Observational Astronomy at the University of Pennsylvania 1751 - 2007
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Fire History and Climate Change
Synthesis of Knowledge: Fire History and Climate Change William T. Sommers Stanley G. Coloff Susan G. Conard JFSP Project 09‐2‐01‐09 Sommers, William T., Stanley G. Coloff and Susan G. Conard 2011: Fire History and Climate Change. Report Submitted to the Joint Fire Science Program for Project 09‐2‐01‐09. 215 pages + 6 Appendices Abstract This report synthesizes available fire history and climate change scientific knowledge to aid managers with fire decisions in the face of ongoing 21st Century climate change. Fire history and climate change (FHCC) have been ongoing for over 400 million years of Earth history, but increasing human influences during the Holocene epoch have changed both climate and fire regimes. We describe basic concepts of climate science and explain the causes of accelerating 21st Century climate change. Fire regimes and ecosystem classifications serve to unify ecological and climate factors influencing fire, and are useful for applying fire history and climate change information to specific ecosystems. Variable and changing patterns of climate‐fire interaction occur over different time and space scales that shape use of FHCC knowledge. Ecosystem differences in fire regimes, climate change and available fire history mean using an ecosystem specific view will be beneficial when applying FHCC knowledge. Authors William T. Sommers is a Research Professor at George Ma‐ son University in Fairfax, Virginia. He completed a B.S. de‐ gree in Meteorology from the City College of New York, a Acknowledgements S.M. degree in Meteorology from the Massachusetts Insti‐ We thank the Joint Fire Sciences Program for tute of Technology and a Ph.D. -
Daguerreian Annual 1990-2015: a Complete Index of Subjects
Daguerreian Annual 1990–2015: A Complete Index of Subjects & Daguerreotypes Illustrated Subject / Year:Page Version 75 Mark S. Johnson Editor of The Daguerreian Annual, 1997–2015 © 2018 Mark S. Johnson Mark Johnson’s contact: [email protected] This index is a work in progress, and I’m certain there are errors. Updated versions will be released so user feedback is encouraged. If you would like to suggest possible additions or corrections, send the text in the body of an email, formatted as “Subject / year:page” To Use A) Using Adobe Reader, this PDF can be quickly scrolled alphabetically by sliding the small box in the window’s vertical scroll bar. - or - B) PDF’s can also be word-searched, as shown in Figure 1. Many index citations contain keywords so trying a word search will often find other instances. Then, clicking these icons Figure 1 Type the word(s) to will take you to another in- be searched in this Adobe Reader Window stance of that word, either box. before or after. If you do not own the Daguerreian Annual this index refers you to, we may be able to help. Contact us at: [email protected] A Acuna, Patricia 2013: 281 1996: 183 Adams, Soloman; microscopic a’Beckett, Mr. Justice (judge) Adam, Hans Christian d’types 1995: 176 1995: 194 2002/2003: 287 [J. A. Whipple] Abbot, Charles G.; Sec. of Smithso- Adams & Co. Express Banking; 2015: 259 [ltr. in Boston Daily nian Institution deposit slip w/ d’type engraving Evening Transcript, 1/7/1847] 2015: 149–151 [letters re Fitz] 2014: 50–51 Adams, Zabdiel Boylston Abbott, J. -
Galaxy Clusters in Radio → Non-Thermal Phenomena
GalaxyGalaxy ClustersClusters inin radioradio ÎÎ NonNon--thermalthermal phenomenaphenomena Luigina Feretti Istituto di Radioastronomia CNR Bologna, Italy Tonanzintla, GH2005, 4-5 July 2005 Lecture 4 : Radio emission from cluster galaxies: Classical radio galaxies Radio – X-ray interaction Distorted structures: NAT and WAT Radio galaxies filling X-ray cavities Confinement : Trigger of radio emission: radio luminosity function Enhancement of star formation RadiogalaxiesRadiogalaxies X-ray:X-ray: ThermalThermal ggasas Radio:Radio: AA 119119 (z(z == 0.0441)0.0441) RadioRadio GalaxiesGalaxies PerseusPerseus X-rayX-ray ROSAROSATT PSPCPSPC HotHot gasgas NGC 1265 RadioRadio WSRTWSRT 4949 cmcm RadioRadio galaxiesgalaxies NGC 1275 IC310 RadioRadio galaxiesgalaxies ooff highhigh andand lowlow ppowerower havehave quitequite differentdifferent morphologiesmorphologies onon thethe largelarge scalescale (Fanaroff(Fanaroff && RileyRiley 11974)974) CygCyg AA FRFR IIII 24.24.55 -1-1 HighHigh popowewer:r: PP1.41.4 GHzGHz >> 1010 WW HzHz 3C3C 444499 24.524.5 -1-1 LowLow power:power: PP1.41.4 GHzGHz << 1010 WW HzHz FRFR II RADIORADIO GALAXIESGALAXIES ATAT INCREASINGINCREASING RADIORADIO POWERPOWER 1024 W Hz-1 at 1.4 GHz 3C 31 DA 240 4C 73.08 1026.5 W Hz-1 From Atlas of P.Leahy, powers computed With H0=75, q0=0.5 Owen and Ledlow 1994 TheThe radioradio emissionemission fromfrom INDIVIDUALINDIVIDUAL GALAXIESGALAXIES isis foufoundnd ttoo extendextend WELLWELL BEYONDBEYOND thethe physicalphysical sizesize ofof thethe hosthost opticaloptical galaxygalaxy (>(> oror -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
RADIO ASTRONOMY OBERVTORY Quarterly Report CHARLOTTESVILLE, VA
1 ; NATIONAL RADIO ASTRONOMY OBSERVATORY Charlottesville, Virginia t PROPERTY OF TH E U.S. G - iM RADIO ASTRONOMY OBERVTORY Quarterly Report CHARLOTTESVILLE, VA. 4 OCT 2 2em , July 1, 1984 - September 30, 1984 .. _._r_.__. _.. RESEARCH PROGRAMS 140-ft Telescope Hours Scheduled observing 1853.75 Scheduled maintenance and equipment changes 205.00 Scheduled tests and calibration 145.25 Time lost due to: equipment failure 122.00 power 3.25 weather 0.25 interference 14.50 The following continuum program was conducted during this quarter. No. Observer Program W193 N. White (European Space Observations at 6 cm of the eclipsing Agency) RS CVn system AR Lac. J. Culhane (Cambridge) J. Kuijpers (Utrecht) K. Mason (Cambridge) A. Smith (European Space Agency) The following line programs were conducted during this quarter. No. Observer Program B406 M. Bell (Herzberg) Observations at 13.9 GHz in search of H. Matthews (Herzberg) C6 H in TMC1. T. Sears (Brookhaven) B422 M. Bell (Herzberg) Observations at 3 cm to search for H. Matthews (Herzberg) C5 H in TMC1 and examination of T. Sears (Brookhaven) spectral features in IRC+10216 thought to be due to HC 9 N or C5 H. B423 M. Bell (Herzberg) Observations at 9895 MHz in an attempt H. Matthews (Herzberg) to detect C3 N in absorption against Cas A. 2 No. Observer Program B424 W. Batria Observations at 9.1 GHz of a newly discovered comet. C216 F. Clark (Kentucky) Observations at 6 cm and 18 cm of OH S. Miller (Kentucky) and H20 to study stellar winds and cloud dynamics. -
Inclination Evolution of Protoplanetary Disks Around Eccentric Binaries
Mon. Not. R. Astron. Soc. 000, 000{000 (0000) Printed 11 October 2017 (MN LATEX style file v2.2) Inclination Evolution of Protoplanetary Disks Around Eccentric Binaries J. J. Zanazzi1?, and Dong Lai1 1Cornell Center for Astrophysics, Planetary Science, Department of Astronomy, Cornell University, Ithaca, NY 14853, USA 11 October 2017 ABSTRACT It is usually thought that viscous torque works to align a circumbinary disk with the binary's orbital plane. However, recent numerical simulations suggest that the disk may evolve to a configuration perpendicular to the binary orbit (\polar alignment") if the binary is eccentric and the initial disk-binary inclination is sufficiently large. We carry out a theoretical study on the long-term evolution of inclined disks around eccentric binaries, calculating the disk warp profile and dissipative torque acting on the disk. For disks with aspect ratio H=r larger than the viscosity parameter α, bend- ing wave propagation effectively makes the disk precess as a quasi-rigid body, while viscosity acts on the disk warp and twist to drive secular evolution of the disk-binary inclination. We derive a simple analytic criterion (in terms of the binary eccentricity and initial disk orientation) for the disk to evolve toward polar alignment with the eccentric binary. When the disk has a non-negligible angular momentum compared to the binary, the final \polar alignment" inclination angle is reduced from 90◦. For typical protoplanetary disk parameters, the timescale of the inclination evolution is shorter than the disk lifetime, suggesting that highly-inclined disks and planets may exist orbiting eccentric binaries. Key words: Physical data and processes: accretion, accretion discs; Physical data and processes: hydrodynamics; stars: binaries: general; protoplanetary discs. -
Wynyard Planetarium & Observatory a Autumn Observing Notes
Wynyard Planetarium & Observatory A Autumn Observing Notes Wynyard Planetarium & Observatory PUBLIC OBSERVING – Autumn Tour of the Sky with the Naked Eye CASSIOPEIA Look for the ‘W’ 4 shape 3 Polaris URSA MINOR Notice how the constellations swing around Polaris during the night Pherkad Kochab Is Kochab orange compared 2 to Polaris? Pointers Is Dubhe Dubhe yellowish compared to Merak? 1 Merak THE PLOUGH Figure 1: Sketch of the northern sky in autumn. © Rob Peeling, CaDAS, 2007 version 1.2 Wynyard Planetarium & Observatory PUBLIC OBSERVING – Autumn North 1. On leaving the planetarium, turn around and look northwards over the roof of the building. Close to the horizon is a group of stars like the outline of a saucepan with the handle stretching to your left. This is the Plough (also called the Big Dipper) and is part of the constellation Ursa Major, the Great Bear. The two right-hand stars are called the Pointers. Can you tell that the higher of the two, Dubhe is slightly yellowish compared to the lower, Merak? Check with binoculars. Not all stars are white. The colour shows that Dubhe is cooler than Merak in the same way that red-hot is cooler than white- hot. 2. Use the Pointers to guide you upwards to the next bright star. This is Polaris, the Pole (or North) Star. Note that it is not the brightest star in the sky, a common misconception. Below and to the left are two prominent but fainter stars. These are Kochab and Pherkad, the Guardians of the Pole. Look carefully and you will notice that Kochab is slightly orange when compared to Polaris. -
Planets Transiting Non-Eclipsing Binaries
A&A 570, A91 (2014) Astronomy DOI: 10.1051/0004-6361/201323112 & c ESO 2014 Astrophysics Planets transiting non-eclipsing binaries David V. Martin1 and Amaury H. M. J. Triaud2;? 1 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, CH-1290 Sauverny, Switzerland e-mail: [email protected] 2 Kavli Institute for Astrophysics & Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA Received 22 November 2013 / Accepted 28 August 2014 ABSTRACT The majority of binary stars do not eclipse. Current searches for transiting circumbinary planets concentrate on eclipsing binaries, and are therefore restricted to a small fraction of potential hosts. We investigate the concept of finding planets transiting non-eclipsing binaries, whose geometry would require mutually inclined planes. Using an N-body code we explore how the number and sequence of transits vary as functions of observing time and orbital parameters. The concept is then generalised thanks to a suite of simulated circumbinary systems. Binaries are constructed from radial-velocity surveys of the solar neighbourhood. They are then populated with orbiting gas giants, drawn from a range of distributions. The binary population is shown to be compatible with the Kepler eclipsing binary catalogue, indicating that the properties of binaries may be as universal as the initial mass function. These synthetic systems produce transiting circumbinary planets occurring on both eclipsing and non-eclipsing binaries. Simulated planets transiting eclipsing binaries are compared with published Kepler detections. We find 1) that planets transiting non-eclipsing binaries are probably present in the Kepler data; 2) that observational biases alone cannot account for the observed over-density of circumbinary planets near the stability limit, which implies a physical pile-up; and 3) that the distributions of gas giants orbiting single and binary stars are likely different. -
A Fresh Insight Into the Evolutionary Status and Third Body Hypothesis of the Eclipsing Binaries AD Andromedae, AL Camelopardalis, and V338 Herculis
A&A 539, A129 (2012) Astronomy DOI: 10.1051/0004-6361/201117386 & c ESO 2012 Astrophysics A fresh insight into the evolutionary status and third body hypothesis of the eclipsing binaries AD Andromedae, AL Camelopardalis, and V338 Herculis A. Liakos1,P.Niarchos1, and E. Budding2,3 1 University of Athens, Department of Astrophysics, Astronomy and Mechanics, 157 84 Zografos, Athens, Greece e-mail: [alliakos;pniarcho]@phys.uoa.gr 2 Carter Observatory & School of Chemical and Physical Sciences, Victoria University, Wellington, New Zealand 3 Department of Physics and Astronomy, University of Canterbury, Christchurch, New Zealand e-mail: [email protected] Received 1 June 2011 / Accepted 11 January 2012 ABSTRACT Aims. We aim to derive the absolute parameters of the components of AD And, AL Cam, and V338 Her, interpret their orbital period changes and discuss their evolutionary status. Methods. New and complete multi-filter light curves of the eclipsing binaries AD And, AL Cam, and V338 Her were obtained and analysed with modern methods. Using all reliably observed times of minimum light, we examined orbital period irregularities using the least squares method. In addition, we acquired new spectroscopic observations during the secondary eclipses for AL Cam and V338 Her. Results. For AL Cam and V338 Her, we derive reliable spectral types for their primary stars. Statistical checks of orbital period analysis for all systems are very reassuring in the cases of V338 Her and AD And, although less so for AL Cam. The LIght-Time Effect (LITE) results are checked by inclusion of a third light option in the photometric analyses. -
Thesis, Anton Pannekoek Institute, Universiteit Van Amsterdam
UvA-DARE (Digital Academic Repository) The peculiar climates of ultra-hot Jupiters Arcangeli, J. Publication date 2020 Document Version Final published version License Other Link to publication Citation for published version (APA): Arcangeli, J. (2020). The peculiar climates of ultra-hot Jupiters. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:09 Oct 2021 Jacob Arcangeli of Ultra-hot Jupiters The peculiar climates The peculiar climates of Ultra-hot Jupiters Jacob Arcangeli The peculiar climates of Ultra-hot Jupiters Jacob Arcangeli © 2020, Jacob Arcangeli Contact: [email protected] The peculiar climates of Ultra-hot Jupiters Thesis, Anton Pannekoek Institute, Universiteit van Amsterdam Cover by Imogen Arcangeli ([email protected]) Printed by Amsterdam University Press ANTON PANNEKOEK INSTITUTE The research included in this thesis was carried out at the Anton Pannekoek Institute for Astronomy (API) of the University of Amsterdam. -
Charles Olivier and the Rise of Meteor Science
Springer Biographies Charles Olivier and the Rise of Meteor Science RICHARD TAIBI Springer Biographies More information about this series at http://www.springer.com/series/13617 Richard Taibi Charles Olivier and the Rise of Meteor Science 123 Richard Taibi Temple Hills, MD USA ISSN 2365-0613 ISSN 2365-0621 (electronic) Springer Biographies ISBN 978-3-319-44517-5 ISBN 978-3-319-44518-2 (eBook) DOI 10.1007/978-3-319-44518-2 Library of Congress Control Number: 2016949123 © Richard Taibi 2017 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors -
Lick Observatory Records: Photographs UA.036.Ser.07
http://oac.cdlib.org/findaid/ark:/13030/c81z4932 Online items available Lick Observatory Records: Photographs UA.036.Ser.07 Kate Dundon, Alix Norton, Maureen Carey, Christine Turk, Alex Moore University of California, Santa Cruz 2016 1156 High Street Santa Cruz 95064 [email protected] URL: http://guides.library.ucsc.edu/speccoll Lick Observatory Records: UA.036.Ser.07 1 Photographs UA.036.Ser.07 Contributing Institution: University of California, Santa Cruz Title: Lick Observatory Records: Photographs Creator: Lick Observatory Identifier/Call Number: UA.036.Ser.07 Physical Description: 101.62 Linear Feet127 boxes Date (inclusive): circa 1870-2002 Language of Material: English . https://n2t.net/ark:/38305/f19c6wg4 Conditions Governing Access Collection is open for research. Conditions Governing Use Property rights for this collection reside with the University of California. Literary rights, including copyright, are retained by the creators and their heirs. The publication or use of any work protected by copyright beyond that allowed by fair use for research or educational purposes requires written permission from the copyright owner. Responsibility for obtaining permissions, and for any use rests exclusively with the user. Preferred Citation Lick Observatory Records: Photographs. UA36 Ser.7. Special Collections and Archives, University Library, University of California, Santa Cruz. Alternative Format Available Images from this collection are available through UCSC Library Digital Collections. Historical note These photographs were produced or collected by Lick observatory staff and faculty, as well as UCSC Library personnel. Many of the early photographs of the major instruments and Observatory buildings were taken by Henry E. Matthews, who served as secretary to the Lick Trust during the planning and construction of the Observatory.