CONTENTS IAU Information Bulletin N° 109
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Evans.2013.HD189733.Albedo.Pdf
ORE Open Research Exeter TITLE The Deep Blue Color of HD 189733b: Albedo Measurements with Hubble Space Telescope/Space Telescope Imaging Spectrograph at Visible Wavelengths AUTHORS Evans, T.M.; Pont, F.; Sing, David K.; et al. JOURNAL Astrophysical Journal DEPOSITED IN ORE 15 December 2014 This version available at http://hdl.handle.net/10871/16042 COPYRIGHT AND REUSE Open Research Exeter makes this work available in accordance with publisher policies. A NOTE ON VERSIONS The version presented here may differ from the published version. If citing, you are advised to consult the published version for pagination, volume/issue and date of publication The Astrophysical Journal Letters, 772:L16 (5pp), 2013 August 1 doi:10.1088/2041-8205/772/2/L16 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE DEEP BLUE COLOR OF HD 189733b: ALBEDO MEASUREMENTS WITH HUBBLE SPACE TELESCOPE/SPACE TELESCOPE IMAGING SPECTROGRAPH AT VISIBLE WAVELENGTHS Thomas M. Evans1,Fred´ eric´ Pont2,DavidK.Sing2, Suzanne Aigrain1, Joanna K. Barstow1, Jean-Michel Desert´ 3,7, Neale Gibson4, Kevin Heng5, Heather A. Knutson3, and Alain Lecavelier des Etangs6 1 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK; [email protected] 2 School of Physics, University of Exeter, EX4 4QL Exeter, UK 3 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 4 European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany 5 University of Bern, Center for Space and Habitability, Sidlerstrasse 5, CH-3012 Bern, Switzerland 6 Institut d’Astrophysique de Paris, UMR7095 CNRS, Universite Pierre et Marie Curie, 98 bis Boulevard Arago, F-75014 Paris, France Received 2013 May 31; accepted 2013 June 15; published 2013 July 11 ABSTRACT We present a secondary eclipse observation for the hot Jupiter HD 189733b across the wavelength range 290–570 nm made using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. -
Curriculum Vitae Name
CURRICULUM VITAE NAME PRIYA (SHAH) HASAN DATE OF BIRTH 13 June 1972 ADDRESS Flat No 101, Desire©s Panorama MLA Colony , Road No 12 Banjara Hills Hyderabad 500 034 Email: [email protected] Ph:9701811881, 9866619519 (Mob) (040)23306959(Res) MARITAL STATUS Married COMPUTER SKILLS Operating Systems: UNIX, LINUX, Windows Word Processing: Latex Image Processing Software: IRAF , IDL Languages: FORTRAN, C, Python. LANGUAGES English, Hindi, Russian , Urdu EDUCATIONAL QUALIFICATIONS BOARD YEAR OF PASSING %/GRADE NAME OF INSTITUTE ICSE 1987 86.67% Jamnabai Narsee School, Juhu, Mumbai HSc 1989 78% D G Ruparel College, Matunga, Mumbai MSc Physics 1996 Grade 4 Physics Department, (Integrated) (scale of 5) Moscow State University, Spl:Astrophysics Moscow, Russia PhD 2004 Department of Astronomy, Osmania University, Hyderabad 500 007 SCHOLARSHIPS/GRANTS/AWARDS The IndoSoviet Cultural Society (ISCUS) scholar (19901996) for MSc (Integrated) to the Moscow State University, Russia IndoFrench Centre for the Promotion of Advanced Research(IFPCAR) (2004 2006) Post Doctoral Fellowship at IUCAA, Pune Department of Science and Technology (DST) Women Scientist Scheme (2006 2009) DST project under the Women Scientist Scheme (SR/WOSA/PS- 26/2005) entitled ªPhotometric studies of star clusters using the 2MASS and observationsº. International Visitor Leadership Program (IVLP ) Invited under the International Visitor Leadership Program (IVLP) by the US Consulate, Hyderabad to visit and interact with American Universities and Research Centres for a period of three weeks in August 2011. TRAVEL GRANT: Department of Science and Technology (DST), International Travel Support (ITS) to present a paper at the conference "From Stars to Galaxies", 2010, at the University of Florida, Gainesville. -
The Solar System and Its Place in the Galaxy in Encyclopedia of the Solar System by Paul R
Giant Molecular Clouds http://www.astro.ncu.edu.tw/irlab/projects/project.htm Æ Galactic Open Clusters Æ Galactic Structure Æ GMCs The Solar System and its Place in the Galaxy In Encyclopedia of the Solar System By Paul R. Weissman http://www.academicpress.com/refer/solar/Contents/chap1.htm Stars in the galactic disk have different characteristic velocities as a function of their stellar classification, and hence age. Low-mass, older stars, like the Sun, have relatively high random velocities and as a result c an move farther out of the galactic plane. Younger, more massive stars have lower mean velocities and thus smaller scale heights above and below the plane. Giant molecular clouds, the birthplace of stars, also have low mean velocities and thus are confined to regions relatively close to the galactic plane. The disk rotates clockwise as viewed from "galactic north," at a relatively constant velocity of 160-220 km/sec. This motion is distinctly non-Keplerian, the result of the very nonspherical mass distribution. The rotation velocity for a circular galactic orbit in the galactic plane defines the Local Standard of Rest (LSR). The LSR is then used as the reference frame for describing local stellar dynamics. The Sun and the solar system are located approxi-mately 8.5 kpc from the galactic center, and 10-20 pc above the central plane of the galactic disk. The circular orbit velocity at the Sun's distance from the galactic center is 220 km/sec, and the Sun and the solar system are moving at approximately 17 to 22 km/sec relative to the LSR. -
Star Clusters
Star Clusters • Eventually, photons and stellar winds clear out the remaining gas and dust and leave behind the stars. • Reflection nebulae provide evidence for remaining dust on the far side of the Pleiades Star Clusters • It may be that all stars are born in clusters. • A good question is therefore why are most stars we see in the Galaxy not members of obvious clusters? • The answer is that the majority of newly-formed clusters are very weakly gravitationally bound. Perturbations from passing molecular clouds, spiral arms or mass loss from the cluster stars `unbind’ most clusters. Star Cluster Ages • We can use the H-R Diagram of the stars in a cluster to determine the age of the cluster. • A cluster starts off with stars along the full main sequence. • Because stars with larger mass evolve more quickly, the hot, luminous end of the main sequence becomes depleted with time. • The `main-sequence turnoff’ moves to progressively lower mass, L and T with time. • Young clusters contain short-lived, massive stars in their main sequence • Other clusters are missing the high-mass MSTO stars and we can infer the cluster age is the main-sequence lifetime of the highest mass star still on the main- sequence. 25Mo 3million years 104 3Mo 500Myrs 102 1M 10Gyr L o 1 0.5Mo 200Gyr 10-2 30000 15000 7500 3750 Temperature Star Clusters Sidetrip • There are two basic types of clusters in the Galaxy. • Globular Clusters are mostly in the halo of the Galaxy, contain >100,000 stars and are very ancient. • Open clusters are in the disk, contain between several and a few thousand stars and range in age from 0 to 10Gyr Galaxy Ages • Deriving galaxy ages is much harder because most galaxies have a star formation history rather than a single-age population of stars. -
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 Wonders of Star Formafion
The Wonders of Star Forma;on A tribute to Hans Zinnecker Edinburgh, Scotland 3-7 September, 2018 i John McIntyre Conference Centre Edinburgh UK 3rd - 7th September 2018 SOC Anthony Whitworth (Cardiff, UK, Co-Chair) Ken Rice (Edinburgh, UK, Co-Chair) Bo Reipurth (Hawaii, USA) Cathie Clarke (Cambridge, UK) Ian Bonnell (St Andrews, UK) Mark McCaughrean (ESA) Stephanie Walch (Cologne, Germany) Hal Yorke (USRA, USA) John Bally (Colorado, USA) Dimitris Stamatellos (UCLAN, UK) LOC Lyndsey Ballantyne Ken Rice ii Contents General Information 1 Information for Speakers . .1 Information for Posters . .1 WiFi Access . .1 Social Media . .1 Open forum: The Challenges Ahead . .2 Timetable . .3 Floorplan . .4 Getting Around Edinburgh . .5 Dining Options . .6 Excursions . .7 Useful Information . .7 Code of Conduct . .8 Talk Abstracts 9 Poster List & Abstracts 87 iii iv General Information Information for Speakers You are welcome to use your own laptops, but we will also be providing a Mac with OS X and a Windows machine for speakers to use. We can accomodate PDF, Keynote and Powerpoint. Please ensure you have uploaded and tested your talk on the computers prior to your session beginning, or have tested your own laptop/device. All contributed talks are 15 minutes plus 5 minutes for questions, while invited review talks are 30 minutes plus 10 minutes for questions. Session chairs will give appropriate warnings when you are approaching your time limit. To ensure the smooth running of each session, please keep to time. Thank you! Information for Posters Posters are allocated a numbered board based on the session to which they've been allocated. -
Book of Abstracts
UDC 520/524(048) ISBN 978-86-80019-55-0 VIII SERBIAN-BULGARIAN ASTRONOMICAL CONFERENCE Leskovac, Serbia, May 8-12, 2012 BOOK OF ABSTRACTS Eds. Milan S. Dimitrijević and Milcho K. Tsvetkov BELGRADE 2012 SCIENTIFIC COMMITTEE LOCAL ORGANIZING COMMITTEE Milan S. Dimitrijević (Co-chairman) Milan S. Dimitrijević (Co-chairman) Milcho K. Tsvetkov (Co-chairman) Žarko Mijajlović (Co-chairman) Žarko Mijajlović (Co-vice chairman) Ognyan Kounchev (Co-vice Chairman) Scientific secretary: Tanyu Bonev Andjelka Kovačević Dimo Dimov Dragana Ilić Members: Darko Jevremović Luka Č. Popović Predrag Jovanović Darko Jevremović Andjelka Kovačević Nadežda Pejović Jelena Kovačević Petko Nedialkov Jelena Kovačević Marko Stalevski Nadežda Pejović Luka Č. Popović Tanja Milovanov Miodrag Dačić Zoran Simić Katya Tsvetkova Zoran Simić Dejan Urošević Under the auspices of Serbian Ministry of Education and Science Bulgarian Academy of Sciences ORGANIZERS: Society of Astronomers of Serbia and Astronomical Observatory Institute of Astronomy with National Astronomical Observarory, BAS Co-organizers: Faculty of Mathematics and Department of Astronomy, University of Belgrade Institute of Mathematics and Informatics of the Bulgarian Academy of Sciences Department of Astronomy, Faculty of Physics, Sofia University ''St. Kliment Ohridski' On the front cover: Panorama of the town of Leskovac On the back cover: A forest on a secret planet, author Vladimir M. Dimitrijević Text arrangement by computer: Tatjana Milovanov Published and copyright © by Serbian Astronomical Society and Astronomical Observatory, Belgrade, Volgina 7, 11060 Belgrade, Serbia Financially supported by the Ministry of Education and Science of Serbia __________________________________________________________________ Production: “BS PRINT”, Jurija Gagarina 29v, Novi Beograd, in 100 copies UDC 520/524(048) ISBN 978-86-80019-55-0 VIII SERBIAN-BULGARIAN ASTRONOMICAL CONFERENCE Leskovac, Serbia, May 8-12, 2012 BOOK OF ABSTRACTS Eds. -
Khag L October 2015
No. 104 KHAG L OCTOBER 2015 Editor : Editorial Assistant : Somak Raychaudhury Manjiri Mahabal ([email protected]) ([email protected]) A quarterly bulletin of the Inter-University Centre for Astronomy and Astrophysics ISSN 0972-7647 (An autonomous institution of the University Grants Commission) Available online at http://ojs.iucaa.ernet.in/ AT THE HELM... Professor Somak Raychaudhury has taken over as the Director, IUCAA, with effect from September 1, 2015 on my superannuation. He had his undergraduate education at Presidency College, Kolkata and the University of Oxford. For his Ph.D. he worked with Professor Donald Lynden- Bell at the Institute of Astronomy, University of Cambridge, UK, followed by post- doctoral fellowships at the Harvard- Smithsonian Center for Astrophysics, Cambridge, Harvard University, USA, and at the Institute of Astronomy. He was a faculty member at IUCAA during 1995 - 2000, and then at the University of Birmingham. In 2012, he joined the Presidency University, Kolkata, where he Somak Raychaudhury (Left) and Ajit Kembhavi was the Head of the Department of Physics and Dean, Natural Sciences. and will be greatly concerned Contents... with the University Programmes Reports of Past Events 1,2,3,4,5,6 Professor Raychaudhury’s research interests of IUCAA. Announcements 7 are in the areas of Galaxy Groups, Galaxy Welcome and Farewell 8 The IUCAA family looks forward Clusters and Large Scale Structures, and New Associates 9 carries out Observational work in the to his leadership in taking IUCAA Seminars 10 Optical, Radio and X-ray domains. Professor further along the path of progress. Visitors 10,11 Raychaudhury is deeply involved in Congratulations 11 Know Thy Birds 12 teaching of Astronomy and Public Outreach, Ajit Kembhavi KHAG L | IJmoc | No. -
Stellar Dynamics and Stellar Phenomena Near a Massive Black Hole
Stellar Dynamics and Stellar Phenomena Near A Massive Black Hole Tal Alexander Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 234 Herzl St, Rehovot, Israel 76100; email: [email protected] | Author's original version. To appear in Annual Review of Astronomy and Astrophysics. See final published version in ARA&A website: www.annualreviews.org/doi/10.1146/annurev-astro-091916-055306 Annu. Rev. Astron. Astrophys. 2017. Keywords 55:1{41 massive black holes, stellar kinematics, stellar dynamics, Galactic This article's doi: Center 10.1146/((please add article doi)) Copyright c 2017 by Annual Reviews. Abstract All rights reserved Most galactic nuclei harbor a massive black hole (MBH), whose birth and evolution are closely linked to those of its host galaxy. The unique conditions near the MBH: high velocity and density in the steep po- tential of a massive singular relativistic object, lead to unusual modes of stellar birth, evolution, dynamics and death. A complex network of dynamical mechanisms, operating on multiple timescales, deflect stars arXiv:1701.04762v1 [astro-ph.GA] 17 Jan 2017 to orbits that intercept the MBH. Such close encounters lead to ener- getic interactions with observable signatures and consequences for the evolution of the MBH and its stellar environment. Galactic nuclei are astrophysical laboratories that test and challenge our understanding of MBH formation, strong gravity, stellar dynamics, and stellar physics. I review from a theoretical perspective the wide range of stellar phe- nomena that occur near MBHs, focusing on the role of stellar dynamics near an isolated MBH in a relaxed stellar cusp. -
PHY206 Exploring the Universe Course Schedule
PHY206 Exploring the Universe Course Schedule The course will cover the following topics. The test dates are set in stone while the course content may shift around them. Motion of the Night Sky and Solar System Cycles Unit 1 Our Planetary Neighborhood Unit 2 Beyond the Solar System Unit 3 Astronomical Numbers Unit 4 Foundations of Astronomy Unit 5 The Night Sky Unit 6 The Year Unit 7 The Time of Day Unit 8 Lunar Cycles Unit 9 Calendars Unit 10 Geometry of the Earth, Moon, and Sun Unit 11 Planets: The Wandering Stars Unit 12 The Beginnings of Modern Astronomy Unit 13 Observing the Sky Thursday 2/17 Test 1 Gravity & Orbits, Light & Telescopes Unit 14 Astronomical Motion: Inertia, Mass, and Force Unit 15 Force, Acceleration, and Interaction Unit 16 The Universal Law of Gravity Unit 17 Measuring a Body’s Mass Using Orbital Motion Unit 18 Orbital and Escape Velocities Unit 19 Tides Unit 21 Light, Matter, and Energy Unit 22 The Electromagnetic Spectrum Unit 23 Thermal Radiation Unit 24 Atomic Spectra: Identifying Atoms by Their Light Unit 25 The Doppler Shift Unit 26 Detecting Light Unit 27 Collecting Light Unit 28 Focusing Light Unit 29 Telescope Resolution Unit 30 The Earth’s Atmosphere and Space Observatories Unit 31 Amateur Astronomy Monday 3/14 Test 2 The Solar System: Sun, Earth, Moon Unit 32 The Structure of the Solar System Unit 33 The Origin of the Solar System Unit 49 The Sun, Our Star Unit 50 The Sun’s Source of Power Unit 51 Solar Activity Unit 35 The Earth as a Terrestrial Planet Unit 36 Earth's Atmosphere and Hydrosphere Unit 37 Our Moon Monday 4/11 Test 3 The Solar System: Planets Unit 38 Mercury Unit 39 Venus Unit 40 Mars Unit 41 Asteroids Unit 42 Comparative Planetology Unit 43 Jupiter and Saturn Unit 44 Uranus and Neptune Unit 45 Satellite Systems and Rings Unit 46 Ice Worlds, Pluto, and Beyond Unit 47 Comets Unit 48 Impacts on Earth Monday 5/2 Test 4 Other Planetary Systems Unit 34 Other Planetary Systems Unit 83 Astrobiology Unit 84 The Search for Life Elsewhere Review Day (Monday 5/9) Thursday 5/19 10:15am 12:15pm Final Exam . -
A Needs Analysis Study of Amateur Astronomers for the National Virtual Observatory : Aaron Price1 Lou Cohen1 Janet Mattei1 Nahide Craig2
A Needs Analysis Study of Amateur Astronomers For the National Virtual Observatory : Aaron Price1 Lou Cohen1 Janet Mattei1 Nahide Craig2 1Clinton B. Ford Astronomical Data & Research Center American Association of Variable Star Observers 25 Birch St, Cambridge MA 02138 2Space Sciences Laboratory University of California, Berkeley 7 Gauss Way Berkeley, CA 94720-7450 Abstract Through a combination of qualitative and quantitative processes, a survey was con- ducted of the amateur astronomy community to identify outstanding needs which the National Virtual Observatory (NVO) could fulfill. This is the final report of that project, which was conducted by The American Association of Variable Star Observers (AAVSO) on behalf of the SEGway Project at the Center for Science Educations @ Space Sci- ences Laboratory, UC Berkeley. Background The American Association of Variable Star Observers (AAVSO) has worked on behalf of the SEGway Project at the Center for Science Educations @ Space Sciences Labo- ratory, UC Berkeley, to conduct a needs analysis study of the amateur astronomy com- munity. The goal of the study is to identify outstanding needs in the amateur community which the National Virtual Observatory (NVO) project can fulfill. The AAVSO is a non-profit, independent organization dedicated to the study of vari- able stars. It was founded in 1911 and currently has a database of over 11 million vari- able star observations, the vast majority of which were made by amateur astronomers. The AAVSO has a rich history and extensive experience working with amateur astrono- mers and specifically in fostering amateur-professional collaboration. AAVSO Director Dr. Janet Mattei headed the team assembled by the AAVSO. -
Year XIX, Supplement Ethnographic Study And/Or a Theoretical Survey of a Their Position in the Article Should Be Clearly Indicated
III. TITLES OF ARTICLES DRU[TVO ANTROPOLOGOV SLOVENIJE The journal of the Slovene Anthropological Society Titles (in English and Slovene) must be short, informa- SLOVENE ANTHROPOLOGICAL SOCIETY Anthropological Notebooks welcomes the submis- tive, and understandable. The title should be followed sion of papers from the field of anthropology and by the name of the author(s), their position, institutional related disciplines. Submissions are considered for affiliation, and if possible, by e-mail address. publication on the understanding that the paper is not currently under consideration for publication IV. ABSTRACT AND KEYWORDS elsewhere. It is the responsibility of the author to The abstract must give concise information about the obtain permission for using any previously published objective, the method used, the results obtained, and material. Please submit your manuscript as an e-mail the conclusions. Authors are asked to enclose in English attachment on [email protected] and enclose your contact information: name, position, and Slovene an abstract of 100 – 200 words followed institutional affiliation, address, phone number, and by three to five keywords. They must reflect the field of e-mail address. research covered in the article. English abstract should be placed at the beginning of an article and the Slovene one after the references at the end. V. NOTES A N T H R O P O L O G I C A L INSTRUCTIONS Notes should also be double-spaced and used sparingly. They must be numbered consecutively throughout the text and assembled at the end of the article just before references. VI. QUOTATIONS Short quotations (less than 30 words) should be placed in single quotation marks with double marks for quotations within quotations.