DOCSLIB.ORG

Applications of Signal Processing in Astrophysics and Cosmology

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Applications of Signal Processing in Astrophysics and Cosmology EURASIP Journal on Applied Signal Processing Applications of Signal Processing in Astrophysics and Cosmology Guest Editors: Ercan E. Kuruoglu and Carlo Baccigalupi EURASIP Journal on Applied Signal Processing Applications of Signal Processing in Astrophysics and Cosmology EURASIP Journal on Applied Signal Processing Applications of Signal Processing in Astrophysics and Cosmology Guest Editors: Ercan E. Kuruoglu and Carlo Baccigalupi Copyright © 2005 Hindawi Publishing Corporation. All rights reserved. This is a special issue published in volume 2005 of “EURASIP Journal on Applied Signal Processing.” All articles are open access articles distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Editor-in-Chief Marc Moonen, Belgium Senior Advisory Editor K. J. Ray Liu, College Park, USA Associate Editors Gonzalo Arce, USA Arden Huang, USA King N. Ngan, Hong Kong Jaakko Astola, Finland Jiri Jan, Czech Douglas O’Shaughnessy, Canada Kenneth Barner, USA Søren Holdt Jensen, Denmark Antonio Ortega, USA Mauro Barni, Italy Mark Kahrs, USA Montse Pardas, Spain Jacob Benesty, Canada Thomas Kaiser, Germany Wilfried Philips, Belgium Kostas Berberidis, Greece Moon Gi Kang, Korea Vincent Poor, USA Helmut Bölcskei, Switzerland Aggelos Katsaggelos, USA Phillip Regalia, France Joe Chen, USA Walter Kellermann, Germany Markus Rupp, Austria Chong-Yung Chi, Taiwan Lisimachos P. Kondi, USA Hideaki Sakai, Japan Satya Dharanipragada, USA Alex Kot, Singapore Bill Sandham, UK Petar M. Djurić, USA C.-C. Jay Kuo, USA Dirk Slock, France Jean-Luc Dugelay, France Geert Leus, The Netherlands Piet Sommen, The Netherlands Frank Ehlers, Germany Bernard C. Levy, USA Dimitrios Tzovaras, Greece Moncef Gabbouj, Finland Mark Liao, Taiwan Hugo Van hamme, Belgium Sharon Gannot, Israel Yuan-Pei Lin, Taiwan Jacques Verly, Belgium Fulvio Gini, Italy Shoji Makino, Japan Xiaodong Wang. USA A. Gorokhov, The Netherlands Stephen Marshall, UK Douglas Williams, USA Peter Handel, Sweden C. Mecklenbräuker, Austria Roger Woods, UK Ulrich Heute, Germany Gloria Menegaz, Italy Jar-Ferr Yang, Taiwan John Homer, Australia Bernie Mulgrew, UK Contents Editorial, Ercan E. Kuruoglu and Carlo Baccigalupi Volume 2005 (2005), Issue 15, Pages 2397-2399 Separation of Correlated Astrophysical Sources Using Multiple-Lag Data Covariance Matrices, L. Bedini, D. Herranz, E. Salerno, C. Baccigalupi, E. E. Kuruoğlu, and A. Tonazzini Volume 2005 (2005), Issue 15, Pages 2400-2412 Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations, Olivier Forni and Nabila Aghanim Volume 2005 (2005), Issue 15, Pages 2413-2425 Detection of Point Sources on Two-Dimensional Images Based on Peaks, M. López-Caniego, D. Herranz, J. L. Sanz, and R. B. Barreiro Volume 2005 (2005), Issue 15, Pages 2426-2436 Blind Component Separation in Wavelet Space: Application to CMB Analysis, Y. Moudden, J.-F. Cardoso, J.-L. Starck, and J. Delabrouille Volume 2005 (2005), Issue 15, Pages 2437-2454 Analysis of the Spatial Distribution of Galaxies by Multiscale Methods, J-L. Starck, V. J. Martínez, D. L. Donoho, O. Levi, P. Querre, and E. Saar Volume 2005 (2005), Issue 15, Pages 2455-2469 Cosmological Non-Gaussian Signature Detection: Comparing Performance of Different Statistical Tests, J. Jin, J.-L. Starck, D. L. Donoho, N. Aghanim, and O. Forni Volume 2005 (2005), Issue 15, Pages 2470-2485 Time-Scale and Time-Frequency Analyses of Irregularly Sampled Astronomical Time Series, C. Thiebaut and S. Roques Volume 2005 (2005), Issue 15, Pages 2486-2499 Restoration of Astrophysical Images—The Case of Poisson Data with Additive Gaussian Noise, H. Lantéri and C. Theys Volume 2005 (2005), Issue 15, Pages 2500-2513 A Data-Driven Multidimensional Indexing Method for Data Mining in Astrophysical Databases, Marco Frailis, Alessandro De Angelis, and Vito Roberto Volume 2005 (2005), Issue 15, Pages 2514-2520 Virtually Lossless Compression of Astrophysical Images, Cinzia Lastri, Bruno Aiazzi, Luciano Alparone, and Stefano Baronti Volume 2005 (2005), Issue 15, Pages 2521-2535 Astrophysical Information from Objective Prism Digitized Images: Classification with an Artificial Neural Network, Emmanuel Bratsolis Volume 2005 (2005), Issue 15, Pages 2536-2545 Multiband Segmentation of a Spectroscopic Line Data Cube: Application to the HI Data Cube of the Spiral Galaxy NGC 4254, Farid Flitti, Christophe Collet, Bernd Vollmer, and François Bonnarel Volume 2005 (2005), Issue 15, Pages 2546-2558 Adaptive DFT-Based Interferometer Fringe Tracking, Edward Wilson, Ettore Pedretti, Jesse Bregman, Robert W. Mah, and Wesley A. Traub Volume 2005 (2005), Issue 15, Pages 2559-2572 Technique for Automated Recognition of Sunspots on Full-Disk Solar Images, S. Zharkov, V. Zharkova, S. Ipson, and A. Benkhalil Volume 2005 (2005), Issue 15, Pages 2573-2584 On-board Data Processing to Lower Bandwidth Requirements on an Infrared Astronomy Satellite: Case of Herschel-PACS Camera, Ahmed Nabil Belbachir, Horst Bischof, Roland Ottensamer, Franz Kerschbaum, and Christian Reimers Volume 2005 (2005), Issue 15, Pages 2585-2594 EURASIP Journal on Applied Signal Processing 2005:15, 2397–2399 c 2005 Hindawi Publishing Corporation Editorial Ercan E. Kuruoglu Istituto di Scienza e Tecnologie dell’Informazione “A. Faedo” (ISTI), Area della ricerca CNR di Pisa, via G. Moruzzi 1, 56124 Pisa, Italy Email: [email protected] Carlo Baccigalupi Scuola Internazionale Superiore di Studi Avanzati (SISSA/ISAS), via Beirut 4, 34014 Trieste, Italy Email: [email protected] We live in an epoch where the frontiers of our investigation formidable challenge for signal processing. We need state-of- and comprehension of fundamental physics depend largely the-art techniques that can analyse, summarise, and extract on the light coming from the sky, that is, on the study of the necessary information from this ocean of data. galactic and extra-galactic radiation. Watching the sky, in Tocontinue with the example above, the microwave sky is principle, we have access to the highest energies conceiv- dominated by the CMB radiation, but several processes con- able, generated by the laws of nature in extreme conditions, tribute to the total emission, coming for instance from all the such as nearby black holes or even close to the origin of processes occurring along the line of sight, such as the emis- the universe itself. For example, in the microwave band, sion from other galaxies or clusters of those, as well as from the extra-Galactic radiation is dominated by a markedly the diffuse gas in our own Galaxy. Each of these processes are isotropic component, obeying a black body spectrum char- most relevant in different contexts in astrophysics and cos- acterized by a temperature of about 2.726 Kelvin. That is mology. Recently, the astrophysics field has benefited a great the relic of the Big Bang, originated just 300 000 years af- deal from the rich research work going on source separation ter the initial starting point of the universe. This radiation, in the signal processing field. Source separation aims at the namely the cosmic microwave background (CMB) radia- recovery of the various different components from the multi- tion, today is the most important observable we have to ac- band observations exploiting the differences between them, cess the mysterious physics of the Big Bang itself. The lat- induced by their independent physical origins. ter is telling us about the unknown fundamental interac- Despite the mutual interest, the two disciplines suffer tions and particles, the physics of spacetime, and the na- from lack of a common publication ground, implying that ture of quantum gravity, and represents the only way to ad- the results produced in one of them are not immediately vis- dress those issues in physics today. Electronics hardware tech- ible in the other. The aim of the present issue is to provide nology has reached in these very recent years the capabil- a unified platform that would strengthen the bridge between ity to study the tiniest details of the CMB, carrying the im- signal processing and astrophysics and cosmology and enable age of the primordial stage of cosmic geometry, structure, the sharing of information. We would like to provide astro- and composition. Such a fantastic challenge is ongoing in physicists and cosmologists with a spectrum of the most ad- this very moment, while several CMB detectors are operating vanced signal processing techniques and the signal process- and advanced probes are being designed for the forthcoming ing community an exposure to various vital real problems in decades. analysing astrophysics data that await solution. Finally, our Many breakthroughs in physics are made possible by aim is to provide a reference for present and future literature, the use of the most advanced data analysis techniques. The in the widest possible context, accounting for various appli- present datasets obtained in astrophysical and cosmologi- cations and algorithms proposed. Indeed, as the reader may cal observations are huge, and cover the entire electromag- see, the topics we collected range from solar physics, thus on netic spectrum, dealing with very different processes, from the scale of stars, to the reconstructuon of the most ambi- gamma and X-rays of the high-energy astrophysics of com- tious signal from the Big Bang, with the reconstruction of pact stars or black holes, to the microwave and infrared emis- the CMB pattern on all sky. The methods
Load more

Recommended publications
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Enrichment of the Galactic Disc with Neutron-Capture Elements: Mo and Ru
    This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record is available online at: https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stz2202/5548790 Enrichment of the Galactic disc with neutron-capture Downloaded from https://academic.oup.com/mnras/advance-article-abstract/doi/10.1093/mnras/stz2202/5548790 by University of Hull user on 14 August 2019 elements: Mo and Ru T. Mishenina1 ⋆, M. Pignatari2,3,6 † *, T. Gorbaneva1, C. Travaglio4,5 † , B. Cˆot´e3,6 † , F.-K. Thielemann7,8, C. Soubiran9 1Astronomical Observatory, Odessa National University, Shevchenko Park, 65014, Odessa, Ukraine 2 E.A. Milne Centre for Astrophysics, Dept of Physics & Mathematics, University of Hull, HU6 7RX, United Kingdom 3 Konkoly Observatory, Hungarian Academy of Sciences, Konkoly Thege Miklos ut 15-17, H-1121 Budapest, Hungary 4 INFN, University of Turin, Via Pietro Giuria 1, 10025 Turin, Italy 5 B2FH Association, Turin, Italy 6 Joint Institute for Nuclear Astrophysics - Center for the Evolution of the Elements, USA 7 Department of Physics, University of Basel, Klingelbergstrabe 82, 4056 Basel, Switzerland 8 GSI Helmholtzzentrum fr Schwerionenforschung, Planckstrasse 1, D-64291 Darmstadt, Germany 9 Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux - CNRS, B18N, all´ee Geoffroy Saint-Hilaire, 33615 Pessac, France Accepted 2015 xxx. Received 2015 xxx; in original form 2015 xxx ABSTRACT We present new observational data for the heavy elements molybdenum (Mo, Z = 42) and ruthenium (Ru, Z = 44) in F-, G-, and K-stars belonging to different substructures of the Milky Way.
    [Show full text]
  • Csillagászati Évkönyv
    meteor csillagászati évkönyv meteor csillagászati évkönyv 2006 szerkesztette: Mizser Attila Taracsák Gábor Magyar Csillagászati Egyesület Budapest, 2005 A z évkönyv összeállításában közreműködött: Horvai Ferenc Jean Meeus (Belgium) Sárneczky Krisztián Szakmailag ellenőrizte: Szabados László (cikkek, beszámolók) Szabadi Péter (táblázatok) Műszaki szerkesztés és illusztrációk: Taracsák Gábor A szerkesztés és a kiadás támogatói: MLog Műszereket Gyártó és Forgalmazó Kft. MTA Csillagászati Kutatóintézete ISSN 0866-2851 Felelős kiadó: Mizser Attila Készült a G-PRINT BT. nyomdájában Felelős vezető: Wilpert Gábor Terjedelem: 18.75 ív + 8 oldal melléklet Példányszám: 4000 2005. október Csillagászati évkönyv 2006 5 Tartalom Tartalom B evezető.......................................................................................................................... 7 Használati útmutató ...................................................... .......................................... 8 Jelek és rövidítések .................................................................................................. 13 A csillagképek latin és magyar n e v e ........................................................................14 Táblázatok Jelenségnaptár............................................................................................................ 16 A bolygók kelése és nyugvása (ábra) ................................................................. 64 A bolygók a d a ta i....................................................................................................
    [Show full text]
  • Orders of Magnitude (Length) - Wikipedia
    03/08/2018 Orders of magnitude (length) - Wikipedia Orders of magnitude (length) The following are examples of orders of magnitude for different lengths. Contents Overview Detailed list Subatomic Atomic to cellular Cellular to human scale Human to astronomical scale Astronomical less than 10 yoctometres 10 yoctometres 100 yoctometres 1 zeptometre 10 zeptometres 100 zeptometres 1 attometre 10 attometres 100 attometres 1 femtometre 10 femtometres 100 femtometres 1 picometre 10 picometres 100 picometres 1 nanometre 10 nanometres 100 nanometres 1 micrometre 10 micrometres 100 micrometres 1 millimetre 1 centimetre 1 decimetre Conversions Wavelengths Human-defined scales and structures Nature Astronomical 1 metre Conversions https://en.wikipedia.org/wiki/Orders_of_magnitude_(length) 1/44 03/08/2018 Orders of magnitude (length) - Wikipedia Human-defined scales and structures Sports Nature Astronomical 1 decametre Conversions Human-defined scales and structures Sports Nature Astronomical 1 hectometre Conversions Human-defined scales and structures Sports Nature Astronomical 1 kilometre Conversions Human-defined scales and structures Geographical Astronomical 10 kilometres Conversions Sports Human-defined scales and structures Geographical Astronomical 100 kilometres Conversions Human-defined scales and structures Geographical Astronomical 1 megametre Conversions Human-defined scales and structures Sports Geographical Astronomical 10 megametres Conversions Human-defined scales and structures Geographical Astronomical 100 megametres 1 gigametre
    [Show full text]
  • Paul Willard Merrill
    NATIONAL ACADEMY OF SCIENCES P A U L W I L L A R D M ERRILL 1887—1961 A Biographical Memoir by OL I N C . W I L S O N Any opinions expressed in this memoir are those of the author(s) and do not necessarily reflect the views of the National Academy of Sciences. Biographical Memoir COPYRIGHT 1964 NATIONAL ACADEMY OF SCIENCES WASHINGTON D.C. PAUL WILLARD MERRILL August i$, 1887—July ig, ig6i BY OLIN C. WILSON A STRONOMY, by its very nature, has always been pre-eminently an 1\- observational science. Progress in astronomy has come about in two ways: first, by the use of more and more powerful methods of observation and, second, by the application of improved physical theory in seeking to interpret the observations. Approximately one hundred years ago the pioneers in stellar spectroscopy began to lay the foundations of modern astrophysics by applying the spectroscope to the study of celestial bodies. Certainly during most of this period observation has led the way in the attack on the unknown. Even today, although theory has made enormous strides in the past thirty or forty years, observation continues to uncover phenomena which were unanticipated by the theorists and which are, in some instances, far from easy to account for. The chosen field of the subject of this memoir was stellar spectros- copy, and his active career spanned the second half of the period since work was begun in that branch of astronomy. To some extent his professional life formed a link between the early pioneering times, when theoretical explanation of the observed phenomena was virtually nonexistent, and the present day.
    [Show full text]
  • Astrophysics
    Publications of the Astronomical Institute rais-mf—ii«o of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE IA U Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 1987 Publications of the Astronomical Institute of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE I A U 10 Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 5 1 987 CHIEF EDITOR OF THE PROCEEDINGS: LUBOS PEREK Astronomical Institute of the Czechoslovak Academy of Sciences 251 65 Ondrejov, Czechoslovakia TABLE OF CONTENTS Preface HI Invited discourse 3.-C. Pecker: Fran Tycho Brahe to Prague 1987: The Ever Changing Universe 3 lorlishdp on rapid variability of single, binary and Multiple stars A. Baglln: Time Scales and Physical Processes Involved (Review Paper) 13 Part 1 : Early-type stars P. Koubsfty: Evidence of Rapid Variability in Early-Type Stars (Review Paper) 25 NSV. Filtertdn, D.B. Gies, C.T. Bolton: The Incidence cf Absorption Line Profile Variability Among 33 the 0 Stars (Contributed Paper) R.K. Prinja, I.D. Howarth: Variability In the Stellar Wind of 68 Cygni - Not "Shells" or "Puffs", 39 but Streams (Contributed Paper) H. Hubert, B. Dagostlnoz, A.M. Hubert, M. Floquet: Short-Time Scale Variability In Some Be Stars 45 (Contributed Paper) G. talker, S. Yang, C. McDowall, G. Fahlman: Analysis of Nonradial Oscillations of Rapidly Rotating 49 Delta Scuti Stars (Contributed Paper) C. Sterken: The Variability of the Runaway Star S3 Arietis (Contributed Paper) S3 C. Blanco, A.
    [Show full text]
  • 1903Aj 23 . . . 22K 22 the Asteojsomic Al
    22 THE ASTEOJSOMIC AL JOUENAL. Nos- 531-532 22K . Taking into account the smallness of the weights in- concerned. Through the use of these tables the positions . volved, the individual differences which make up the and motions of many stars not included in the present 23 groups in the preceding table agree^very well. catalogue can be brought into systematic harmony with it, and apparently without materially less accuracy for the in- dividual stars than could be reached by special compu- Tables of Systematic Correction for N2 and A. tations for these stars in conformity with the system of B. 1903AJ The results of the foregoing comparisons. have been This is especially true of the star-places computed by utilized to form tables of systematic corrections for ISr2, An, Dr. Auwers in the catalogues, Ai and As. As will be seen Ai and As. In right-ascension no distinction is necessary by reference to the catalogue the positions and motions of between the various catalogues published by Dr. Auwers, south polar stars taken from N2 agree better with the beginning with the Fundamental-G at alo g ; but in decli- results of this investigation than do those taken from As, nation the distinction between the northern, intermediate, which, in turn, are quoted from the Cape Catalogue for and southern catalogues must be preserved, so far as is 1890. SYSTEMATIC COBEECTIOEB : CEDEE OF DECLINATIONS. Eight-Ascensions ; Cokrections, ¿las and 100z//xtf. Declinations; Corrections, Æs and IOOzZ/x^. B — ISa B —A B —N2 B —An B —Ai âas 100 â[is âas 100 âgô âSs 100
    [Show full text]
  • Bibliography from ADS File: Lambert.Bib August 16, 2021 1
    Bibliography from ADS file: lambert.bib Reddy, A. B. S. & Lambert, D. L., “VizieR Online Data Cata- August 16, 2021 log: Abundance ratio for 5 local stellar associations (Reddy+, 2015)”, 2018yCat..74541976R ADS Reddy, A. B. S., Giridhar, S., & Lambert, D. L., “VizieR Online Data Deepak & Lambert, D. L., “Lithium in red giants: the roles of the He-core flash Catalog: Line list for red giants in open clusters (Reddy+, 2015)”, and the luminosity bump”, 2021arXiv210704624D ADS 2017yCat..74504301R ADS Deepak & Lambert, D. L., “Lithium in red giants: the roles of the He-core flash Ramírez, I., Yong, D., Gutiérrez, E., et al., “Iota Horologii Is Unlikely to Be an and the luminosity bump”, 2021MNRAS.tmp.1807D ADS Evaporated Hyades Star”, 2017ApJ...850...80R ADS Deepak & Lambert, D. L., “Lithium abundances and asteroseismology of red gi- Ramya, P., Reddy, B. E., Lambert, D. L., & Musthafa, M. M., “VizieR On- ants: understanding the evolution of lithium in giants based on asteroseismic line Data Catalog: Hercules stream K giants analysis (Ramya+, 2016)”, parameters”, 2021MNRAS.505..642D ADS 2017yCat..74601356R ADS Federman, S. R., Rice, J. S., Ritchey, A. M., et al., “The Transition Hema, B. P., Pandey, G., Kamath, D., et al., “Abundance Analyses of from Diffuse Molecular Gas to Molecular Cloud Material in Taurus”, the New R Coronae Borealis Stars: ASAS-RCB-8 and ASAS-RCB-10”, 2021ApJ...914...59F ADS 2017PASP..129j4202H ADS Bhowmick, A., Pandey, G., & Lambert, D. L., “Fluorine detection in hot extreme Pandey, G. & Lambert, D. L., “Non-local Thermodynamic Equilibrium Abun- helium stars”, 2020JApA...41...40B ADS dance Analyses of the Extreme Helium Stars V652 Her and HD 144941”, Reddy, A.
    [Show full text]
  • Meteor Csillagászati Évkönyv 2015
    Ár: 3000 Ft 015 2 csillagászati évkönyv r meteor o e csillagászati évkönyv t e m 2015 ISSN 0866 - 2851 9 7 7 0 8 6 6 2 8 5 0 0 2 METEOR CSILLAGÁSZATI ÉVKÖNYV 2015 METEOR CSILLAGÁSZATI ÉVKÖNYV 2015 MCSE – 2014. SZEPTEMBER–NOVEMBER METEOR CSILLAGÁSZATI ÉVKÖNYV 2015 MCSE – 2014. SZEPTEMBER–NOVEMBER meteor csillagászati évkönyv 2015 Szerkesztette: Benkõ József Mizser Attila Magyar Csillagászati Egyesület www.mcse.hu Budapest, 2014 METEOR CSILLAGÁSZATI ÉVKÖNYV 2015 MCSE – 2014. SZEPTEMBER–NOVEMBER Az évkönyv kalendárium részének összeállításában közremûködött: Bagó Balázs Görgei Zoltán Kaposvári Zoltán Kiss Áron Keve Kovács József Molnár Péter Sárneczky Krisztián Sánta Gábor Szabadi Péter Szabó M. Gyula Szabó Sándor Szöllôsi Attila A kalendárium csillagtérképei az Ursa Minor szoftverrel készültek. www.ursaminor.hu Szakmailag ellenôrizte: Szabados László A kiadvány a Magyar Tudományos Akadémia támogatásával készült. További támogatóink mindazok, akik az SZJA 1%-ával támogatják a Magyar Csillagászati Egyesületet. Adószámunk: 19009162-2-43 Felelôs kiadó: Mizser Attila Nyomdai elôkészítés: Kármán Stúdió, www.karman.hu Nyomtatás, kötészet: OOK-Press Kft., www.ookpress.hu Felelôs vezetô: Szathmáry Attila Terjedelem: 23 ív fekete-fehér + 8 oldal színes melléklet 2014. november ISSN 0866-2851 METEOR CSILLAGÁSZATI ÉVKÖNYV 2015 MCSE – 2014. SZEPTEMBER–NOVEMBER Tartalom Bevezetô ................................................... 7 Kalendárium ............................................... 13 Cikkek Kiss László: A változócsillagászat újdonságai .................... 227 Tóth Imre: Az üstökösök megismerésének mérföldkövei ........... 242 Petrovay Kristóf: Az éghajlatváltozás és a Nap ................... 265 Kovács József: A kozmológiai állandótól a sötét energiáig – 100 éves az általános relativitáselmélet ...................... 280 Szabados László: A jó „öreg” Hubble-ûrtávcsô ................... 296 Kolláth Zoltán: A fényszennyezésrôl a Fény Nemzetközi Évében 311 Beszámolók Mizser Attila: A Magyar Csillagászati Egyesület 2013.
    [Show full text]
  • Variable Star Section Circular
    The British Astronomical Association Variable Star Section Circular No. 177 September 2018 Office: Burlington House, Piccadilly, London W1J 0DU Contents Observers Workshop – Variable Stars, Photometry and Spectroscopy 3 From the Director 4 CV&E News – Gary Poyner 6 AC Herculis – Shaun Albrighton 8 R CrB in 2018 – the longest fully substantiated fade – John Toone 10 KIC 9832227, a potential Luminous Red Nova in 2022 – David Boyd 11 KK Per, an irregular variable hiding a secret - Geoff Chaplin 13 Joint BAA/AAVSO meeting on Variable Stars – Andy Wilson 15 A Zooniverse project to classify periodic variable stars from SuperWASP - Andrew Norton 30 Eclipsing Binary News – Des Loughney 34 Autumn Eclipsing Binaries – Christopher Lloyd 36 Items on offer from Melvyn Taylor’s library – Alex Pratt 44 Section Publications 45 Contributing to the VSSC 45 Section Officers 46 Cover images Vend47 or ASASSN-V J195442.95+172212.6 2018 August 14.294, iTel 0.62m Planewave CDK @ f6.5 + FLI PL09--- CCD. 60 secs lum. Martin Mobberley Spectrum taken with a LISA spectroscope on Aug 16.875UT. C-11. Total exposure 1.1hr David Boyd Click on images to see in larger scale 2 Back to contents Observers' Workshop - Variable Stars, Photometry and Spectroscopy. Venue: Burlington House, Piccadilly, London, W1J 0DU (click to see map) Date: Saturday, 2018, September 29 - 10:00 to 17:30 For information about booking for this meeting, click here. A workshop to help you get the best from observing the stars, be it visually, with a CCD or DSLR or by using a spectroscope. The topics covered will include: • Visual observing with binoculars or a telescope • DSLR and CCD observing • What you can learn from spectroscopy And amongst those topics the types of star covered will include, CV and Eruptive Stars, Pulsating Stars and Eclipsing Binaries.
    [Show full text]
  • Instruction Manual
    iOptron® GEM28 German Equatorial Mount Instruction Manual Product GEM28 and GEM28EC Read the included Quick Setup Guide (QSG) BEFORE taking the mount out of the case! This product is a precision instrument and uses a magnetic gear meshing mechanism. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. You must hold the mount firmly when disengaging or adjusting the gear switches. Otherwise personal injury and/or equipment damage may occur. Any worm system damage due to improper gear meshing/slippage will not be covered by iOptron’s limited warranty. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while observing. 2 Table of Content Table of Content ................................................................................................................................................. 3 1. GEM28 Overview .......................................................................................................................................... 5 2. GEM28 Terms ................................................................................................................................................ 6 2.1. Parts List .................................................................................................................................................
    [Show full text]
  • Abundances of Neutron-Capture Elements in Stars of the Galactic Disk Substructures Formed Right After the Third Dredged-Up Event Straniero Et Al
    Astronomy & Astrophysics manuscript no. aa˙ref˙ang c ESO 2018 September 11, 2018 Abundances of neutron-capture elements in stars of the galactic disk substructures ⋆ ⋆⋆ T.V. Mishenina1,2, M. Pignatari3, S.A. Korotin1, C. Soubiran2, C. Charbonnel4,5, F.-K. Thielemann3, T.I. Gorbaneva1, and N.Yu. Basak1 1 Astronomical Observatory, Odessa National University, and Isaac Newton Institute of Chile, Odessa Branch, T.G.Shevchenko Park, Odessa 65014 Ukraine, email:[email protected] 2 Universit´ede Bordeaux 1 - CNRS - Laboratoire d’Astrophysique de Bordeaux, UMR 5804, BP 89, 33271 Floirac Cedex, France, email:[email protected] 3 Department of Physics, University of Basel, Klingelbergstrabe 82, 4056 Basel, Switzerland email:[email protected] 4 Geneva Observatory, University of Geneva, 1290 Versoix, Switzerland 5 IRAP, UMR 5277 CNRS and Universit´ede Toulouse, 31400 Toulouse, France ABSTRACT Aims. The aim of this work is to present and discuss the observations of the iron peak (Fe, Ni) and neutron-capture element (Y, Zr, Ba, La, Ce, Nd, Sm, and Eu) abundances for 276 FGK dwarfs, located in the galactic disk with metallicity -1 < [Fe/H] < +0.3. Methods. Atmospheric parameters and chemical composition of the studied stars were determined from an high resolution, high signal-to-noise echelle spectra obtained with the echelle spectrograph ELODIE at the Observatoire de Haute-Provence (France). Effective temperatures were estimated by the line depth ratio method and from the Hα line-wing fitting. Surface gravities (log g) were determined by parallaxes and the ionization balance of iron. Abundance determinations were carried out using the LTE approach, taking the hyperfine structure for Eu into account, and the abundance of Ba was computed under the NLTE approximation.
    [Show full text]