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Spectroscopic Orbits of Three Dwarf Barium Stars
SPECTROSCOPIC ORBITS OF THREE DWARF BARIUM STARS By P. L. North1, A. Jorissen2, A. Escorza2;3, B. Miszalski4;5, and J. Mikoajewska6 1Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique F´ed´erale de Lausanne (EPFL), Switzerland 2Institut d'Astronomie et d'Astrophysique, Universit´eLibre de Bruxelles, Belgium 3Instituut voor Sterrenkunde, KU Leuven, Belgium 4South African Astronomical Observatory 5Southern African Large Telescope Foundation 6N. Copernicus Astronomical Center, Polish Academy of Sciences, Warsaw, Poland Barium stars are thought to result from binary evolution in systems wide enough to allow the more massive component to reach the asymptotic giant branch and eventually become a CO white dwarf. While Ba stars were initially known only among giant or subgiant stars, some were subsequently discovered also on the main sequence (and known as dwarf Ba stars). We provide here the orbital parameters of three dwarf Ba stars, completing the sample of 27 orbits published recently by Escorza et al. with these three southern targets. We show that these new orbital parameters are consistent with those of other dwarf Ba stars. Introduction Barium stars are not evolved enough to synthesize in their interiors and dredge up to their surface the s-process elements (including Ba) that are very abundant in their atmospheres. On the other hand, we have convincing statistical indications that they all belong to SB1-type binary systems [1] [2], and UV arXiv:2001.11319v1 [astro-ph.SR] 30 Jan 2020 observations have revealed the white -
Longterm MWL Behavior of 1ES1959+650
Fakultät Physik – Experimentelle Physik 5 Long-term observations of the TeV blazar 1ES 1959+650 Temporal and spectral behavior in the multi-wavelength context Dissertation zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften (Dr. rer. nat.) vorgelegt von Dipl.-Phys. Michael Backes Dezember 2011 Contents 1 Introduction 1 2 Brief Introduction to Astroparticle Physics 3 2.1 ChargedCosmicRays .............................. 4 2.1.1 CompositionofCosmicRays . 4 2.1.2 EnergySpectrumofCosmicRays. 5 2.1.3 Sources of Cosmic Rays up to 1018 eV................ 6 ∼ 2.1.4 Sources of Cosmic Rays above 1018 eV................ 8 ∼ 2.2 AstrophysicalNeutrinos . ... 12 2.3 PhotonsfromOuterSpace. 13 2.3.1 Leptonic Processes: Connecting Low and High Energy Photons . 13 2.3.2 Hadronic Processes: Connecting Photons, Protons, and Neutrinos . 16 2.4 ActiveGalacticNuclei . 16 2.4.1 Blazars .................................. 17 2.4.2 EmissionModels ............................. 19 2.4.3 BinaryBlackHolesinAGN . 20 3 Instruments for Multi-Wavelength Astronomy 25 3.1 RadioandMicrowave .............................. 25 3.1.1 Single-DishInstruments . 25 3.1.2 Interferometers .............................. 26 3.1.3 Satellites ................................. 27 3.2 Infrared ...................................... 27 3.3 Optical ...................................... 28 3.3.1 Satellite-Born............................... 28 3.3.2 Ground-Based .............................. 28 3.4 Ultraviolet..................................... 29 3.5 X-Rays ..................................... -
NORDIC OPTICAL TELESCOPE Johannes Andersen Student
NORDIC OPTICAL TELESCOPE Johannes Andersen Student programme The Nordic Optical Telescope1 (NOT) at La Palma, Spain, invites applications for Research Studentships starting at any time from January 2021 onward. NOT is a modern 2.6-m telescope with state-of-the-art optical and near-IR instruments. Our staff of ~18, including astronomers, engineers, and students, and informal, hands-on style of operation offer attractive training opportunities for young Nordic scientists and engineers. The NOT Research Studentship programme offers support for a limited number of PhD or advanced MSc astronomy or engineering students who wish to profit from these opportunities. Stipends cover living expenses on La Palma for periods of typically a year; in return, students spend ~30% of their time contributing to the operation or development of NOT, with the rest devoted to thesis work. Thesis subjects may be astronomical and include observations with the NOT, or they may concern developments in optics, detectors, electronics, or software. An extension of the studentships by 6 months is normally granted. Johannes Andersen (1943-2020) has been an extremely important person in the history of NOT, being many years member of the NOT Council, and being its director from 2002 till 2013. Johannes has been instrumental in making NOT what it is today, but his pride and joy was the studentship programme, which he largely shaped to its present form. In his honour, and in recognition of his fundamental contribution, the studentship programme has been named after Johannes. Applicants should (see http://www.not.iac.es/general/studentships/ for further details): 1. -
NORDIC OPTICAL TELESCOPE Research Studentships
NORDIC OPTICAL TELESCOPE Research Studentships The Nordic Optical Telescope1 (NOT) at La Palma, Spain, invites applications for Research Studentships starting at any time from June 2020 onward. NOT is a modern 2.6-m telescope with state-of-the-art optical and near-IR instruments. Our staff of ~18, including astronomers, engineers, and students, and informal, hands-on style of operation offer attractive training opportunities for young Nordic scientists and engineers. The NOT Research Studentship programme offers support for a limited number of PhD or advanced MSc astronomy or engineering students who wish to profit from these opportunities. Stipends cover living expenses on La Palma for periods of typically a year; in return, students spend ~30% of their time contributing to the operation or development of NOT, with the rest devoted to thesis work. Thesis subjects may be astronomical and include observations with the NOT, or they may concern developments in optics, detectors, electronics, or software. Our staff will monitor the progress of each student and provide scientific and technical guidance as appropriate in each case. An extension of the studentships by 6 months is normally granted. Applicants should (see http://www.not.iac.es/general/studentships/ for further details): 1. Be enrolled in a PhD or MSc programme in astronomy or a related technical discipline at a recognised university or similar academic institution. Preference is given to PhD students and applicants from the Nordic countries. 2. Have a strong interest in observational astrophysics and/or astronomical instrumentation. 3. Be capable and willing to work during night- as well as daytime, occasionally also on weekends or public holidays, at an altitude of 2400 metres above sea level, and to take up residence on La Palma for the duration of the Studentship. -
Nordic Research Board - Application for Research Training Course Beslutning: Mottagit: Ref.Nr
Nordic Research Board - Application for research training course Beslutning: Mottagit: Ref.nr.: 1 Last name First name Sex Title/position Sollerman Jesper Male Docent/Researcher University Academic degree Copenhagen University PhD, Docent Department/institution Telephone (work) Mobile Danish Dark Universe Centre, Niels Bohr Institute +46 8 5537 8554 Department/institution address Telefax (work) NBI, Juliane Maries Vej 30 +45 35 32 59 89 Postal code City Country E-mail 2100 Copenhagen Denmark [email protected] 2 Title of the project/activity (max 50 characters) Observational Astrophysics at the Telescope 3 Date of single course (dd.mm.yyyy): 4 Subject area (See last page) From: 01 07 2006 To: 14 07 2006 Physics 5 Meeting venue Country Roque de los Muchachos,La Palma,Canary Isl. Spain 6 Estimated number of Other Other DK FI IS NO SE EE LV LT RU inside outside the Total Men Women participants the EU* EU* Research students 3 3 1 2 3 1 1 1 1 0 0 16 8 8 Other participants Teachers 3 1 1 2 7 5 2 *Other countries 7 Summary. Give a short description of the course´s targets and aims (max. 200 words). Nordic Research Board reserves the right to use parts of or the text in full for information purposes. The aim of the course is to introduce about 16 Nordic PhD students to observational astrophysics. At La Palma, we will have access to the modern facilities required for the successful execution of this advanced graduate course. The Nordic Optical Telescope (NOT) and the Swedish Solar Telescope (SST) are both up-to-date telescopes. -
Stellar Spectral Classification of Previously Unclassified Stars Gsc 4461-698 and Gsc 4466-870" (2012)
University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2012 Stellar Spectral Classification Of Previously Unclassified tS ars Gsc 4461-698 And Gsc 4466-870 Darren Moser Grau Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Grau, Darren Moser, "Stellar Spectral Classification Of Previously Unclassified Stars Gsc 4461-698 And Gsc 4466-870" (2012). Theses and Dissertations. 1350. https://commons.und.edu/theses/1350 This Thesis is brought to you for free and open access by the Theses, Dissertations, and Senior Projects at UND Scholarly Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. STELLAR SPECTRAL CLASSIFICATION OF PREVIOUSLY UNCLASSIFIED STARS GSC 4461-698 AND GSC 4466-870 By Darren Moser Grau Bachelor of Arts, Eastern University, 2009 A Thesis Submitted to the Graduate Faculty of the University of North Dakota in partial fulfillment of the requirements For the degree of Master of Science Grand Forks, North Dakota December 2012 Copyright 2012 Darren M. Grau ii This thesis, submitted by Darren M. Grau in partial fulfillment of the requirements for the Degree of Master of Science from the University of North Dakota, has been read by the Faculty Advisory Committee under whom the work has been done and is hereby approved. _____________________________________ Dr. Paul Hardersen _____________________________________ Dr. Ronald Fevig _____________________________________ Dr. Timothy Young This thesis is being submitted by the appointed advisory committee as having met all of the requirements of the Graduate School at the University of North Dakota and is hereby approved. -
I Am: Astronomy Who Is? Travel in a Path Around
I am: Astronomy I am: Orbit Who is? travel in a path Who is? More oval in shape around the Sun than perfectly circular I am: Rotate I am: Solar system Who is? An imaginary line Who is? Spins on an axis that runs through the middle of an object I am: An axis I am: Gravity Who is? Used to measure Who is? A force that keeps distances in the solar satellites in orbit system I am: An astronomical unit I am: A nebula Who is? A rotating cloud of Who is? Mercury, Venus, dust and gas Earth & Mars I am: The inner planets I am: A crater Who is? A bowl shaped depression that forms when The smallest inner an object crashes into a Who is? surface planet I am: Mercury I am: Venus Who is? The second planet Who is? The third planet from the Sun? from the Sun I am: Earth I am: Revolve Who is? The fourth planet Who is? The path made from the Sun? during a revolution around the Sun I am: Mars I am: Asteroids Who is? Small, rocky Who is? Beyond the objects that orbit the Sun asteroid belt I am: Elliptical I am: The outer planets Who is? The Sun and all it’s Who is? So large that all satellites other planets could fit in it I am: Jupiter I am: Saturn Who is? The second largest Who is? 4 times larger than planet in the solar system Earth? I am: Uranus I am: Comets Who is? Frozen chunks of Who is? Pieces of rock or ice, gas and dust metal in space, smaller than a few hundred meters I am: Meteoroids I am: Meteor Who is? Streak of light from Who is? Meteor that hits a burning meteoroid the Earth’s surface I am: Meteorite I am: Nuclear fusion Who is? A reaction -
Optical Counterparts of ROSAT X-Ray Sources in Two Selected Fields at Low
Astronomy & Astrophysics manuscript no. sbg˙comsge˙ed c ESO 2018 October 16, 2018 Optical counterparts of ROSAT X-ray sources in two selected fields at low vs. high Galactic latitudes J. Greiner1, G.A. Richter2 1 Max-Planck-Institut f¨ur extraterrestrische Physik, 85740 Garching, Germany 2 Sternwarte Sonneberg, 96515 Sonneberg, Germany Received 14 October 2013 / Accepted 12 August 2014 ABSTRACT Context. The optical identification of large number of X-ray sources such as those from the ROSAT All-Sky Survey is challenging with conventional spectroscopic follow-up observations. Aims. We investigate two ROSAT All-Sky Survey fields of size 10◦× 10◦ each, one at galactic latitude b = 83◦ (26 Com), the other at b = –5◦ (γ Sge), in order to optically identify the majority of sources. Methods. We used optical variability, among other more standard methods, as a means of identifying a large number of ROSAT All- Sky Survey sources. All objects fainter than about 12 mag and brighter than about 17 mag, in or near the error circle of the ROSAT positions, were tested for optical variability on hundreds of archival plates of the Sonneberg field patrol. Results. The present paper contains probable optical identifications of altogether 256 of the 370 ROSAT sources analysed. In partic- ular, we found 126 AGN (some of them may be misclassified CVs), 17 likely clusters of galaxies, 16 eruptive double stars (mostly CVs), 43 chromospherically active stars, 65 stars brighter than about 13 mag, 7 UV Cet stars, 3 semiregular resp. slow irregular variable stars of late spectral type, 2 DA white dwarfs, 1 Am star, 1 supernova remnant and 1 planetary nebula. -
FIES: the High-Resolution Fiber-Fed Echelle Spectrograph at the Nordic Optical Telescope
Astron. Nachr. /AN 335, No. 1, 41 – 45 (2014) / DOI 10.1002/asna.201312007 FIES: The high-resolution Fiber-fed Echelle Spectrograph at the Nordic Optical Telescope J.H. Telting1,, G. Avila2, L. Buchhave3,S.Frandsen4,D.Gandolfi5, B. Lindberg6, H.C. Stempels7,the NOT staff1, and S. Prins8 1 Nordic Optical Telescope, Roque de Los Muchachos Observatory, Rambla Jos´eAnaFern´andez P´erez 7, 38711 Bre˜na Baja, La Palma, Canarias, Spain 2 Photonics and Optics Group, European Southern Observatory, Germany 3 Niels Bohr Institute, University of Copenhagen, Denmark 4 Department of Physics and Astronomy, University of Aarhus, Denmark 5 Research and Scientific Support Department, ESTEC/ESA, Netherlands 6 LensTech AB, Skellefte˚a, Sweden 7 Department of Physics and Astronomy, Uppsala University, Sweden 8 Mercator Telescope, Instituut voor Sterrenkunde, KULeuven, Belgium Received 2013 Aug 30, accepted 2013 Nov 1 Published online 2014 Jan 15 Key words instrumentation: spectrographs – techniques: radial velocities – techniques: spectroscopic FIES is a cross-dispersed high-resolution echelle spectrograph at the 2.56 m Nordic Optical Telescope (NOT), and was optimised for throughput and stability in 2006. The major 2006 upgrade involved the relocation of FIES to a stable environment and development of a fiber bundle that offers 3 different resolution modes, and made FIES an attractive tool for the user community of the NOT. Radial-velocity stability is achieved through double-chamber active temperature control. A dedicated data reduction tool, FIEStool, was developed. As a result of these upgrades, FIES is now one of the work-horse instruments at the NOT. c 2014 WILEY-VCH Verlag GmbH & Co. -
KELT-17: a Chemically Peculiar Am Star and a Hot-Jupiter Planet
manuscript no. saffe c 2020 July 29, 2020 KELT-17: a chemically peculiar Am star and a hot-Jupiter planet⋆ C. Saffe1, 2, 6, P. Miquelarena1, 2, 6, J. Alacoria1, 6, J. F. González1, 2, 6, M. Flores1, 2, 6, M. Jaque Arancibia4, 5, D. Calvo2, E. Jofré7, 3, 6 and A. Collado1, 2, 6 1 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), C.C 467, 5400, San Juan, Argentina. 2 Universidad Nacional de San Juan (UNSJ), Facultad de Ciencias Exactas, Físicas y Naturales (FCEFN), San Juan, Argentina. 3 Observatorio Astronómico de Córdoba (OAC), Laprida 854, X5000BGR, Córdoba, Argentina. 4 Instituto de Investigación Multidisciplinar en Ciencia y Tecnología, Universidad de La Serena, Raúl Bitrán 1305, La Serena, Chile 5 Departamento de Física y Astronomía, Universidad de La Serena, Av. Cisternas 1200 N, La Serena, Chile. 6 Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Argentina 7 Instituto de Astronomía, Universidad Nacional Autónoma de México, Ciudad Universitaria, CDMX, C.P. 04510, México Received xxx, xxx ; accepted xxxx, xxxx ABSTRACT Context. The detection of planets orbiting chemically peculiar stars is very scarcely known in the literature. Aims. To determine the detailed chemical composition of the remarkable planet host star KELT-17. This object hosts a hot-Jupiter planet with 1.31 MJup detected by transits, being one of the more massive and rapidly rotating planet hosts to date. We aimed to derive a complete chemical pattern for this star, in order to compare it with those of chemically peculiar stars. Methods. We carried out a detailed abundance determination in the planet host star KELT-17 via spectral synthesis. -
Refined Chemical Abundances of Π Dra and Hr 7545 With
International Journal of Research in Science and Technology http://www.ijrst.com (IJRST) 2017, Vol. No. 7, Issue No. III, Jul-Sep e-ISSN: 2249-0604, p-ISSN: 2454-180X REFINED CHEMICAL ABUNDANCES OF DRA AND HR 7545 WITH ATLAS12 *Doğuş Özuyar, *Aslı Elmaslı, *Şeyma Çalışkan *Department of Astronomy and Space Sciences, Ankara University, Science Faculty Ankara, Turkey ABSTRACT We present the more refined abundances of elements (C, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Ni, Zn, Sr, Y, Zr and Ba) determined using the computationally intensive ATLAS12 atmosphere model for the metallic-line stars Dra and HR 7545. We compare the chemical abundances derived from ATLAS9 model atmosphere with those of derived from ATLAS12. The abundances are in agreement with each other, within their uncertainties. We thus state that ATLAS9 may be used for the abundance analysis of slowly rotating chemically peculiar stars, such as Dra and HR 7545. Keywords: metallic-line stars; Dra; HR 7545; chemical abundance; ATLAS9; ATLAS12) INTRODUCTION One of A-type star sub-groups, called metallic-line A-type (hereafter Am) stars, exhibits generally A-type spectral behavior with some elemental anomalies. These anomalies are typically deficiency of Sc and sometimes Ca, under-abundances in the light elements (C, O, etc.), followed by an increase in iron-peak element (Cr, Mn, Fe, Ni, etc.) abundances, and a considerably overabundances in the heavy elements, such as Sr, Y, Zr, and Ba, with respect to the solar values [1]. Another characteristic property of Am stars is their low rotational velocities compared to normal A-type stars (< 120 km s-1, [2]). -
THE UBC-OAN PHOTOMETRIC SURVEY by FRANCOIS
SEARCHING FOR NORTHERN ROAP STARS: THE UBC-OAN PHOTOMETRIC SURVEY By FRANCOIS CHAGNON B. Sc. (Specialise en Physique) Universite de Montreal (1996) A THESIS SUBMITTED IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE in THE FACULTY OF GRADUATE STUDIES DEPARTMENT OF PHYSICS & ASTRONOMY We accept this thesis as conforming to the required standard THE UNIVERSITY OF BRITISH COLUMBIA September 1998 © FRANCOIS CHAGNON, 1998 In presenting this thesis in partial fulfilment of the requirements for an advanced degree at the University of British Columbia, I agree that the Library shall make it freely available for reference and study. I further agree that permission for extensive copying of this thesis for scholarly purposes may be granted by the head of my department or by his or her representatives. It is understood that copying or publication of this thesis for financial gain shall not be allowed without my written permission. Department of Physics & Astronomy The University of British Columbia 129-2219 Main Mall Vancouver, Canada V6T 1Z4 Date: Abstract Because they pulsate in multiple high-overtone p-modes, rapidly oscillating Ap stars (roAp) represent a very powerful tool to apply the techniques of asteroseismology, which can lead to the global properties and internal structure of stars. The majority of roAp stars are in the Southern Hemisphere, beyond the reach of northern observatories like CFHT and DAO, which have superb coude spectrographs that can help reveal additional modes and clues to the pulsation dynamics. To try to correct this imbalance, we began a systematic search for roAp stars in the Northern Hemisphere.