Charles Augustus Young
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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. -
FIXED STARS a SOLAR WRITER REPORT for Churchill Winston WRITTEN by DIANA K ROSENBERG Page 2
FIXED STARS A SOLAR WRITER REPORT for Churchill Winston WRITTEN BY DIANA K ROSENBERG Page 2 Prepared by Cafe Astrology cafeastrology.com Page 23 Churchill Winston Natal Chart Nov 30 1874 1:30 am GMT +0:00 Blenhein Castle 51°N48' 001°W22' 29°‚ 53' Tropical ƒ Placidus 02' 23° „ Ý 06° 46' Á ¿ 21° 15° Ý 06' „ 25' 23° 13' Œ À ¶29° Œ 28° … „ Ü É Ü 06° 36' 26' 25° 43' Œ 51'Ü áá Œ 29° ’ 29° “ àà … ‘ à ‹ – 55' á á 55' á †32' 16° 34' ¼ † 23° 51'Œ 23° ½ † 06' 25° “ ’ † Ê ’ ‹ 43' 35' 35' 06° ‡ Š 17° 43' Œ 09° º ˆ 01' 01' 07° ˆ ‰ ¾ 23° 22° 08° 02' ‡ ¸ Š 46' » Ï 06° 29°ˆ 53' ‰ Page 234 Astrological Summary Chart Point Positions: Churchill Winston Planet Sign Position House Comment The Moon Leo 29°Le36' 11th The Sun Sagittarius 7°Sg43' 3rd Mercury Scorpio 17°Sc35' 2nd Venus Sagittarius 22°Sg01' 3rd Mars Libra 16°Li32' 1st Jupiter Libra 23°Li34' 1st Saturn Aquarius 9°Aq35' 5th Uranus Leo 15°Le13' 11th Neptune Aries 28°Ar26' 8th Pluto Taurus 21°Ta25' 8th The North Node Aries 25°Ar51' 8th The South Node Libra 25°Li51' 2nd The Ascendant Virgo 29°Vi55' 1st The Midheaven Gemini 29°Ge53' 10th The Part of Fortune Capricorn 8°Cp01' 4th Chart Point Aspects Planet Aspect Planet Orb App/Sep The Moon Semisquare Mars 1°56' Applying The Moon Trine Neptune 1°10' Separating The Moon Trine The North Node 3°45' Separating The Moon Sextile The Midheaven 0°17' Applying The Sun Semisquare Jupiter 0°50' Applying The Sun Sextile Saturn 1°52' Applying The Sun Trine Uranus 7°30' Applying Mercury Square Uranus 2°21' Separating Mercury Opposition Pluto 3°49' Applying Venus Sextile -
GEORGE HERBIG and Early Stellar Evolution
GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study. -
Extrasolar Planet Detection and Characterization with the KELT-North Transit Survey
Extrasolar Planet Detection and Characterization With the KELT-North Transit Survey DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Thomas G. Beatty Graduate Program in Astronomy The Ohio State University 2014 Dissertation Committee: Professor B. Scott Gaudi, Advisor Professor Andrew P. Gould Professor Marc H. Pinsonneault Copyright by Thomas G. Beatty 2014 Abstract My dissertation focuses on the detection and characterization of new transiting extrasolar planets from the KELT-North survey, along with a examination of the processes underlying the astrophysical errors in the type of radial velocity measurements necessary to measure exoplanetary masses. Since 2006, the KELT- North transit survey has been collecting wide-angle precision photometry for 20% of the sky using a set of target selection, lightcurve processing, and candidate identification protocols I developed over the winter of 2010-2011. Since our initial set of planet candidates were generated in April 2011, KELT-North has discovered seven new transiting planets, two of which are among the five brightest transiting hot Jupiter systems discovered via a ground-based photometric survey. This highlights one of the main goals of the KELT-North survey: to discover new transiting systems orbiting bright, V< 10, host stars. These systems offer us the best targets for the precision ground- and space-based follow-up observations necessary to measure exoplanetary atmospheres. In September 2012 I demonstrated the atmospheric science enabled by the new KELT planets by observing the secondary eclipses of the brown dwarf KELT-1b with the Spitzer Space Telescope. -
Weak-Line T Tauri Star Disks I. Initial Spitzer Results from the Cores to Disks Legacy Project
Weak-line T Tauri Star Disks I. Initial Spitzer Results from the Cores to Disks Legacy Project Deborah L. Padgett1, Lucas Cieza2, Karl R. Stapelfeldt3, Neal J. Evans, II2, David Koerner4, Anneila Sargent5, Misato Fukagawa1, Ewine F. van Dishoek6, Jean-Charles Augereau6, Lori Allen7, Geoff Blake5, Tim Brooke5, Nicholas Chapman8, Paul Harvey2, Alicia Porras7, Shih-Ping Lai8, Lee Mundy8, Philip C. Myers7, William Spiesman2, Zahed Wahhaj4 ABSTRACT Using the Spitzer Space Telescope, we have observed 90 weak-line and clas- sical T Tauri stars in the vicinity of the Ophiuchus, Lupus, Chamaeleon, and Taurus star-forming regions as part of the Cores to Disks (c2d) Spitzer Legacy project. In addition to the Spitzer data, we have obtained contemporaneous op- tical photometry to assist in constructing spectral energy distributions. These objects were specifically chosen as solar-type young stars with low levels of Hα emission, strong X-ray emission, and lithium absorption i.e. weak-line T Tauri stars, most of which were undetected in the mid-to-far IR by the IRAS survey. Weak-line T Tauri stars are potentially extremely important objects in determin- ing the timescale over which disk evolution may take place. Our objective is to determine whether these young stars are diskless or have remnant disks which arXiv:astro-ph/0603370v1 14 Mar 2006 are below the detection threshold of previous infrared missions. We find that only 5/83 weak-line T Tauri stars have detectable excess emission between 3.6 and 70 µm which would indicate the presence of dust from the inner few tenths of an AU out to the planet-forming regions a few tens of AU from the star. -
Peering Into the Formation History of Β Pictoris B with VLTI/GRAVITY Long-Baseline Interferometry? GRAVITY Collaboration: M
A&A 633, A110 (2020) https://doi.org/10.1051/0004-6361/201936898 Astronomy & © GRAVITY Collaboration 2020 Astrophysics Peering into the formation history of β Pictoris b with VLTI/GRAVITY long-baseline interferometry? GRAVITY Collaboration: M. Nowak1,16, S. Lacour1,2,3, P. Mollière10,4, J. Wang15,??, B. Charnay1, E. F. van Dishoeck3,10, R. Abuter2, A. Amorim8,12, J. P. Berger7, H. Beust7, M. Bonnefoy7, H. Bonnet2, W. Brandner4, A. Buron3, F. Cantalloube4, C. Collin1, F. Chapron1, Y. Clénet1, V. Coudé du Foresto1, P. T. de Zeeuw3,10, R. Dembet1, J. Dexter3, G. Duvert7, A. Eckart6,5, F. Eisenhauer3, N. M. Förster Schreiber3, P. Fédou1, R. Garcia Lopez9,4, F. Gao3, E. Gendron1, R. Genzel3,11, S. Gillessen3, F. Haußmann3, T. Henning4, S. Hippler4, Z. Hubert1, L. Jocou7, P. Kervella1, A.-M. Lagrange7, V. Lapeyrère1, J.-B. Le Bouquin7, P. Léna1, A.-L. Maire14,4, T. Ott3, T. Paumard1, C. Paladini2, K. Perraut7, G. Perrin1, L. Pueyo13, O. Pfuhl3,2, S. Rabien3, C. Rau3, G. Rodríguez-Coira1, G. Rousset1, S. Scheithauer4, J. Shangguan3, O. Straub1,3, C. Straubmeier6, E. Sturm3, L. J. Tacconi3, F. Vincent1, F. Widmann3, E. Wieprecht3, E. Wiezorrek3, J. Woillez2, S. Yazici3,6, and D. Ziegler1 (Affiliations can be found after the references) Received 11 October 2019 / Accepted 29 November 2019 ABSTRACT Context. β Pictoris is arguably one of the most studied stellar systems outside of our own. Some 30 yr of observations have revealed a highly-structured circumstellar disk, with rings, belts, and a giant planet: β Pictoris b. However very little is known about how this system came into being. -
Direct Imaging of Exoplanets
Direct Imaging of Exoplanets Wesley A. Traub Jet Propulsion Laboratory, California Institute of Technology Ben R. Oppenheimer American Museum of Natural History A direct image of an exoplanet system is a snapshot of the planets and disk around a central star. We can estimate the orbit of a planet from a time series of images, and we can estimate the size, temperature, clouds, atmospheric gases, surface properties, rotation rate, and likelihood of life on a planet from its photometry, colors, and spectra in the visible and infrared. The exoplanets around stars in the solar neighborhood are expected to be bright enough for us to characterize them with direct imaging; however, they are much fainter than their parent star, and separated by very small angles, so conventional imaging techniques are totally inadequate, and new methods are needed. A direct-imaging instrument for exoplanets must (1) suppress the bright star’s image and diffraction pattern, and (2) suppress the star’s scattered light from imperfections in the telescope. This chapter shows how exoplanets can be imaged by controlling diffraction with a coronagraph or interferometer, and controlling scattered light with deformable mirrors. 1. INTRODUCTION fainter than its star, and separated by 12.7 arcsec (98 AU at 7.7 pc distance). It was detected at two epochs, clearly showing The first direct images of exoplanets were published in common motion as well as orbital motion (see inset). 2008, fully 12 years after exoplanets were discovered, and Figure 2 shows a near-infrared composite image of exo- after more than 300 of them had been measured indirectly planets HR 8799 b,c,d by Marois et al. -
Rings Beyond the Giant Planets BRUNO SICARDY, MARYAME EL MOUTAMID, ALICE C
7 Rings beyond the giant planets BRUNO SICARDY, MARYAME EL MOUTAMID, ALICE C. QUILLEN, PAUL M. SCHENK, MARK R. SHOWALTER, AND KEVIN WALSH 7.1 Introduction scattered by gravitational tugs from Neptune or Uranus (Gladman et al., 2008). Until 2013, only the giant planets were known to host ring Chariklo was discovered in February 1997 (Scotti, 1997) systems. In June 2013, a stellar occulation revealed the pres- and is the largest Centaur known to date, with a diameter ence of narrow and dense rings around Chariklo, a small of about 240 km. Its very low geometric albedo (about 4%, Centaur object that orbits between Saturn and Uranus. see Table 7.1) makes it one of the darkest objects of the so- Meanwhile, the Cassini spacecraft revealed evidence for the lar system. It moves close to a 4:3 mean-motion resonance possible past presence of rings around the Saturnian satel- with Uranus, its main perturber. Dynamical studies indicate lites Rhea and Iapetus. Mars and Pluto are expected to have that Chariklo has been captured in its present orbital con- tenuous dusty rings, though they have so far evaded detec- figuration some 10 Myr ago, and that the half-life time of tion. More remotely, transit events observed around a star its unstable current orbit is about 10 Myr (Horner et al., in 2007 may have revealed for the first time exoplanetary 2004), a very short timescale compared to the age of the rings around a giant planet orbiting that star. solar system. So, evidence is building to show that rings are more com- Year-scale photometric (Belskaya et al., 2010) and spec- mon features in the universe than previously thought. -
Age Consistency Between Exoplanet Hosts and Field Stars
A&A 585, A5 (2016) Astronomy DOI: 10.1051/0004-6361/201527297 & c ESO 2015 Astrophysics Age consistency between exoplanet hosts and field stars A. Bonfanti1;2, S. Ortolani1;2, and V. Nascimbeni2 1 Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy e-mail: [email protected] 2 Osservatorio Astronomico di Padova, INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy Received 2 September 2015 / Accepted 3 November 2015 ABSTRACT Context. Transiting planets around stars are discovered mostly through photometric surveys. Unlike radial velocity surveys, photo- metric surveys do not tend to target slow rotators, inactive or metal-rich stars. Nevertheless, we suspect that observational biases could also impact transiting-planet hosts. Aims. This paper aims to evaluate how selection effects reflect on the evolutionary stage of both a limited sample of transiting-planet host stars (TPH) and a wider sample of planet-hosting stars detected through radial velocity analysis. Then, thanks to uniform deriva- tion of stellar ages, a homogeneous comparison between exoplanet hosts and field star age distributions is developed. Methods. Stellar parameters have been computed through our custom-developed isochrone placement algorithm, according to Padova evolutionary models. The notable aspects of our algorithm include the treatment of element diffusion, activity checks in terms of 0 log RHK and v sin i, and the evaluation of the stellar evolutionary speed in the Hertzsprung-Russel diagram in order to better constrain age. Working with TPH, the observational stellar mean density ρ? allows us to compute stellar luminosity even if the distance is not available, by combining ρ? with the spectroscopic log g. -
January 2016 BRAS Newsletter
January,2016 Next Meeting: Monday, Jan. 11th at 7pm at the HRPO Club member Craig Brenden participating in some outreach at the LPB Family Fun Fest What's In This Issue? President's Message Secretary's Summary of December Meeting Astro Short: Magnetically Levitating Black Holes Message from the HRPO Call for Volunteers for Adult Courses at HRPO Recent BRAS Forum Entries 20/20 Vision Campaign Observing Notes by John Nagle President's Message Welcome to a new year! There is a lot to be excited about this year. Chris Deselles will be giving his talk on Astrophotography, going into more detail and depth on processing the image, at the Cajun Clickers Computer Club on Thursday, January 7th, at the Broadmoor Methodist Church, located at Sharp and Mollylea in the adult building in the back, at 6:30 PM. Come hear the talk and support Chris. Annual retreat to the Rockefellers Wildlife Preserve will be on the first weekend in February, and Hodges Gardens Star Party in the beginning of April, details are on our website: www.brastro.org . On May 9th, Mercury will do a transit of the Sun for the first time in 10 years. More info will be in the newsletter as we get closer to the date. Dues are now due. You can bring them to the meeting on January 11th, or you can print out the application form on our website, and mail it with your payment to the address on the form. BRAS still has an opening for an Outreach Co-coordinator. Anyone interested, let me know. -
A SPECTROSCOPIC and PHOTOMETRIC INVESTIGA TION of the STELLAR ASSOCIATION CEPHEUS OB2. Th
This dissertation has been microfilmed exactly as received 68—3067 SIMONSON, HI, Simon Christian, 1938- A SPECTROSCOPIC AND PHOTOMETRIC INVESTIGA TION OF THE STELLAR ASSOCIATION CEPHEUS OB2. The Ohio State University, Ph.D., 1967 Astronomy University Microfilms, Inc., Ann Arbor, Michigan A SPECTROSCOPIC AND PHOTOMETRIC INVESTIGATION OP THE STELLAR ASSOCIATION CEPHEUS OB2 DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Simon Christian Simonson, III, S.B., M.Sc, The Ohio State University 1967 Approved fcy Department of Astronomy MKNOWLEDGMEHTS It is a pleasure to thank my adviser, Professor Arne Slettebak, for his encouragement, guidance, and support in this investigation. Professor Phillip C. Keenan and Pro fessor Carlos Jaschek read the manuscript and provided much helpful advice and criticism. I am also indebted to them and to Professor Slettebak for many discussions about the spectral classification. My wife, Jade, cheerfully endured the discomforts of a disrupted household, provided many useful ideas about computer programming, and also typed the manuscript and final copy in a most professional way. For all this and her loyal encouragement throughout the production of this thesis, I am grateful. The Lowell Observatory generously provided six nights of their 21-inch telescope time and gave substantial sup port during my observing period with the 72-inch telescope. I particularly thank Dr. John S. Hall, the director? Dr. Peter B. Boyce, who made his integrating photometer avail able? Dr. K. Serkowski, who provided his gain calibration in advance of publication? and Mr. Erik H. -
230Th AAS Session Table of Contents
230th AAS Austin, TX – June, 2017 Meeting Abstracts Session Table of Contents 100 – Welcome Address by AAS President Christine Jones (Harvard-Smithsonian, CfA) 101 – Kavli Foundation Lecture: Dark Matter in the Universe, Katherine Freese (University of Michigan) 102 – Extrasolar Planets: Detection and Future Prospects 103 – Instrumentation, and Things to do with Instrumentation: From the Ground 104 – Topics in Astrostatistics 105 – Inner Solar Systems: Planet Compositions as Tracers of Formation Location 106 – Annie Jump Cannon Award: Origins of Inner Solar Systems, Rebekah Dawson (Penn State University) 108 – Astronomy Education: Research, Practice, and Outreach Across the Human Continuum 109 – Bridging Laboratory & Astrophysics: Atomic Physics 110 – Preparing for JWST Observations: Insights from First Light and Assembly of Galaxies GTO Programs I 111 – Inner Solar Systems: Super-Earth Orbital Properties: Nature vs. Nurture 112 – Plenary Talk: The Universe's Most Extreme Star-forming Galaxies, Caitlin Casey (University of Texas, Austin) 113 – Plenary Talk: Science Highlights from SOFIA, Erick Young (USRA) 114 – Preparing for JWST Observations Poster Session 115 – Astronomy Education: Research, Practice, and Outreach Across the Human Continuum Poster Session 116 – Societal Matters Poster Session 117 – Instrumentation Poster Session 118 – Extrasolar Planets Poster Session 119 – The Solar System Poster Session 200 – LAD Plenary Talk: The Rosetta Mission to Comet 67P/ Churyumov-Gerasimenko, Bonnie Buratti (JPL) 201 –