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Astronomers Find First Planet from Another Galaxy (W/ Video) 18 November 2010
Astronomers find first planet from another galaxy (w/ Video) 18 November 2010 even though the star now finds itself within our own galaxy. It is part of the so-called Helmi stream - a group of stars that originally belonged to a dwarf galaxy that was devoured by our galaxy, the Milky Way, in an act of galactic cannibalism about six to nine billion years ago. The results are published today in Science Express. "This discovery is very exciting," says Rainer Klement of the Max-Planck-Institut für Astronomie (MPIA), who was responsible for the selection of the target stars for this study. "For the first time, astronomers have detected a planetary system in a stellar stream of extragalactic origin. Because of the great distances involved, there are no This artist’s impression shows HIP 13044 b, an confirmed detections of planets in other galaxies. exoplanet orbiting a star that entered our galaxy, the But this cosmic merger has brought an Milky Way, from another galaxy. This planet of extragalactic planet within our reach." extragalactic origin was detected by a European team of astronomers using the MPG/ESO 2.2-metre telescope at The star is known as HIP 13044, and it lies about ESO’s La Silla Observatory in Chile. The Jupiter-like 2000 light-years from Earth in the southern planet is particularly unusual, as it is orbiting a star nearing the end of its life and could be about to be constellation of Fornax (the Furnace). The engulfed by it, giving clues about the fate of our own astronomers detected the planet, called HIP 13044 planetary system in the distant future. -
The Comet's Tale
THE COMET’S TALE Newsletter of the Comet Section of the British Astronomical Association Volume 5, No 1 (Issue 9), 1998 May A May Day in February! Comet Section Meeting, Institute of Astronomy, Cambridge, 1998 February 14 The day started early for me, or attention and there were displays to correct Guide Star magnitudes perhaps I should say the previous of the latest comet light curves in the same field. If you haven’t day finished late as I was up till and photographs of comet Hale- got access to this catalogue then nearly 3am. This wasn’t because Bopp taken by Michael Hendrie you can always give a field sketch the sky was clear or a Valentine’s and Glynn Marsh. showing the stars you have used Ball, but because I’d been reffing in the magnitude estimate and I an ice hockey match at The formal session started after will make the reduction. From Peterborough! Despite this I was lunch, and I opened the talks with these magnitude estimates I can at the IOA to welcome the first some comments on visual build up a light curve which arrivals and to get things set up observation. Detailed instructions shows the variation in activity for the day, which was more are given in the Section guide, so between different comets. Hale- reminiscent of May than here I concentrated on what is Bopp has demonstrated that February. The University now done with the observations and comets can stray up to a offers an undergraduate why it is important to be accurate magnitude from the mean curve, astronomy course and lectures are and objective when making them. -
The Comet's Tale
THE COMET’S TALE Journal of the Comet Section of the British Astronomical Association Number 33, 2014 January Not the Comet of the Century 2013 R1 (Lovejoy) imaged by Damian Peach on 2013 December 24 using 106mm F5. STL-11k. LRGB. L: 7x2mins. RGB: 1x2mins. Today’s images of bright binocular comets rival drawings of Great Comets of the nineteenth century. Rather predictably the expected comet of the century Contents failed to materialise, however several of the other comets mentioned in the last issue, together with the Comet Section contacts 2 additional surprise shown above, put on good From the Director 2 appearances. 2011 L4 (PanSTARRS), 2012 F6 From the Secretary 3 (Lemmon), 2012 S1 (ISON) and 2013 R1 (Lovejoy) all Tales from the past 5 th became brighter than 6 magnitude and 2P/Encke, 2012 RAS meeting report 6 K5 (LINEAR), 2012 L2 (LINEAR), 2012 T5 (Bressi), Comet Section meeting report 9 2012 V2 (LINEAR), 2012 X1 (LINEAR), and 2013 V3 SPA meeting - Rob McNaught 13 (Nevski) were all binocular objects. Whether 2014 will Professional tales 14 bring such riches remains to be seen, but three comets The Legacy of Comet Hunters 16 are predicted to come within binocular range and we Project Alcock update 21 can hope for some new discoveries. We should get Review of observations 23 some spectacular close-up images of 67P/Churyumov- Prospects for 2014 44 Gerasimenko from the Rosetta spacecraft. BAA COMET SECTION NEWSLETTER 2 THE COMET’S TALE Comet Section contacts Director: Jonathan Shanklin, 11 City Road, CAMBRIDGE. CB1 1DP England. Phone: (+44) (0)1223 571250 (H) or (+44) (0)1223 221482 (W) Fax: (+44) (0)1223 221279 (W) E-Mail: [email protected] or [email protected] WWW page : http://www.ast.cam.ac.uk/~jds/ Assistant Director (Observations): Guy Hurst, 16 Westminster Close, Kempshott Rise, BASINGSTOKE, Hampshire. -
Mètodes De Detecció I Anàlisi D'exoplanetes
MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits -
A Planet from Another Galaxy
Image courtesy of ESO / S Steinhöfel A planet from another galaxy As though planets from outside our Solar System were not exciting enough, astronomers have recently discovered a planet orbiting a star from outside our galaxy. Johny Setiawan reports. or two decades, astronomers Our research group at the Max Recently, our team have successfully have known that there are Planck Institute for Astronomy in detected a planet around the star HIP planets beyond our Solar Heidelberg, Germany, however, 13044, which has left the red giant FSystem (Wolszczan & Frail, 1992). concentrates on the search for plan- phase. Orbiting other stars, they are known etary companions around stars that as extrasolar planets or exoplanets. are not in the main-sequence phase, An extragalactic star So far, more than 500 exoplanets have but in later evolutionary stages. These The star HIP 13044, which is about been detected, the majority of which include what is known as the red giant 2000 light years away from our Solar orbit stars with characteristics similar phase, during which the star expands System in the southern constellation to those of the Sun (as described in to hundreds of times its original diam- of Fornax (‘the furnace’), is signifi- Jørgensen, 2006). In particular, more eter. The detection of planets around cantly different from other known than 90% of the stars hosting exoplan- such giant stars is important for the stars with planets. In particular, it has ets are in the same evolutionary phase study of the evolution of planetary a very low abundance of the metal as the Sun – the main-sequence phase, systems. -
Investigating the Neutral Sodium Emissions Observed at Comets
Investigating the neutral sodium emissions observed at comets K. S. Birkett M.Sci. Physics, Imperial College London, UK (2012) Department of Space and Climate Physics University College London Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey. RH5 6NT. United Kingdom THESIS Submitted for the degree of Doctor of Philosophy, University College London 2017 2 I, Kimberley Si^anBirkett, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. 3 Abstract Neutral sodium emission is typically very easy to detect in comets, and has been seen to form a distinct neutral sodium tail at some comets. If the source of neutral cometary sodium could be determined, it would shed light on the composition of the comet, therefore allowing deeper understanding of the conditions present in the early solar system. Detection of neutral sodium emission at other solar system objects has also been used to infer chemical and physical processes that are difficult to measure directly. Neutral cometary sodium tails were first studied in depth at comet Hale-Bopp, but to date the source of neutral sodium in comets has not been determined. Many authors considered that orbital motion may be a significant factor in conclusively identifying the source of neutral sodium, so in this work details of the development of the first fully heliocentric distance and velocity dependent orbital model, known as COMPASS, are presented. COMPASS is then applied to a range of neutral sodium observations, includ- ing spectroscopic measurements at comet Hale-Bopp, wide field images of comet Hale- Bopp, and SOHO/LASCO observations of neutral sodium tails at near-Sun comets. -
Post-Main-Sequence Planetary System Evolution Rsos.Royalsocietypublishing.Org Dimitri Veras
Post-main-sequence planetary system evolution rsos.royalsocietypublishing.org Dimitri Veras Department of Physics, University of Warwick, Coventry CV4 7AL, UK Review The fates of planetary systems provide unassailable insights Cite this article: Veras D. 2016 into their formation and represent rich cross-disciplinary Post-main-sequence planetary system dynamical laboratories. Mounting observations of post-main- evolution. R. Soc. open sci. 3: 150571. sequence planetary systems necessitate a complementary level http://dx.doi.org/10.1098/rsos.150571 of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the Received: 23 October 2015 interpretation and modelling of currently known systems and Accepted: 20 January 2016 upcoming discoveries. 1. Introduction Subject Category: Decades of unsuccessful attempts to find planets around other Astronomy Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around Subject Areas: the millisecond pulsar PSR B1257+12 were the first confidently extrasolar planets/astrophysics/solar system reported extrasolar planets to withstand enduring scrutiny due to their well-constrained masses and orbits. However, a retrospective Keywords: historical analysis reveals even more surprises. We now know that dynamics, white dwarfs, giant branch stars, the eponymous celestial body that Adriaan van Maanen observed pulsars, asteroids, formation in the late 1910s [3,4]isanisolatedwhitedwarf(WD)witha metal-enriched atmosphere: direct evidence for the accretion of planetary remnants. These pioneering discoveries of planetary material around Author for correspondence: or in post-main-sequence (post-MS) stars, although exciting, Dimitri Veras represented a poor harbinger for how the field of exoplanetary e-mail: [email protected] science has since matured. -
The Agb Newsletter
THE AGB NEWSLETTER An electronic publication dedicated to Asymptotic Giant Branch stars and related phenomena Official publication of the IAU Working Group on Abundances in Red Giants No. 167 — 1 June 2011 http://www.astro.keele.ac.uk/AGBnews Editors: Jacco van Loon and Albert Zijlstra Editorial Dear Colleagues, It is a pleasure to present you the 167th issue of the AGB Newsletter. As always, it is full of informative and inspiring new results. Looking for a postdoctoral researcher position? There’s one in Tenerife! The next issue is planned to be distributed (hopefully) in early July 2011. Editorially Yours, Jacco van Loon and Albert Zijlstra Food for Thought This month’s thought-provoking statement is: Is there a place for solid hydrogen in circumstellar envelopes? Reactions to this statement or suggestions for next month’s statement can be e-mailed to [email protected] (please state whether you wish to remain anonymous) 1 Refereed Journal Papers The oxygen abundance in the Solar Neighborhood M´onica Rodr´ıguez1 and Gloria Delgado-Inglada1 1INAOE, M´exico We present a homogeneous analysis of the oxygen abundance in five H ii regions and eight planetary nebulae (PNe) located at distances lower than 2 kpc and with available spectra of high quality. We find that both the collisionally excited lines and recombination lines imply that the PNe are overabundant in oxygen by about 0.2 dex. An explanation that reconciles the oxygen abundances derived with collisionally excited lines for H ii regions and PNe with the values found for B-stars, the Sun, and the diffuse ISM requires the presence in H ii regions of an organic refractory dust component that is not present in PNe. -
No Evidence of the Planet Orbiting the Extremely Metal-Poor Extragalactic Star HIP 13044
A&A 562, A129 (2014) Astronomy DOI: 10.1051/0004-6361/201322132 & c ESO 2014 Astrophysics No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044 M. I. Jones1,2 and J. S. Jenkins2 1 Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile e-mail: [email protected] 2 Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Casilla 36-D Santiago, Chile Received 25 June 2013 / Accepted 25 August 2013 ABSTRACT Context. The recent discovery of three giant planets orbiting the extremely metal-poor stars HIP 11952 and HIP 13044 have chal- lenged theoretical predictions of the core-accretion model. According to this, the metal content of the protoplanetary disk from which giant planets are formed is a key ingredient for the early formation of planetesimals prior to the runaway accretion of the surrounding gas. Aims. We reanalyzed the original FEROS data that were used to detect the planets to prove or refute their existence, employing our new reduction and analysis methods. Methods. We applied the cross-correlation technique to FEROS spectra to measure the radial velocity variation of HIP 13044 and HIP 11952. We reached a typical precision of ∼35 m s−1 for HIP 13044 and ∼25 m s−1 for HIP 11952, which is significantly superior to the uncertainties presented previously. Results. We found no evidence of the planet orbiting the metal-poor extragalactic star HIP 13044. We show that given our radial ve- locity precision, and considering the large number of radial velocity epochs, the probability for a non-detection of the radial velocity signal recently claimed is lower than 10−4. -
Comet Kohoutek (NASA 990 Convair )
Madrid, UCM, Oct 27, 2017 Comets in UV Shustov B., Sachkov M., Savanov I. Comets – major part of minor body population of the Solar System There are a lot of comets in the Solar System. (Oort cloud contains cometary 4 bodies which total mass is ~ 5 ME , ~10 higher than mass of the Main Asteroid Belt). Comets keep dynamical, mineralogical, chemical, and structural information that is critically important for understanding origin and early evolution of the Solar System. Comets are considered as important objects in the aspect of space threats and resources. Comets are intrinsically different from one another (A’Hearn+1995). 2 General comments on UV observations of comets Observations in the UV range are very informative, because this range contains the majority of аstrophysically significant resonance lines of atoms (OI, CI, HI, etc.), molecules (CO, CO2, OH etc.), and their ions. UV background is relatively low. UV imaging and spectroscopy are both widely used. In order to solve most of the problems, the UV data needs to be complemented observations in other ranges including ground-based observations. 3 First UV observations of comets from space Instruments Feeding Resolu Spectral range Comets Found optics tion Orbiting Astronomical 4x200mm ~10 Å 1100-2000 Å Bennett OH (1657 Å) Observatory (OAO-2) ~20 Å 2000-4000 Å С/1969 Y1 OI (1304 Å) 2 scanning spectrophotometers Launched in 1968 Orbiting Geophysical ~100cm2 Bennett Lyman-α Observatory (OGO-5) С/1969 Y1 halo Launched in 1968 Aerobee sounding D=50mm ~1 Å 1100-1800 Å Tago- Lyman-α halo rocket Sato- wide-angle all-reflective Kosaka spectrograph С/1969 Y1 Launched in 1970 Skylab 3 space station D=75mm Kohoutek Huge Lyman- Launched in 1973 С/1969 Y1 α halo NASA 990 Convair D=300mm Kohoutek OH (3090Å) aircraft. -
SMCAS Events Continue Virtually …
The SAN MATEO COUNTY ASTRONOMICAL SOCIETY Sept. – Dec. • 2020 Issue 669th General Meeting: September 19 770th General Meeting: October 24 771st General Meeting: November 21 772nd General Meeting: December 19 Founded in 1960, the San Mateo County Astronomical Society is a 501(c)(3) non-profit organiza- SMCAS Events Continue tion for amateur astronomers and interested members of the Virtually … public. Visitors may attend Society meetings and lectures on the first Friday of each month, September to June, and Star Parties two Saturdays a month. All events are free for visitors and guests. Family memberships are offered at a nominal annual cost. Detailed membership information is found at http://www.smcasas- tro.com/membership.html where those who want can join via PayPal. Membership also includes access to our Event Horizon newsletter, discounted costs and subscriptions to calendars and magazines, monthly star parties of the Society and the College of San Mateo, use of loaner telescopes, field trips, social occasions and general meetings presenting guest speakers and programs. For additional information, please email us at [email protected] or call (650) See page 3 or page 5 for more details 678-2762. Membership forms are available NOTE: CSM is closed due to the pandemic. SMCAS near the end of this newsletter events are online until further notice. beginning on page 17. 1 Table of Contents From the Prez (President’s Corner)............................................................................ 3 Upcoming Events ....................................................................................................... 5 SMCAS Presentations Now in Conjunction with Star Parties................................... 5 CalStar 2020 ● September 17 to 20 ● Lake San Antonio Park ................................. 6 Solar System Rise and Set Times.............................................................................. -
A Model of the Physical Properties of Comet Encke
https://ntrs.nasa.gov/search.jsp?R=19730024004 2020-03-23T01:27:56+00:00Z NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Technical Report 32-1590 A Model of the Physical Properties of Comet Encke F. W, Taylor C. M. Michaux R, L Newburn, Jr. Hm 3- £r" JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY PASADENA, CALIFORNIA October 1, 1973 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Technical Report 32-1590 A Model of the Physical Properties of Comet Encke F. W. Taylor C. M. Michaux R. L. Newburn, Jr. JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY PASADENA, CALIFORNIA October 1, 1973 Preface The work described in this report was performed by the Space Sciences Division of the Jet Propulsion Laboratory. Comet Encke is presently regarded as the likely target of NASA's first cometary mission, probably a slow flyby projected to take place in 1980. This document presents a model of Encke which is intended to be useful for the design of scientific experiments and spacecraft systems for such a mission. Data on the physical properties of comets are generally very sparse, and Encke is no exception. Much of the numerical information contained herein is, there- fore, based on calculations of a highly conjectural nature, and the results have large uncertainties associated with 'them. The user is cautioned that this is a model and not a specification, and must be treated as such if it is to be useful. The starting point for this work was an earlier study of Encke (Ref. 9) prepared by the TRW Systems Group under contract to JPL.