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Evidence for Very Extended Gaseous Layers Around O-Rich Mira Variables and M Giants B
The Astrophysical Journal, 579:446–454, 2002 November 1 # 2002. The American Astronomical Society. All rights reserved. Printed in U.S.A. EVIDENCE FOR VERY EXTENDED GASEOUS LAYERS AROUND O-RICH MIRA VARIABLES AND M GIANTS B. Mennesson,1 G. Perrin,2 G. Chagnon,2 V. Coude du Foresto,2 S. Ridgway,3 A. Merand,2 P. Salome,2 P. Borde,2 W. Cotton,4 S. Morel,5 P. Kervella,5 W. Traub,6 and M. Lacasse6 Received 2002 March 15; accepted 2002 July 3 ABSTRACT Nine bright O-rich Mira stars and five semiregular variable cool M giants have been observed with the Infrared and Optical Telescope Array (IOTA) interferometer in both K0 (2.15 lm) and L0 (3.8 lm) broad- band filters, in most cases at very close variability phases. All of the sample Mira stars and four of the semire- gular M giants show strong increases, from ’20% to ’100%, in measured uniform-disk (UD) diameters between the K0 and L0 bands. (A selection of hotter M stars does not show such a large increase.) There is no evidence that K0 and L0 broadband visibility measurements should be dominated by strong molecular bands, and cool expanding dust shells already detected around some of these objects are also found to be poor candi- dates for producing these large apparent diameter increases. Therefore, we propose that this must be a con- tinuum or pseudocontinuum opacity effect. Such an apparent enlargement can be reproduced using a simple two-component model consisting of a warm (1500–2000 K), extended (up to ’3 stellar radii), optically thin ( ’ 0:5) layer located above the classical photosphere. -
Transit of Venus Presentation
http://sunearthday.nasa.gov/2012/transit/webcast.php Venus visible Venus with the unaided eye: "morning star" or the Earth "evening star. • Similar to Earth: – diameter: 12,103 km – 0.95 Earth’s – mass 0.89 of Earth's – few craters -- young surface – densities, chemical compositions are similar • rotation unusually slow (Venus day = 243 Earth days -- longer than Venus' year) • rotation retrograde • periods of Venus' rotation and of its orbit are synchronized -- always same face toward Earth when the two planets are at their closest approach • greenhouse effect -- surface temperature hot enough to melt lead M ikhail Lomonosov, june 5, 1761 discovered, during a transit, that V enus has an atmosphere The atmosphere is is composed mostly of carbon dioxide. There are several layers of clouds, many kilometers thick, composed of sulfuric acid. Mariner 10 Image of Venus V enera 13 Venus’ orbit is inclined (by 3.39 degrees) relative to the ecliptic If in the same plane we would have 5 transits in 8 years Venus: 13 years , Earth: 8 years Each time Earth completes 1.6 orbits, Venus catches up to it after 2.6 of its orbits Progress of the 2004 Transit of Venus pictured from NASA's Soho solar observatory. Credit: NASA Ascending (A) or Duration since last transit Date of transit Descending (D) node (years and months) 6 December 1631 A 4 December 1639 A 8 yrs 6 June 1761 D 121 yrs 6 months 3 June 1769 D 8 yrs 9 December 1874 A 105 yrs 6 months 6 December 1882 A 8 yrs 8 June 2004 D 121 yrs 6 months 5 June 2012 D 8 yrs 11 December 2117 A 105 yrs 6 months 8 December 2125 A 8 yrs In 6000 years 81 transits only Venus’ Role in History Copernican System vs Ptolemaic System http://astro.unl.edu/classaction/animations/renaissance/venusphases.html Venus’ Role in History Size of the Solar System - Revealed! • Kepler predicted the transit of December 1631 (though not observed!) and 120 year cycle. -
1 0929 Rioja Dodson__Precise Radio Astrometry.Pdf
Astron Astrophys Rev (2020)28:6 https://doi.org/10.1007/s00159-020-00126-z(0123456789().,-volV)(0123456789().,-volV) REVIEW ARTICLE Precise radio astrometry and new developments for the next generation of instruments 1,2,3 2 Marı´a J. Rioja • Richard Dodson Received: 9 January 2020 / Accepted: 17 June 2020 Ó Springer-Verlag GmbH Germany, part of Springer Nature 2020 Abstract We present a technique-led review of the progression of precise radio astrometry, from the first demonstrations, half a century ago, until to date and into the future. We cover the developments that have been fundamental to allow high accuracy and precision astrometry to be regularly achieved. We review the opportunities provided by the next generation of instruments coming online, which are primarily: SKA, ngVLA, and pathfinders, along with EHT and other (sub)mm-wavelength arrays, Space-VLBI, Geodetic arrays, and optical astrometry from GAIA. From the his- torical development, we predict the future potential astrometric performance, and, therefore, the instrumental requirements that must be provided to deliver these. The next generation of methods will allow ultra-precise astrometry to be performed at a much wider range of frequencies (hundreds of MHz to hundreds of GHz). One of the key potentials is that astrometry will become generally applicable, and, there- fore, unbiased large surveys can be performed. The next-generation methods are fundamental in allowing this. We review the small but growing number of major astrometric surveys in the radio, to highlight the scientific impact that such projects can provide. Based on these perspectives, the future of radio astrometry is bright. -
Astrometrically Registered Maps of H2O and Sio Masers Toward VX Sagittarii
ARTICLE DOI: 10.1038/s41467-018-04767-8 OPEN Astrometrically registered maps of H2O and SiO masers toward VX Sagittarii Dong-Hwan Yoon1,2, Se-Hyung Cho2,3, Youngjoo Yun2, Yoon Kyung Choi2, Richard Dodson4, María Rioja4,5, Jaeheon Kim6, Hiroshi Imai7, Dongjin Kim3, Haneul Yang1,2 & Do-Young Byun2 The supergiant VX Sagittarii is a strong emitter of both H2O and SiO masers. However, previous VLBI observations have been performed separately, which makes it difficult to 1234567890():,; spatially trace the outward transfer of the material consecutively. Here we present the astrometrically registered, simultaneous maps of 22.2 GHz H2O and 43.1/42.8/86.2/129.3 GHz SiO masers toward VX Sagittarii. The H2O masers detected above the dust-forming layers have an asymmetric distribution. The multi-transition SiO masers are nearly circular ring, suggesting spherically symmetric wind within a few stellar radii. These results provide the clear evidence that the asymmetry in the outflow is enhanced after the smaller molecular gas clump transform into the inhomogeneous dust layers. The 129.3 GHz maser arises from the outermost region compared to that of 43.1/42.8/86.2 GHz SiO masers. The ring size of the 129.3 GHz maser is maximized around the optical maximum, suggesting that radiative pumping is dominant. 1 Astronomy Program, Department of Physics and Astronomy, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Korea. 2 Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Korea. 3 Department of Astronomy, Yonsei University, 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Korea. -
Transit of Venus M
National Aeronautics and Space Administration The Transit of Venus June 5/6, 2012 HD209458b (HST) The Transit of Venus June 5/6, 2012 Transit of Venus Mathof Venus Transit Top Row – Left image - Photo taken at the US Naval Math Puzzler 3 - The duration of the transit depends Observatory of the 1882 transit of Venus. Middle on the relative speeds between the fast-moving image - The cover of Harpers Weekly for 1882 Venus in its orbit and the slower-moving Earth in its showing children watching the transit of Venus. orbit. This speed difference is known to be 5.24 km/sec. If the June 5, 2012, transit lasts 24,000 Right image – Image from NASA's TRACE satellite seconds, during which time the planet moves an of the transit of Venus, June 8, 2004. angular distance of 0.17 degrees across the sun as Middle - Geometric sketches of the transit of Venus viewed from Earth, what distance between Earth and by James Ferguson on June 6, 1761 showing the Venus allows the distance traveled by Venus along its shift in the transit chords depending on the orbit to subtend the observed angle? observer's location on Earth. The parallax angle is related to the distance between Earth and Venus. Determining the Astronomical Unit Bottom – Left image - NOAA GOES-12 satellite x-ray image showing the Transit of Venus 2004. Middle Based on the calculations of Nicolas Copernicus and image – An observer of the 2004 transit of Venus Johannes Kepler, the distances of the known planets wearing NASA’s Sun-Earth Day solar glasses for from the sun could be given rather precisely in terms safe viewing. -
This Is an Electronic Reprint of the Original Article. This Reprint May Differ from the Original in Pagination and Typographic Detail
This is an electronic reprint of the original article. This reprint may differ from the original in pagination and typographic detail. Author(s): Sterken, Christiaan; Aspaas, Per Pippin; Dunér, David; Kontler, László; Neul, Reinhard; Pekonen, Osmo; Posch, Thomas Title: A voyage to Vardø - A scientific account of an unscientific expedition Year: 2013 Version: Please cite the original version: Sterken, C., Aspaas, P. P., Dunér, D., Kontler, L., Neul, R., Pekonen, O., & Posch, T. (2013). A voyage to Vardø - A scientific account of an unscientific expedition. The Journal of Astronomical Data, 19(1), 203-232. http://www.vub.ac.be/STER/JAD/JAD19/jad19.htm All material supplied via JYX is protected by copyright and other intellectual property rights, and duplication or sale of all or part of any of the repository collections is not permitted, except that material may be duplicated by you for your research use or educational purposes in electronic or print form. You must obtain permission for any other use. Electronic or print copies may not be offered, whether for sale or otherwise to anyone who is not an authorised user. MEETING VENUS C. Sterken, P. P. Aspaas (Eds.) The Journal of Astronomical Data 19, 1, 2013 A Voyage to Vardø. A Scientific Account of an Unscientific Expedition Christiaan Sterken1, Per Pippin Aspaas,2 David Dun´er,3,4 L´aszl´oKontler,5 Reinhard Neul,6 Osmo Pekonen,7 and Thomas Posch8 1Vrije Universiteit Brussel, Brussels, Belgium 2University of Tromsø, Norway 3History of Science and Ideas, Lund University, Sweden 4Centre for Cognitive Semiotics, Lund University, Sweden 5Central European University, Budapest, Hungary 6Robert Bosch GmbH, Stuttgart, Germany 7University of Jyv¨askyl¨a, Finland 8Institut f¨ur Astronomie, University of Vienna, Austria Abstract. -
Newsletter 75 – October 2011
COMMISSION 46 ASTRONOMY EDUCATION AND DEVELOPMENT Education et Développement de l’Astronomie Newsletter 75 – October 2011 Commission 46 seeks to further the development and improvement of astronomical education at all levels throughout the world. ___________________________________________________________________________ Contributions to this newsletter are gratefully received at any time. PLEASE WOULD NATIONAL LIAISONS DISTRIBUTE THIS NEWSLETTER IN THEIR COUNTRIES This newsletter is available at the following website http://astronomyeducation.org (this is a more memorable URL for the IAU C46 website than www.iaucomm46.org, to which the new URL links) and also at http://physics.open.ac.uk/~bwjones/IAU46/ IAU C46 NL75 October 2011 B W Jones 1 of 23 30/10/11 10:12 BST CONTENTS Editorial The Editor is to retire Message from the President The forthcoming transit of Venus DVD for teaching basic astronomy Vinnitsa planetarium Space scoop Virtual experiments Latin-American Journal of Astronomy Education (RELEA) Netware for astronomy school education (NASE) From Hans Haubold at the UN Book reviews The sky’s dark labyrinth Atlas of astronomical discoveries News of meetings and of people Cosmic rays SpS17: light pollution Useful websites for information on astronomy education and outreach meetings Information that will be found on the IAU C46 website Organizing Committee of Commission 46 Program Group Chairs and Vice Chairs IAU C46 NL75 October 2011 B W Jones 2 of 23 30/10/11 10:12 BST EDITORIAL Thanks to everyone who has made a contribution to this edition of the Newsletter. Please note the text in this Editorial highlighted in RED. For the March 2012 issue the copy date is Friday 16 March 2012. -
TRACE Observations of the 15 November 1999 Transit of Mercury and the Black Drop Effect: Considerations for the 2004 Transit of Venus
Icarus 168 (2004) 249–256 www.elsevier.com/locate/icarus TRACE observations of the 15 November 1999 transit of Mercury and the Black Drop effect: considerations for the 2004 transit of Venus Glenn Schneider,a,∗ Jay M. Pasachoff,b and Leon Golub c a Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA b Williams College—Hopkins Observatory, Williamstown, MA 01267, USA c Smithsonian Astrophysical Observatory, Mail Stop 58, 60 Garden Street, Cambridge, MA 02138, USA Received 15 May 2003; revised 14 October 2003 Abstract Historically, the visual manifestation of the “Black Drop effect,” the appearance of a band linking the solar limb to the disk of a transiting planet near the point of internal tangency, had limited the accuracy of the determination of the Astronomical Unit and the scale of the Solar System in the 18th and 19th centuries. This problem was misunderstood in the case of Venus during its rare transits due to the presence of its atmosphere. We report on observations of the 15 November 1999 transit of Mercury obtained, without the degrading effects of the Earth’s atmosphere, with the Transition Region and Coronal Explorer spacecraft. In spite of the telescope’s location beyond the Earth’s atmosphere, and the absence of a significant mercurian atmosphere, a faint Black Drop effect was detected. After calibration and removal of, or compensation for, both internal and external systematic effects, the only radially directed brightness anisotropies found resulted from the convolution of the instrumental point-spread function with the solar limb-darkened, back-lit, illumination function. -
Étude De L'atmosphère De Vénus À L'aide D'un Modèle De Réfraction Lors
Étude de l’atmosphère de Vénus à l’aide d’un modèle de réfraction lors du passage devant le Soleil des 5-6 Juin 2012 Christophe Pere To cite this version: Christophe Pere. Étude de l’atmosphère de Vénus à l’aide d’un modèle de réfraction lors du pas- sage devant le Soleil des 5-6 Juin 2012. Autre. Université Côte d’Azur, 2016. Français. NNT : 2016AZUR4063. tel-01477867 HAL Id: tel-01477867 https://tel.archives-ouvertes.fr/tel-01477867 Submitted on 27 Feb 2017 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. UNIVERSITE´ NICE SOPHIA ANTIPOLIS - UFR Sciences E´cole doctorale no 364 : Sciences Fondamentales et Appliqu´e es THE`SE pour obtenir le titre de Docteur en Sciences de l’UNIVERSITE´ Nice Sophia Antipolis Sp´ecialit´e: “SCIENCES DE LA PLANETE` ET DE L’UNIVERS” pr´esent´eeet soutenue publiquement par Christophe PERE Etude´ de l’atmosph`ere de V´enus `al’aide d’un mod`ele de r´efraction lors du passage devant le Soleil du 5-6 Juin 2012 Directeur de th`ese : Paolo TANGA Co-directeur de th`ese : Thomas WIDEMANN le 23 septembre 2016 Jury M. -
Quantization of Planetary Systems and Its Dependency on Stellar Rotation Jean-Paul A
Quantization of Planetary Systems and its Dependency on Stellar Rotation Jean-Paul A. Zoghbi∗ ABSTRACT With the discovery of now more than 500 exoplanets, we present a statistical analysis of the planetary orbital periods and their relationship to the rotation periods of their parent stars. We test whether the structure of planetary orbits, i.e. planetary angular momentum and orbital periods are ‘quantized’ in integer or half-integer multiples with respect to the parent stars’ rotation period. The Solar System is first shown to exhibit quantized planetary orbits that correlate with the Sun’s rotation period. The analysis is then expanded over 443 exoplanets to statistically validate this quantization and its association with stellar rotation. The results imply that the exoplanetary orbital periods are highly correlated with the parent star’s rotation periods and follow a discrete half-integer relationship with orbital ranks n=0.5, 1.0, 1.5, 2.0, 2.5, etc. The probability of obtaining these results by pure chance is p<0.024. We discuss various mechanisms that could justify this planetary quantization, such as the hybrid gravitational instability models of planet formation, along with possible physical mechanisms such as inner discs magnetospheric truncation, tidal dissipation, and resonance trapping. In conclusion, we statistically demonstrate that a quantized orbital structure should emerge naturally from the formation processes of planetary systems and that this orbital quantization is highly dependent on the parent stars rotation periods. Key words: planetary systems: formation – star: rotation – solar system: formation 1. INTRODUCTION The discovery of now more than 500 exoplanets has provided the opportunity to study the various properties of planetary systems and has considerably advanced our understanding of planetary formation processes. -
1709.07167.Pdf
Publication Year 2017 Acceptance in OA@INAF 2020-11-24T18:03:22Z Title The science case for simultaneous mm-wavelength receivers in radio astronomy Authors Dodson, Richard; Rioja, María J.; Jung, Taehyun; Goméz, José L.; Bujarrabal, Valentin; et al. DOI 10.1016/j.newar.2017.09.003 Handle http://hdl.handle.net/20.500.12386/28522 Journal NEW ASTRONOMY REVIEWS Number 79 The Science Case for Simultaneous mm-Wavelength Receivers in Radio Astronomy Richard Dodsona, Mar´ıaJ. Riojaa,b,c, Taehyun Jungd,e, Jos´eLuis Gom´ezf, Valentin Bujarrabalc, Luca Moscadillig, James C. A. Miller-Jonesh, Alexandra J. Tetarenkoi, Gregory R. Sivakoffi aInternational Centre for Radio Astronomy Research, The University of Western Australia, 35 Stirling Hwy, Western Australia bCSIRO Astronomy and Space Science, 26 Dick Perry Avenue, Kensington WA 6151, Australia cObservatorio Astron´omicoNacional (IGN), Alfonso XII, 3 y 5, 28014 Madrid, Spain dKorea Astronomy and Space Science Institute 776, Daedeokdae-ro, Yuseong-gu, Daejeon, 34055, Republic of Korea eUniversity of Science and Technology, 217, Gajeong-ro, Yuseong-gu, Daejeon, 34113, Korea fInstituto de Astrof´ısicade Andaluc´ıa-CSIC,Glorieta de la Astronom´ıas/n, E-18008 Granada, Spain gINAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy hInternational Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth, WA 6845, Australia iDepartment of Physics, CCIS 4-183, University of Alberta, Edmonton, AB T6G 2E1, Canada Abstract This review arose from the European Radio Astronomy Technical Forum (ERATec) meeting held in Firenze, October 2015, and aims to highlight the breadth and depth of the high-impact science that will be aided and assisted by the use of simultaneous mm-wavelength receivers. -
Session 2 Presentations
Mercury: From Mariner to MESSENGER Sean C. Solomon Lamont-Doherty Earth Observatory Columbia University LPI 50th Anniversary Science Symposium 17 March 2018 40th LPSC The Woodlands, Texas 25 March 2009 Mariner 10 (1973–1975) • Mariner 10 – the last in the Mariner series – was the first spacecraft to visit Mercury. • Launched in November 1973, Mariner 10 flew by Mercury three times, in March and September 1974 and March 1975. Mariner 10 backup spacecraft, Udvar-Hazy Center. Mariner 10 and Mercury’s Magnetic Field • Mariner 10’s first flyby detected a magnetic field near Mercury. • Mariner 10’s third flyby (at high latitude on Mercury’s night side) confirmed that the field is internal. • A dipole field could fit the data, but there were large uncertainties. Mariner 10 third flyby observations of Mercury’s magnetic field [Connerney and Ness, 1988]. Mariner 10 and Mercury’s Geology • Mariner 10 imaged about 45% of Mercury’s surface. • Heavily cratered terrain was thought to be comparable in age to the lunar highlands. • Smooth plains were seen to be less cratered and younger, but unlike the lunar maria are not darker than the surrounding highlands. Mariner 10 mosaic of the Caloris basin. LPI Topical Conference (1976) • LPI convened a topical conference on Comparisons of Mercury and the Moon in November 1976. • A number of the papers given at the conference were collected into a special issue of Physics of the Earth and Planetary Interiors (1977). Mercury’s Exosphere • Mariner 10 had detected H and He in Mercury’s exosphere and set an upper bound on O.