Astronomy Terms for Stars
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Invited Talks and Lectures
Invited Talks and Lectures Fundamental Problems in Planetary Science and Astrobiology 13th IAU-Abdul Jabbar Astronomy Workshop Bangladesh University of Engineering and Technology Dhaka, Bangladesh (November 6, 2020) Terrestrial Planet Formation in Modern Era: Current State and Future Direction Pathways to Habitability Bad Hofgastein, Austria (January 12-18, 2020) Life Stories; A Career in Planetology Keynote Presentation at EPSC-DPS 2019 Geneva, Switzerland (September 15, 2019) Planets in Binary Stars Institute of Physical Sciences of the National Autonomous University of Mexico (ICF-UNAM) Cuernavaca, Mexico (February 20, 2019) New Advances in the Formation of Terrestrial Planets National Institute for Space Research San Jose Campos, Brazil (October 2, 2018) Four Lectures on Exoplanet Formation and Kepler Telescope’s Discoveries 3rd Astrobiology School at the National Observatory of Brazil Rio de Janeiro, Brazil (October 1 – 5, 2018) Planet Formation: The Gateway to Astrobiology Keynote talk at the 3rd AbGradE Symposium Berlin, Germany (September 22 – 24, 2018) From Dust to Planets Summer School on the Formation and Evolution of Stars and Planets, the Early Solar System, and the Emergence of Life Vienna, Austria (August 17 – 18, 2018) Modern Simulations of Terrestrial Planet Formation and the Origin of Earth’s Water Leibniz Institute for Astrophysics Potsdam, Germany (June 7, 2018) Modern Simulations of Terrestrial Planet Formation and the Origin of Earth’s Water University of Groningen Groningen, Netherlands (June 4, 2018) Modern Simulations -
Antony Hewish
PULSARS AND HIGH DENSITY PHYSICS Nobel Lecture, December 12, 1974 by A NTONY H E W I S H University of Cambridge, Cavendish Laboratory, Cambridge, England D ISCOVERY OF P U L S A R S The trail which ultimately led to the first pulsar began in 1948 when I joined Ryle’s small research team and became interested in the general problem of the propagation of radiation through irregular transparent media. We are all familiar with the twinkling of visible stars and my task was to understand why radio stars also twinkled. I was fortunate to have been taught by Ratcliffe, who first showed me the power of Fourier techniques in dealing with such diffraction phenomena. By a modest extension of existing theory I was able to show that our radio stars twinkled because of plasma clouds in the ionosphere at heights around 300 km, and I was also able to measure the speed of ionospheric winds in this region (1) . My fascination in using extra-terrestrial radio sources for studying the intervening plasma next brought me to the solar corona. From observations of the angular scattering of radiation passing through the corona, using simple radio interferometers, I was eventually able to trace the solar atmo- sphere out to one half the radius of the Earth’s orbit (2). In my notebook for 1954 there is a comment that, if radio sources were of small enough angular size, they would illuminate the solar atmosphere with sufficient coherence to produce interference patterns at the Earth which would be detectable as a very rapid fluctuation of intensity. -
Planetary Diagrams — Descriptions, Models, Theories: from Carolingian Deployments to Copernican Debates
Planetary Diagrams — Descriptions, Models, Theories: from Carolingian Deployments to Copernican Debates Bruce Eastwood and Gerd Graßhoff Contents 1 Introduction . 1 2 The Beginnings in Carolingian Europe . 1 2.1 Astronomy and Computus before 800 . 1 2.2 Schools and Texts . 3 2.3 Diagrams and the Study of Texts . 7 2.4 Dynamics of Diagrams: Calcidius and Pliny . 7 2.5 Dynamics of Diagrams: Martianus Capella . 21 3 Qualitative Theory in the High and Later Middle Ages . 29 3.1 Dynamics of Diagrams: Construction of a Planetary The- ory............................ 29 3.2 The Capellan Tradition through the Fifteenth Century . 32 4 Merging Two Traditions: The Sixteenth Century . 37 1 INTRODUCTION Through three distinct periods from ca. 800 to ca. 1600 we find that European as- tronomers were concerned with questions about the planets that involved the dis- cussion and invention of models without quantitative expression. This qualitative tradition was first developed in the ninth century in the course of studying ancient Latin texts on cosmology and astronomy. The diagrams, used to represent different phenomena and aspects of planetary motion, continued as long as they were found useful for teaching, for exposing questions, or for proposing theoretical positions. The history of this tradition of planetary diagrams indicates a constant concern for qualitative theory and the co-existence of both qualitative and quantitative plane- tary theory after the introduction of the Greco-Arabic mathematical tradition of planetary astronomy in twelfth-century Europe. In the sixteenth century the same qualitative tradition continued as a source for approaches to new phenomena and problems. 2 THE BEGINNINGS IN CAROLINGIAN EUROPE 2.1 ASTRONOMY AND COMPUTUS BEFORE 800 From the sixth century to the twelfth century in Western Europe there was no direct influence of Greek works in the exact sciences. -
Flares on Active M-Type Stars Observed with XMM-Newton and Chandra
Flares on active M-type stars observed with XMM-Newton and Chandra Urmila Mitra Kraev Mullard Space Science Laboratory Department of Space and Climate Physics University College London A thesis submitted to the University of London for the degree of Doctor of Philosophy I, Urmila Mitra Kraev, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. Abstract M-type red dwarfs are among the most active stars. Their light curves display random variability of rapid increase and gradual decrease in emission. It is believed that these large energy events, or flares, are the manifestation of the permanently reforming magnetic field of the stellar atmosphere. Stellar coronal flares are observed in the radio, optical, ultraviolet and X-rays. With the new generation of X-ray telescopes, XMM-Newton and Chandra , it has become possible to study these flares in much greater detail than ever before. This thesis focuses on three core issues about flares: (i) how their X-ray emission is correlated with the ultraviolet, (ii) using an oscillation to determine the loop length and the magnetic field strength of a particular flare, and (iii) investigating the change of density sensitive lines during flares using high-resolution X-ray spectra. (i) It is known that flare emission in different wavebands often correlate in time. However, here is the first time where data is presented which shows a correlation between emission from two different wavebands (soft X-rays and ultraviolet) over various sized flares and from five stars, which supports that the flare process is governed by common physical parameters scaling over a large range. -
Institute of Theoretical Astronomy, 10, Kutuzov Quay, St.Petersburg, 191187, Russia
The Library of the Institute of Theoretical Astronomy of the Russian Academy of Sciences (1924 -1994). History, Present State, Perspectives for the Future M.V.Lapteva Institute of Theoretical Astronomy, 10, Kutuzov Quay, St.Petersburg, 191187, Russia e-mail: [email protected] fax: (812) 272-79-68 The Library of the Institute of Theoretical Astronomy (formerly The Library of the Astronomical Institute of the People’s Commisariat of Edu- cation, USSR (1924 - 1938); the Library of the Astronomical Institute of the USSR Academy of Sciences (1939 - 1943 (Dec. 16))) was established by the decision of the first director and founder of the Institute, Boris Vasil’evich Numerov (1891 - 1941), an outstanding astronomer in the fields of celestial mechanics, astrometry and geodesy, a corresponding member of the USSR Academy of Sciences since 1929 and a very gifted person who perished a victim to a repressive stalinist regime in 1941. The basis of the Library holdings formed the collections of books and pe- riodicals belonging to the Computational and Astronomo-Geodetic Institutes which merged in 1923 to form the Astronomical Institute. From the time of its foundation (1924) to 1930 the library had no profes- sional librarian. Beginning with 1924 and to 1936 (the time of his arrest) the director of the Institute B.V.Numerov devoted much of his time and efforts to primary and then current acquisition of relevant publications. During his numerous scientific missions abroad (Germany, USA, the coun- tries of the South America, etc) along with equipment he purchased urgently needed foreign publications and laid the basis for exchange of publications with foreign astronomical institutions since from 1922 the Institute started publishing its own works: 1. -
Need and Possibilities of Astronomy Teaching in the Finnish Comprehensive School
UNIVERSITY OF HELSINKI REPORT SERIES IN PHYSICS HU•P•D124 Need and possibilities of astronomy teaching in the Finnish comprehensive school Irma Hannula DEPARTMENT OF PHYSICAL SCIENCES P.O. BOX FIN•00014 UNIVERSITY OF HELSINKI HELSINKI, FINLAND Academic Dissertation To be presented, with the permission of the Faculty of Science of the University of Helsinki, for public criticism in the Small Auditorium E204 of the Department of Physical Sciences, on July 29th, 2005, at 12 o’clock. Helsinki 2005 ISBN 952•10•2103•9 (printed version) ISSN 0356•0961 ISBN 952•10•2104•7 (pdf•version) http://ethesis.helsinki.fi/ Photo: Aurora Borealis /Irma Hannula Yliopistopaino Helsinki Daniel my dear first•born grandchild you are joy and blessing for my life! I. Hannula: Need and possibilities of astronomy teaching in the Finnish comprehensive school, University of Helsinki, 2005, vii, 250 p., University of Helsinki, Report Series in Physics, HU•P•D124, ISBN 952•10• 2103•9 (printed version), ISSN 0356•0961, ISBN 952•10•2104•7 (pdf•version), http://ethesis.helsinki.fi/. Classification (INSPEC): A0140D, A0140E, A0140G, A0140J, A0190 Keywords: astronomy teaching, worldview, attitude, conceptual and processual structure Abstract The purpose of this work is to create a research•based foundation for planning the structure, content and methods of astronomy teaching in the Finnish comprehensive school. At first, a critical analysis of the significance of astronomy teaching from the point of view of the educational aims was made, in order to verify the need of it and to find significance factors, which would offer a basis for defining principles of astronomy teaching. -
Uv Ceti Type Variable Stars Presented in the General Catalogue of Variable Stars
IX BULGARIAN-SERBIAN ASTRONOMICAL CONFERENCE: . ASTROINFORMATICS . Sofia, 2 – 4 July, 2014 UV CETI TYPE VARIABLE STARS PRESENTED IN THE GENERAL CATALOGUE OF VARIABLE STARS Katya Tsvetkova Institute of Mathematics and Informatics, Bulgarian Academy of Sciences Sofia, 2 – 4 July, 2014 IX BULGARIAN-SERBIAN ASTRONOMICAL CONFERENCE: . ASTROINFORMATICS . Abstract We present the place and the status of UV Ceti type variable stars in the General Catalogue of Variable Stars (GCVS4, edition April 2013) having in view the improved typological classification, which is accepted in the already prepared GCVS4.2 edition. The improved classification is based on understanding the major astrophysical reasons for variability. The distribution statistics is done on the basis of the data from the GCVS4 and addition of data from the 80th Name List of Variable Stars - altogether 47 967 variable stars with determined type of variability. The class of the eruptive variable stars includes variables showing irregular or semi-regular brightness variations as a consequence of violent processes and flares occurring in their chromospheres and coronae and accompanied by shell events or mass outflow as stellar winds and/or by interaction with the surrounding interstellar matter. In this class the type of the UV Ceti stars is referred together with the types of Irregular variables (Herbig Ae/Be stars; T Tau type stars (classical and weak- line ones), connected with diffuse nebulae, or RW Aurigae type stars without such connection; FU Orionis type; YY Orionis type; Yellow -
Arab Conference on Astronomy and Geophysics the 5Th Assembly (ACAG-5) By: Sultana N
Arab Conference on Astronomy and Geophysics the 5th Assembly (ACAG-5) By: Sultana N. Nahar, The Ohio State University The international Arab Conference on Astronomy and Geophysics (ACAG) has been held every two years since its initiation in 2008 by the Minister of Higher Education and Scientific Research of Egypt and the General Secretary of the League of Arab States. The objectives are to hold ACAG in all Arab states and strengthen the collaborations among the Arab countries. However, any non-Arabic country is welcome to join. I attended the 5th Assembly held at the National Research Institute of The author of this article, Sultana N. Astronomy and Geophysics (NRIAG) in Helwan, Egypt during Nahar, the first woman Guest of Honor at October 17 - 20, 2016. It was my honor to be invited as the first female ACAG-5. Guest of Honor at ACAG along with two Emirs from the United Arab Emirates. As told, I might be the first female guest of honor at any other Arab conferences. NRIAG in Egypt has been the main host for ACAGs, but the plan is now to move to other Arab countries. Egypt is the most attractive place for students and researchers of North African and Middle-Eastern countries for education and research. Founded in 1839 in Boulac, NRIAG (previously the Helwan observatory) is the oldest observatory in North Africa. It moved to Abbassia and then to Helwan in 1903 where it is currently located. It runs 11 labs all over Egypt with space and solar, seismology, geomagnetism, geoelectric, and geodynamics research labs. -
GEORGE HERBIG and Early Stellar Evolution
GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study. -
Evaluation Report for the Division of Theoretical Astronomy of NAOJ Piet
Evaluation Report for the Division of Theoretical Astronomy of NAOJ Piet Hut, Yipeng Jing, Doug Lin, Shin Mineshige, Masayuki Umemura February 2008 1. Summary We are impressed by the many accomplishments that have been made in the Theory and Computation Division of the National Astronomical Observatory of Japan (NAOJ) in the past four years. We agree with the self-evaluation report of the Division, which has high- lighted many important areas of research to which the Division has made major contri- butions. In particular, we agree with their analysis of their scienti¯c output: they have published a large number of papers with signi¯cant impact on the international community. If anything, the self-evaluation has been too modest. The Division of Theoretical Astronomy / Center for Computational Astrophysics (DTA/CfCA) is truly an international center of excellence in computational astrophysics, one of the most important centers of that type in the world. Much progress has been made on the development and application of numerical algorithms as well as actual hardware which enable large scale computation in areas ranging from solar system formation to the emergence of structure in the Universe. The 4D2U initiative has produced an e®ective package for public outreach as well as a valuable research tool. We strongly endorse future expansion of the theoretical e®ort especially in the development of innovative algorithms and state-of-the-art simulations. These simulations can provide predictions as well as interpretations of observations to be obtained from the various next- generation astronomical facilities. No matter how important direct observations and pure theoretical thought may be, their signi¯cance can only be understood through the bridge between the two that is provided by means of detailed simulations. -
Star Factories at the End of the World | Maxplanckresearch 1/2013
Star Factories at the End of the World When the universe came into being 13.7 billion years ago, there was initially only radiation. A few hundred million years later, however, the space was filled with galaxies – tremendously productive star factories that don’t fit quite so well with the image of a gradual cosmic evolution. Researchers like Fabian Walter from the Max Planck Institute for Astronomy in Heidelberg are attempting to illuminate a dark epoch of the universe. TEXT ALEXANDER STIRN FOCUS_Cosmology A deeper view into the cosmos: This section from the Hubble Ultra Deep Field shows the galaxies at the edge of space and time. Huge numbers of stars are born in these young Milky Ways. inding catchy designations But this is slowly changing: “Because It’s still detective work – a laborious for incomprehensible pro- our telescopes are continually improv- search that has practically nothing to cesses has never been a prob- ing and becoming more sensitive, we do with the colorful photos that astron- lem for astronomers: They see things today that we couldn’t have omy otherwise produces. Many of these call the era that begins just observed ten years ago,” says Fabian typical, vivid photographs are hanging F 380,000 years after the birth of the uni- Walter, an astronomer at the Max in the stairwell of the Heidelberg-based verse the Dark Ages. At that time, the Planck Institute for Astronomy in Hei- institute, a concrete structure located positively charged ions emerging from delberg. There, the 41-year-old investi- on the Königstuhl promontory high the Big Bang set about catching the free gates how and when the first stars above the city. -
The Kepler Catalog of Stellar Flares James R
Western Washington University Masthead Logo Western CEDAR Physics & Astronomy College of Science and Engineering 9-20-2016 The Kepler Catalog of Stellar Flares James R. A. Davenport Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/physicsastronomy_facpubs Part of the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation Davenport, James R. A., "The Kepler Catalog of Stellar Flares" (2016). Physics & Astronomy. 15. https://cedar.wwu.edu/physicsastronomy_facpubs/15 This Article is brought to you for free and open access by the College of Science and Engineering at Western CEDAR. It has been accepted for inclusion in Physics & Astronomy by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. The Astrophysical Journal, 829:23 (12pp), 2016 September 20 doi:10.3847/0004-637X/829/1/23 © 2016. The American Astronomical Society. All rights reserved. THE KEPLER CATALOG OF STELLAR FLARES James R. A. Davenport1 Department of Physics & Astronomy, Western Washington University, Bellingham, WA 98225, USA Received 2016 June 20; revised 2016 July 7; accepted 2016 July 12; published 2016 September 16 ABSTRACT A homogeneous search for stellar flares has been performed using every available Kepler light curve. An iterative light curve de-trending approach was used to filter out both astrophysical and systematic variability to detect flares. The flare recovery completeness has also been computed throughout each light curve using artificial flare injection tests, and the tools for this work have been made publicly available. The final sample contains 851,168 candidate flare events recovered above the 68% completeness threshold, which were detected from 4041 stars, or 1.9% of the stars in the Kepler database.