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September 2020 BRAS Newsletter
A Neowise Comet 2020, photo by Ralf Rohner of Skypointer Photography Monthly Meeting September 14th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: NASA Michoud Assembly Facility Director, Robert Champion What's In This Issue? President’s Message Secretary's Summary Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner –My Quest For A Dark Place, by Chris Carlton Astro-Photos by BRAS Members Messages from the HRPO REMOTE DISCUSSION Solar Viewing Plus Night Mercurian Elongation Spooky Sensation Great Martian Opposition Observing Notes: Aquila – The Eagle Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 27 September 2020 President’s Message Welcome to September. You may have noticed that this newsletter is showing up a little bit later than usual, and it’s for good reason: release of the newsletter will now happen after the monthly business meeting so that we can have a chance to keep everybody up to date on the latest information. Sometimes, this will mean the newsletter shows up a couple of days late. But, the upshot is that you’ll now be able to see what we discussed at the recent business meeting and have time to digest it before our general meeting in case you want to give some feedback. Now that we’re on the new format, business meetings (and the oft neglected Light Pollution Committee Meeting), are going to start being open to all members of the club again by simply joining up in the respective chat rooms the Wednesday before the first Monday of the month—which I encourage people to do, especially if you have some ideas you want to see the club put into action. -
Transiting Exoplanets from the Corot Space Mission. XI. Corot-8B: a Hot
Astronomy & Astrophysics manuscript no. corot-8b c ESO 2018 October 23, 2018 Transiting exoplanets from the CoRoT space mission XI. CoRoT-8b: a hot and dense sub-Saturn around a K1 dwarf? P. Borde´1, F. Bouchy2;3, M. Deleuil4, J. Cabrera5;6, L. Jorda4, C. Lovis7, S. Csizmadia5, S. Aigrain8, J. M. Almenara9;10, R. Alonso7, M. Auvergne11, A. Baglin11, P. Barge4, W. Benz12, A. S. Bonomo4, H. Bruntt11, L. Carone13, S. Carpano14, H. Deeg9;10, R. Dvorak15, A. Erikson5, S. Ferraz-Mello16, M. Fridlund14, D. Gandolfi14;17, J.-C. Gazzano4, M. Gillon18, E. Guenther17, T. Guillot19, P. Guterman4, A. Hatzes17, M. Havel19, G. Hebrard´ 2, H. Lammer20, A. Leger´ 1, M. Mayor7, T. Mazeh21, C. Moutou4, M. Patzold¨ 13, F. Pepe7, M. Ollivier1, D. Queloz7, H. Rauer5;22, D. Rouan11, B. Samuel1, A. Santerne4, J. Schneider6, B. Tingley9;10, S. Udry7, J. Weingrill20, and G. Wuchterl17 (Affiliations can be found after the references) Received ?; accepted ? ABSTRACT Aims. We report the discovery of CoRoT-8b, a dense small Saturn-class exoplanet that orbits a K1 dwarf in 6.2 days, and we derive its orbital parameters, mass, and radius. Methods. We analyzed two complementary data sets: the photometric transit curve of CoRoT-8b as measured by CoRoT and the radial velocity curve of CoRoT-8 as measured by the HARPS spectrometer??. Results. We find that CoRoT-8b is on a circular orbit with a semi-major axis of 0:063 ± 0:001 AU. It has a radius of 0:57 ± 0:02 RJ, a mass of −3 0:22 ± 0:03 MJ, and therefore a mean density of 1:6 ± 0:1 g cm . -
Transit Analysis of the Corot-5, Corot-8, Corot-12, Corot-18
MNRAS 483, 824–839 (2019) doi:10.1093/mnras/sty3085 Advance Access publication 2018 November 15 Transit analysis of the CoRoT-5, CoRoT-8, CoRoT-12, CoRoT-18, CoRoT-20, and CoRoT-27 systems with combined ground- and space-based photometry Downloaded from https://academic.oup.com/mnras/article-abstract/483/1/824/5184487 by Inst. Astrofisica Andalucia CSIC user on 28 August 2019 St. Raetz,1,2,3‹ A. M. Heras,3 M. Fernandez,´ 4 V. Casanova,4 and C. Marka5 1Institute for Astronomy and Astrophysics Tubingen¨ (IAAT), University of Tubingen,¨ Sand 1, D-72076 Tubingen,¨ Germany 2Freiburg Institute of Advanced Studies (FRIAS), University of Freiburg, Albertstraße 19, D-79104 Freiburg, Germany 3Science Support Office, Directorate of Science, European Space Research and Technology Centre (ESA/ESTEC), Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands 4Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Apdo. 3004, 18080 Granada, Spain 5Instituto Radioastronom´ıa Milimetrica´ (IRAM), Avenida Divina Pastora 7, E-18012 Granada, Spain Accepted 2018 November 8. Received 2018 November 7; in original form 2018 April 6 ABSTRACT We have initiated a dedicated project to follow-up with ground-based photometry the transiting planets discovered by CoRoT in order to refine the orbital elements, constrain their physical parameters, and search for additional bodies in the system. From 2012 September to 2016 December we carried out 16 transit observations of six CoRoT planets (CoRoT-5 b, CoRoT- 8 b, CoRoT-12 b, CoRoT-18 b, CoRoT-20 b, and CoRoT-27 b) at three observatories located in Germany and Spain. These observations took place between 5 and 9 yr after the planet’s discovery, which has allowed us to place stringent constraints on the planetary ephemeris. -
An Analysis of Noise in the Corot Data Aaron Sampson '
An Analysis of Noise in the CoRoT Data by Aaron Sampson Submitted to the Department of Physics in partial fulfillment of the requirements for the degree of Bachelor of Science in Physics at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY June 2010 © Massachusetts Institute of Technology 2010. All rights reserved. '/ Author............... ------- .- ..---...-v-----f ----- Department of Physics May 17, 2010 Certified by............ .... ..... ... ... .< . ... .. Sara Seager Associate Professor of Physics Thesis Supervisor Accepted by ................... ............... ................ Professor David E. Pritchard Senior Thesis Coordinator, Department of Physics OF TECHNOLOGY ARCHIVES AUG 13 2010 LIBRARIES 2 An Analysis of Noise in the CoRoT Data by Aaron Sampson Submitted to the Department of Physics on May 17, 2010, in partial fulfillment of the requirements for the degree of Bachelor of Science in Physics Abstract In this thesis, publically available data from the French/ESA satellite mission CoRoT, designed to seek out extrasolar planets, was analyzed using MATLAB. CoRoT at- tempts to observe the transits of these planets accross their parent stars. CoRoT occupies an orbit which periodically carries it through the Van Allen Belts, resulting in a a very high level of high outliers in the flux data. Known systematics and out- liers were removed from the data and the remaining scatter was evaluated using the median of abolute deviations from the median (MAD), a measure of scatter which is robust to outliers. The level of scatter (evaluated with MAD) present in this data is indicative of the lower limits on the size of planets detectable by CoRoT or a similar satellite. The MAD for CoRoT stars is correlated with the magnitude. -
Transiting Exoplanets from the Corot Space Mission XXIX
A&A 635, A122 (2020) Astronomy https://doi.org/10.1051/0004-6361/201732393 & © P. Bordé et al. 2020 Astrophysics Transiting exoplanets from the CoRoT space mission XXIX. The hot Jupiters CoRoT-30 b and CoRoT-31 b? P. Bordé1, R. F. Díaz2,3,4, O. Creevey5,6, C. Damiani6,7, H. Deeg10,11, P. Klagyivik10,11, G. Wuchterl29, D. Gandolfi8,9, M. Fridlund12,13,14, F. Bouchy2,16, S. Aigrain15, R. Alonso10,11, J.-M. Almenara2,16, A. Baglin17, S. C. C. Barros16,18, A. S. Bonomo19, J. Cabrera20, Sz. Csizmadia20, M. Deleuil16, A. Erikson20, S. Ferraz-Mello21, E. W. Guenther22, T. Guillot5, S. Grziwa23, A. Hatzes22, G. Hébrard24, T. Mazeh25, M. Ollivier6,17, H. Parviainen26, M. Pätzold23, H. Rauer20,27, D. Rouan17, A. Santerne16, and J. Schneider28 (Affiliations can be found after the references) Received 1 December 2017 / Accepted 1 September 2019 ABSTRACT Aims. We report the discovery as well as the orbital and physical characterizations of two new transiting giant exoplanets, CoRoT-30 b and CoRoT-31 b, with the CoRoT space telescope. Methods. We analyzed two complementary data sets: photometric transit light curves measured by CoRoT, and radial velocity curves measured by the HARPS spectrometer. To derive the absolute masses and radii of the planets, we modeled the stars from available magnitudes and spectra. Results. We find that CoRoT-30 b is a warm Jupiter on a close-to-circular 9.06-day orbit around a G3V star with a semi-major axis 3 of about 0.08 AU. It has a radius of 1:01 0:08 RJ, a mass of 2:90 0:22 MJ, and therefore a mean density of 3:45 0:65 g cm− . -
IRF Applied to the Transit of Corot Planets
Chapter 3 IRF applied to the transit of CoRoT planets In this chapter, the IRF is applied to the CoRoT light curves of the first seven planets and brown dwarf discovered by CoRoT. The phase folded transits of the IRF-filtered light curves are fitted to derive the planet parameters using a Levenberg-Marquardt algorithm and the analytical transit models of Mandel & Agol (2002). The results are compared to the parameters published in the planet/brown dwarf discovery papers. Some of the work presented in this chapter has been published: in Fridlund et al. (2010) for the work on CoRoT-6b and in Léger et al. (2009) for the work on CoRoT-7b. The IRF was used as an independent analysis of the transit light curves. The method was optimised further since these publications, especially in the understanding (strengths and limitations) of the IRF and of the techniques used to find the best model to the transit. 3.1 Description of the CoRoT data 3.1.1 Instrument CoRoT (Convection, Rotation and planetary Transits)1 is a modest scale mission (626 kg satellite, 80 million euros in cost) primarily funded by the French space agency CNES (Centre National d’Etude Spaciale), with contributions from ESA (European Space Agency), Belgium, Austria, Germany, Spain and Brazil. The satellite was launched on December 27th 2006 into a polar orbit at 900 km of altitude. ∼ CoRoT is the first space-based telescope designed for high precision photometry with long time coverage after MOST2 (150 days for the long runs and 20-30 days for the short runs, with duty cycle greater than 93%). -
Title Observations of Nova Aquilae No. 3 Author(S) Yamamoto, I.; Ueta, Y
Title Observations of Nova Aquilae No. 3 Author(s) Yamamoto, I.; Ueta, Y.; Kudara, K. Memoirs of the College of Science, Kyoto Imperial University Citation (1919), 4(1): 23-42 Issue Date 1919-09-15 URL http://hdl.handle.net/2433/256530 Right Type Departmental Bulletin Paper Textversion publisher Kyoto University Observations of Nova Aquilae No. 3. I. Yamamoto, Y. Ueta, and K. Kndara. (Received May 21, 1919) Introduction. The Nova Aquilae, No. 3, was found by the first two of the writers on the occasion of the Solar Eclipse Expedition at Torisima (St. Peter's Island) in the Northwest Pacific Ocean, at about zh Greenw. Mean Time on June rr, 1918. At that time, however, no suitable instrumental equipment being available only magnitude estimations, visually, were made, and that thru broken cloud. They returned to Kyoto a few days later, arriving there on June I 6, when they learnt that Mr. Kudara had also noticed the Nova and begun observations. Since then, a constant watch has been kept by us three. To our d~epest regret, the rainy season had already begun, so that we were very often troubled by meteorological irregularities. ( i ) Estimations of Magnitudes. Magnitudes were estimated usually by the method of interpolation, comparisons being made with neighbouring stars, and the Harvard system of scale adopted. Most of the reductions were made by Kudara. 1) I. Yamamoto's Estimations. Observations were made at Kyoto with the naked eye, unless otherwise stated, during the first half of the series; but, for the remaining period, more precisely, after August 3, the Observer made an excursion to the Kasumi-ga-ura Region, east of Tokyo for Gravity Measurements, during which the observations were made with a pair of binoculars, the names of daily stations will be found in the column of Remarks. -
Transiting Exoplanets: Characterisation in the Presence of Stellar Activity
—————————————————— Transiting exoplanets: characterisation in the presence of stellar activity Aude Ekundayo Pauline ALAPINI ODUNLADE —————————————————— Submitted by Mrs Aude Ekundayo Pauline Alapini Odunlade, to the University of Exeter as a thesis for the degree of Doctor of Philosophy in Physics, March 2010. This thesis is available for Library use on the understanding that it is copyright material and that no quo- tation from the thesis may be published without proper acknowledgement. I certify that all material in this thesis which is not my own work has been identified and that no material has previously been submitted and approved for the award of a degree by this or any other University. Mrs Aude E. P. Alapini Odunlade March 2010 This thesis was supervised by Dr. Suzanne Aigrain – University of Exeter, University of Oxford Abstract The combined observations of a planet’s transits and the radial velocity variations of its host star allow the determination of the planet’s orbital parameters, and most inter- estingly of its radius and mass, and hence its mean density. Observed densities provide important constraints to planet structure and evolution models. The uncertainties on the parameters of large exoplanets mainly arise from those on stellar masses and radii. For small exoplanets, the treatment of stellar variability limits the accuracy on the de- rived parameters. The goal of this PhD thesis was to reduce these sources of uncertainty by developing new techniques for stellar variability filtering and for the determination of stellar temperatures, and by robustly fitting the transits taking into account external constraints on the planet’s host star. -
The Corot Exoplanet Program for the Next 3 Years
EPSC Abstracts Vol. 7 EPSC2012-198-2 2012 European Planetary Science Congress 2012 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2012 The CoRoT Exoplanet Program for the next 3 years J. Cabrera on behalf of the CoRoT Scientific Committee (1) Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt, Rutherfordstr. 2, 12489 Berlin, Germany ([email protected]) Abstract ameter yields a photometric precision ten times higher than CoRoT and it is devoted to the search of small, The CoRoT mission is a space telescope devoted to the rocky planets in long orbits, with preference on those search and characterization of extrasolar planets and in the habitable zone. the study of stellar interiors via asteroseismology. The The observational strategy of CoRoT is determined nominal mission lifetime of 3 years was extended in by the choice of its orbit and therefore only two re- October 2010 until March 2013. Recently, the CoRoT gions of the sky, called the CoRoT Eyes [5], are within Scientific Comittee has submitted a proposal for a 3 reach. These regions are located towards the constella- year prolongation. We describe here the main goals of tions of Monoceros (winter observations) and Aquila the exoplanet program for the proposed CoRoT exten- (summer observations) and each one has a diameter of sion period 2013-2015. approximately 15 degrees. A second limitation of the orbit is the maximum duration of a continuous point- ing, which is of 150 days. 1 Introduction Therefore, CoRoT cannot observe as long as Kepler the same field and it cannot reach the same photomet- The asteroseismology of stellar interiors and the dis- ric precision as Kepler for stars of the same magnitude. -
REACH for the STARS, Division B DESCRIPTION: Students Will
REACH FOR THE STARS, Division B DESCRIPTION: Students will demonstrate an understanding of the properties and Evolution of stars and their observation with different portions of the electromagnetic Spectrum: Radio, Infrared, Visible, Ultraviolet, X-Ray and Gamma Ray. Part I: Constellation, Star, and Deep Sky Object (DSO) Identification Part II: i: Stellar Evolution stellar nurseries, protostars, main sequence stars, red giants, planetary nebulas, white dwarfs, red supergiants, type Ia supernovas, Type II supernovas, neutron stars black holes ii: Spectral Classification of Stars spectra and the H-R diagram iii: The Electromagnetic Spectrum multiwavelength observations iv: Stellar Temperatures, Radii, and Luminosities the H-R diagram, blackbody radiation Part I: Constellations, Stars, and DSO’s Aquila: Altair, CoRoT-2A, SS433 Hercules: M13 Aquarius: NGC 7293 Leo: Regulus Auriga: Capella Lyra: Vega, M57 Bootes: Arcturus Orion: Betelgeuse, Rigel, M42 Canis Major: Sirius Perseus: Algol Canis Minor: Procyon Sagittarius: Sag A*, M17, G359.23-0.82 Carina: Eta Carinae Scorpius: Antares Centaurus: Proxima Centauri Taurus: Aldebaran, HL Tau, M1, M45 Cassiopeia: Cas A, Tycho, NGC 281 Hyades Dorado: 30 Doradus Ursa Minor: Polaris Cygnus: Deneb, Cygnus X-1, Ursa Major: Mizar, Alcor, SN1993J NGC 7000 Vela: γ Velorum, Vela SNR Gemini: Castor, Pollux, Geminga Virgo: Spica Libra: Gliese 581 Aquila: Altair, CoRoT-2A (star with planet), SS433 (X-Ray Binary) Aquila: Altair, CoRoT-2A (star with planet), SS433 (X-Ray Binary) Aquarius: NGC 7293 (The Helix Nebula) -
Volume 5 Nos 1 and 2 December 2000 LONGINES' T--' Xjenza 2000; 5:1/2 1
Volume 5 Nos 1 and 2 December 2000 LONGINES' T--' Xjenza 2000; 5:1/2 1 Contents .- editorial Is There a Future for Xjenza? 2 Oficial Journal of the Mlrlm Chamber of research articles Nignments Along the Main Axes at Scientists Mnajdra Temples Chris Micalief Edilor Angela Xuereb Preliminary report on B-carotene production in the halotolerant microalga Associate Editon Dunaliella bardawil 16 Marlin Ebejcr Richard Muscat Zammit-Mangion Marion and Felice Alex Editaria1 Address Xjenza, The Newton-Leibniz Priority Dispute 20 C/o University of Malta, ct?=ticlt? Gwardamangia, Emmanuel Cardona 1Malm. ~0ntmentUry Reflections On The Coming Era of Tel: (+356) 25951882 Artificial Intelligence Rx: (456) 235638 Nicholas Sarnmut Typeset Anthony Sullana abstracts Biology Symposium Printers PEG. Ltd., news Science Fair - 6th to 8th ApriI 2000 San Gwann. instructions for authors Cover Picture: Pull nioon alignment at Mnaidra lowcr temple. (Phoio: Mr. ~auri&Mieallef). P.O. Box 45, Valletta B.P.O., Valletta, Malta. 02000 Molm Chamber of Scienrirfs Xjenza 2000; 5212 Editorial Is There a Future for Xjenza? This issue of Xjenza is a single issue for the year 2000. the other fully-fledged scientists? Where are the results It is not for the lack of sponsorship or funds, or an over- of their research on crucial local issues - on atmos- worked editorial board. There simply were insufficient pheric pollution, on marine pollution, on waste manage- contributions to justify more than one issue. In the main, ment? Why is it that we only read snippets about such the papers featured in this issue were the only ones sub- local research in newspapers - headlines to cater for the mitted to Xjenza during the year. -
Corot Pictures Transiting Exoplanets
CoRoT pictures transiting exoplanets Claire Moutou1;2 and Magali Deleuil2 1 Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Highway, Kamuela HI 96743, [email protected] 2 Laboratoire d’Astrophysique de Marseille, 38 rue Fr´ed´ericJoliot-Curie, 13376 Marseille cedex 13, France, [email protected] Abstract The detection and characterization of exoplanets have made huge progresses since the first discoveries in the late nineties. In particular, the independent measurement of the mass and radius of planets, by combining the transit and radial-velociy techniques, allowed exploring their density and hence, their internal structure. With CoRoT (2007- 2012), the pioneering CNES space-based mission in this investigation, about thirty new planets were characterized. CoRoT has enhanced the diversity of giant exoplanets and discovered the first telluric exoplanet. Following CoRoT, the NASA Kepler mission has extended our knowledge to small-size planets, multiple systems and planets orbit- ing binaries. Exploring these new worlds will continue with the NASA/TESS (2017) and ESA/PLATO (2024) missions. Keywords: Astrophysics - Space mission - Planetary systems - Observations - Internal structure of planets 1. Introduction The search for exoplanets around solar-type stars has started in the 1990’s with the direct imaging method and the radial velocity method. While the first one uses high-contrast and high-resolution imaging of nearby stars to search for the dim light of a sub-stellar companion, the second method uses indirect measurements of stars and searches for velocity wobbling due to the gravitational pull by an invisible planet. Both methods had their first results in 1995: the first detected brown dwarf companion Gl 229 B (about 50 Jupiter masses) by direct imaging [1] and the first detected Jupiter- arXiv:1510.01372v1 [astro-ph.EP] 5 Oct 2015 like exoplanet 51 Pegasi b, orbiting a solar-type star [2].