commons.erau.edu/mcnair Recommended Citation Wilson, Maurice; Eastman, Jason; and Johnson, John (2016) "High Precision Photometry of Transiting Exoplanets," McNair Scholars Research Journal: Vol. 3 , Article 3. Available at: https://commons.erau.edu/mcnair/vol3/iss1/3 This Article is brought to you for free and open access by the Journals at Scholarly Commons. It has been accepted for inclusion in McNair Scholars Research Journal by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. Wilson et al.: High Precision Photometry of Transiting Exoplanets High Precision Photometry of Transiting Exoplanets Maurice Wilson1,2, Jason Eastman2, and John Johnson2 1Embry-Riddle Aeronautical University 2Harvard-Smithsonian Center for Astrophysics In order to increase the rate of finding, confirming, and characterizing Earth-like exoplanets, the MINiature Exoplanet Radial Velocity Array (MINERVA) was recently built with the purpose of obtaining the spectroscopic and photometric precision necessary for these tasks. Achieving the satisfactory photometric precision is the primary focus of this work. This is done with the four telescopes of MINERVA and the defocusing technique. The satisfactory photometric precision derives from the defocusing technique. The use of MINERVA’s four telescopes benefits the relative photometry that must be conducted. Typically, it is difficult to find satisfactory comparison stars within a telescope’s field of view when the primary target is very bright. -
The AAVSO DSLR Observing Manual
The AAVSO DSLR Observing Manual AAVSO 49 Bay State Road Cambridge, MA 02138 email: [email protected] Version 1.2 Copyright 2014 AAVSO Foreword This manual is a basic introduction and guide to using a DSLR camera to make variable star observations. The target audience is first-time beginner to intermediate level DSLR observers, although many advanced observers may find the content contained herein useful. The AAVSO DSLR Observing Manual was inspired by the great interest in DSLR photometry witnessed during the AAVSO’s Citizen Sky program. Consumer-grade imaging devices are rapidly evolving, so we have elected to write this manual to be as general as possible and move the software and camera-specific topics to the AAVSO DSLR forums. If you find an area where this document could use improvement, please let us know. Please send any feedback or suggestions to [email protected]. Most of the content for these chapters was written during the third Citizen Sky workshop during March 22-24, 2013 at the AAVSO. The persons responsible for creation of most of the content in the chapters are: Chapter 1 (Introduction): Colin Littlefield, Paul Norris, Richard (Doc) Kinne, Matthew Templeton Chapter 2 (Equipment overview): Roger Pieri, Rebecca Jackson, Michael Brewster, Matthew Templeton Chapter 3 (Software overview): Mark Blackford, Heinz-Bernd Eggenstein, Martin Connors, Ian Doktor Chapters 4 & 5 (Image acquisition and processing): Robert Buchheim, Donald Collins, Tim Hager, Bob Manske, Matthew Templeton Chapter 6 (Transformation): Brian Kloppenborg, Arne Henden Chapter 7 (Observing program): Des Loughney, Mike Simonsen, Todd Brown Various figures: Paul Valleli Clear skies, and Good Observing! Arne Henden, Director Rebecca Turner, Operations Director Brian Kloppenborg, Editor Matthew Templeton, Science Director Elizabeth Waagen, Senior Technical Assistant American Association of Variable Star Observers Cambridge, Massachusetts June 2014 i Index 1. -
Practical Observational Astronomy Photometry
Practical Observational Astronomy Lecture 5 Photometry Wojtek Pych Warszawa, October 2019 History ● Hipparchos 190 – 120 B.C. visible stars divided into 6 magnitudes ● John Hershel 1792- 1871 → Norman Robert Pogson A.D. 1829 - 1891 I m I 1 =100 m1−m2=−2.5 log( ) I m+5 I 2 Visual Observations ●Argelander method ●Cuneiform photometer ●Polarimetric photometer Visual Observations Copyright AAVSO The American Association of Variable Star Observers Photographic Plates Blink comparator Scanning Micro-Photodensitometer Photographic plates Liller, Martha H.; 1978IBVS.1527....1L Photoelectric Photometer ● Photomultiplier tubes – Single star measurement – Individual photons Photoelectric Photometer ● 1953 - Harold Lester Johnson - UBV system – telescope with aluminium covered mirrors, – detector is photomultiplier 1P21, – for V Corning 3384 filter is used, – for B Corning 5030 + Schott CG13 filters are used, – for U Corning 9863 filter is used. – Telescope at altitude of >2000 meters to allow the detection of sufficent amount of UV light. UBV System Extensions: R,I ● William Wilson Morgan ● Kron-Cousins CCD Types of photometry ● Aperture ● Profile ● Image subtraction Aperture Photometry Aperture Photometry Profile Photometry Profile Photometry DAOphot ● Find stars ● Aperture photometry ● Point Spread Function ● Profile photometry Image Subtraction Image Subtraction ● Construct a template image – Select a number of best quality images – Register all images into a selected astrometric position ● Find common stars ● Calculate astrometric transformation -
“Astrometry/Photometry of Solar System Objects After Gaia”
ISSN 1621-3823 ISBN 2-910015-77-7 NOTES SCIENTIFIQUES ET TECHNIQUES DE L’INSTITUT DE MÉCANIQUE CÉLESTE S106 Proceedings of the Workshop and colloquium held at the CIAS (Meudon) on October 14-18, 2015 “Astrometry/photometry of Solar System objects after Gaia” Institut de mécanique céleste et de calcul des éphémérides CNRS UMR 8028 / Observatoire de Paris 77, avenue Denfert-Rochereau 75014 Paris Mars 2017 Dépôt légal : Mars 2017 ISBN 2-910015-77-7 Foreword The modeling of the dynamics of the solar system needs astrometric observations made on a large interval of time to validate the scenarios of evolution of the system and to be able to provide ephemerides extrapolable in the next future. That is why observations are made regularly for most of the objects of the solar system. The arrival of the Gaia reference star catalogue will allow us to make astrometric reductions of observations with an increased accuracy thanks to new positions of stars and a more accurate proper motion. The challenge consists in increasing the astrometric accuracy of the reduction process. More, we should think about our campaigns of observations: due to this increased accuracy, for which objects, ground based observations will be necessary, completing space probes data? Which telescopes and targets for next astrometric observations? The workshop held in Meudon tried to answer these questions. Plans for the future have been exposed, results on former campaigns such as Phemu15 campaign, have been provided and amateur astronomers have been asked for continuing their participation to new observing campaigns of selected objects taking into account the new possibilities offered by the Gaia reference star catalogue. -
Variable Star Section Circular No
The British Astronomical Association Variable Star Section Circular No. 176 June 2018 Office: Burlington House, Piccadilly, London W1J 0DU Contents Joint BAA-AAVSO meeting 3 From the Director 4 V392 Per (Nova Per 2018) - Gary Poyner & Robin Leadbeater 7 High-Cadence measurements of the symbiotic star V648 Car using a CMOS camera - Steve Fleming, Terry Moon and David Hoxley 9 Analysis of two semi-regular variables in Draco – Shaun Albrighton 13 V720 Cas and its close companions – David Boyd 16 Introduction to AstroImageJ photometry software – Richard Lee 20 Project Melvyn, May 2018 update – Alex Pratt 25 Eclipsing Binary news – Des Loughney 27 Summer Eclipsing Binaries – Christopher Lloyd 29 68u Herculis – David Conner 36 The BAAVSS Eclipsing Binary Programme lists – Christopher Lloyd 39 Section Publications 42 Contributing to the VSSC 42 Section Officers 43 Cover image V392 Per (Nova Per 2018) May 6.129UT iTelescope T11 120s. Martin Mobberley 2 Back to contents Joint BAA/AAVSO Meeting on Variable Stars Warwick University Saturday 7th & Sunday 8th July 2018 Following the last very successful joint meeting between the BAAVSS and the AAVSO at Cambridge in 2008, we are holding another joint meeting at Warwick University in the UK on 7-8 July 2018. This two-day meeting will include talks by Prof Giovanna Tinetti (University College London) Chemical composition of planets in our Galaxy Prof Boris Gaensicke (University of Warwick) Gaia: Transforming Stellar Astronomy Prof Tom Marsh (University of Warwick) AR Scorpii: a remarkable highly variable -
Highlights of Discoveries for $\Delta $ Scuti Variable Stars from the Kepler
Highlights of Discoveries for δ Scuti Variable Stars from the Kepler Era Joyce Ann Guzik1,∗ 1Los Alamos National Laboratory, Los Alamos, NM 87545 USA Correspondence*: Joyce Ann Guzik [email protected] ABSTRACT The NASA Kepler and follow-on K2 mission (2009-2018) left a legacy of data and discoveries, finding thousands of exoplanets, and also obtaining high-precision long time-series data for hundreds of thousands of stars, including many types of pulsating variables. Here we highlight a few of the ongoing discoveries from Kepler data on δ Scuti pulsating variables, which are core hydrogen-burning stars of about twice the mass of the Sun. We discuss many unsolved problems surrounding the properties of the variability in these stars, and the progress enabled by Kepler data in using pulsations to infer their interior structure, a field of research known as asteroseismology. Keywords: Stars: δ Scuti, Stars: γ Doradus, NASA Kepler Mission, asteroseismology, stellar pulsation 1 INTRODUCTION The long time-series, high-cadence, high-precision photometric observations of the NASA Kepler (2009- 2013) [Borucki et al., 2010; Gilliland et al., 2010; Koch et al., 2010] and follow-on K2 (2014-2018) [Howell et al., 2014] missions have revolutionized the study of stellar variability. The amount and quality of data provided by Kepler is nearly overwhelming, and will motivate follow-on observations and generate new discoveries for decades to come. Here we review some highlights of discoveries for δ Scuti (abbreviated as δ Sct) variable stars from the Kepler mission. The δ Sct variables are pre-main-sequence, main-sequence (core hydrogen-burning), or post-main-sequence (undergoing core contraction after core hydrogen burning, and beginning shell hydrogen burning) stars with spectral types A through mid-F, and masses around 2 solar masses. -
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 -
The Search for Transiting Extrasolar Planets in the Open Cluster M52
THE SEARCH FOR TRANSITING EXTRASOLAR PLANETS IN THE OPEN CLUSTER M52 A Thesis Presented to the Faculty of San Diego State University In Partial Fulfillment of the Requirements for the Degree Master of Sciences in Astronomy by Tiffany M. Borders Summer 2008 SAN DIEGO STATE UNIVERSITY The Undersigned Faculty Committee Approves the Thesis of Tiffany M. Borders: The Search for Transiting Extrasolar Planets in the Open Cluster M52 Eric L. Sandquist, Chair Department of Astronomy William Welsh Department of Astronomy Calvin Johnson Department of Physics Approval Date iii Copyright 2008 by Tiffany M. Borders iv DEDICATION To all who seek new worlds. v Success is to be measured not so much by the position that one has reached in life as by the obstacles which he has overcome. –Booker T. Washington All the world’s a stage, And all the men and women merely players. They have their exits and their entrances; And one man in his time plays many parts... –William Shakespeare, “As You Like It”, Act 2 Scene 7 vi ABSTRACT OF THE THESIS The Search for Transiting Extrasolar Planets in the Open Cluster M52 by Tiffany M. Borders Master of Sciences in Astronomy San Diego State University, 2008 In this survey we attempt to discover short-period Jupiter-size planets in the young open cluster M52. Ten nights of R-band photometry were used to search for planetary transits. We obtained light curves of 4,128 stars and inspected them for variability. No planetary transits were apparent; however, some interesting variable stars were discovered. In total, 22 variable stars were discovered of which, 19 were not previously known as variable. -
METEOR CSILLAGÁSZATI ÉVKÖNYV 2019 Meteor Csillagászati Évkönyv 2019
METEOR CSILLAGÁSZATI ÉVKÖNYV 2019 meteor csillagászati évkönyv 2019 Szerkesztette: Benkő József Mizser Attila Magyar Csillagászati Egyesület www.mcse.hu Budapest, 2018 Az évkönyv kalendárium részének összeállításában közreműködött: Tartalom Bagó Balázs Görgei Zoltán Kaposvári Zoltán Kiss Áron Keve Kovács József Bevezető ....................................................................................................... 7 Molnár Péter Sánta Gábor Kalendárium .............................................................................................. 13 Sárneczky Krisztián Szabadi Péter Cikkek Szabó Sándor Szőllősi Attila Zsoldos Endre: 100 éves a Nemzetközi Csillagászati Unió ........................191 Zsoldos Endre Maria Lugaro – Kereszturi Ákos: Elemkeletkezés a csillagokban.............. 203 Szabó Róbert: Az OGLE égboltfelmérés 25 éve ........................................218 A kalendárium csillagtérképei az Ursa Minor szoftverrel készültek. www.ursaminor.hu Beszámolók Mizser Attila: A Magyar Csillagászati Egyesület Szakmailag ellenőrizte: 2017. évi tevékenysége .........................................................................242 Szabados László Kiss László – Szabó Róbert: Az MTA CSFK Csillagászati Intézetének 2017. évi tevékenysége .........................................................................248 Petrovay Kristóf: Az ELTE Csillagászati Tanszékének működése 2017-ben ............................................................................ 262 Szabó M. Gyula: Az ELTE Gothard Asztrofi zikai Obszervatórium -
SATELLITE COMMUNICATION UNIT I OVERVIEW of SATELLITE SYSTEMS, ORBITS and LAUNCHING METHODS Introduction
www.jntuhweb.com JNTUH WEB SATELLITE COMMUNICATION UNIT I OVERVIEW OF SATELLITE SYSTEMS, ORBITS AND LAUNCHING METHODS Introduction – Frequency allocations for satellite services – Intelsat – U.S domsats – Polar orbiting satellites – Problems – Kepler’s first law – Kepler’s second law – Kepler’s third law – Definitions of terms for earth – Orbiting satellites – Orbital elements – Apogee and perigee heights – Orbital perturbations – Effects of a non-spherical earth – Atmospheric drag – Inclined orbits – Calendars – Universal time – Julian dates – Sidereal time – The orbital plane – The geocentric – Equatorial coordinate system – Earth station referred to the IJK frame – The topcentric – Horizon co-ordinate system – The subsatellite point – Predicting satellite position. PART A 1. What is Satellite? Mention the types. An artificial body that is projected from earth to orbit either earth (or) another body of solar systems. Types: Information satellites and Communication Satellites 2. State Kepler’s first law. It states that the path followed by the satellite around the primary will be an ellipse. An ellipse has two focal points F1 and F2. The center of mass of the two body system, termed the barycenter is always centered on one of the foci. e = [square root of ( a2– b2) ] / a 3. State Kepler’s second law. It states that for equal time intervals, the satellite will sweep out equal areas in its orbital Skyupsmediaplane, focused at the barycenter. 4. State Kepler’s third law. It states that the square of the periodic time of orbit is perpendicular to the cube of the mean distance between the two bodies. JNTUH WEB www.jntuhweb.com JNTUH WEB a3= 3 / n2 Where, n = Mean motion of the satellite in rad/sec. -
From Dinuclear Systems to Close Binary Stars: Application to Source
From Dinuclear Systems to Close Binary Stars: Application to Source of Energy in the Universe V.V. Sargsyan1,2, H. Lenske2, G.G. Adamian1, and N.V. Antonenko1 1Joint Institute for Nuclear Research, 141980 Dubna, Russia, 2Institut f¨ur Theoretische Physik der Justus–Liebig–Universit¨at, D–35392 Giessen, Germany (Dated: January 1, 2019) Abstract The evolution of close binary stars in mass asymmetry (transfer) coordinate is considered. The conditions for the formation of stable symmetric binary stars are analyzed. The role of symmetriza- tion of asymmetric binary star in the transformation of potential energy into internal energy of star and the release of a large amount of energy is revealed. PACS numbers: 26.90.+n, 95.30.-k Keywords: close binary stars, mass transfer, mass asymmetry arXiv:1812.11338v1 [astro-ph.SR] 29 Dec 2018 1 I. INTRODUCTION Because mass transfer is an important observable for close binary systems in which the two stars are nearly in contact [1–8], it is meaningful and necessary to study the evolution of these stellar systems in the mass asymmetry coordinate η = (M1 − M2)/(M1 + M2) where Mi, (i = 1, 2), are the stellar masses. In our previous work [9], we used classical Newtonian mechanics and study the evolution of the close binary stars in their center-of- mass frame by analyzing the total potential energy U(η) as a function of η at fixed total mass M = M1 + M2 and orbital angular momentum L = Li of the system. The limits for the formation and evolution of the di-star systems were derived and analyzed. -
Stsci Newsletter: 2011 Volume 028 Issue 02
National Aeronautics and Space Administration Interacting Galaxies UGC 1810 and UGC 1813 Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) 2011 VOL 28 ISSUE 02 NEWSLETTER Space Telescope Science Institute We received a total of 1,007 proposals, after accounting for duplications Hubble Cycle 19 and withdrawals. Review process Proposal Selection Members of the international astronomical community review Hubble propos- als. Grouped in panels organized by science category, each panel has one or more “mirror” panels to enable transfer of proposals in order to avoid conflicts. In Cycle 19, the panels were divided into the categories of Planets, Stars, Stellar Rachel Somerville, [email protected], Claus Leitherer, [email protected], & Brett Populations and Interstellar Medium (ISM), Galaxies, Active Galactic Nuclei and Blacker, [email protected] the Inter-Galactic Medium (AGN/IGM), and Cosmology, for a total of 14 panels. One of these panels reviewed Regular Guest Observer, Archival, Theory, and Chronology SNAP proposals. The panel chairs also serve as members of the Time Allocation Committee hen the Cycle 19 Call for Proposals was released in December 2010, (TAC), which reviews Large and Archival Legacy proposals. In addition, there Hubble had already seen a full cycle of operation with the newly are three at-large TAC members, whose broad expertise allows them to review installed and repaired instruments calibrated and characterized. W proposals as needed, and to advise panels if the panelists feel they do not have The Advanced Camera for Surveys (ACS), Cosmic Origins Spectrograph (COS), the expertise to review a certain proposal. Fine Guidance Sensor (FGS), Space Telescope Imaging Spectrograph (STIS), and The process of selecting the panelists begins with the selection of the TAC Chair, Wide Field Camera 3 (WFC3) were all close to nominal operation and were avail- about six months prior to the proposal deadline.