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Observation of the Airglow from the ISS by the IMAP Mission *Y
2013/3/13(ANGWIN workshop, Tachikawa) Observation of the airglow from the ISS by the IMAP mission *Y. Akiya [1], A. Saito [1], T. Sakanoi [2], Y. Hozumi [1], A. Yamazaki [3], Y. Otsuka [4] [1] Graduation School of Science, Kyoto University , [2] PPARC, Tohoku University, [3] ISAS/JAXA, [4] STE Laboratory, Nagoya University ----- Outline ----- Introduction of the IMAP mission Visible and near-infrared spectrographic imager Samples of airglow observation by VISI Summary “ISS-IMAP” mission Ionosphere, Mesosphere, Upper atmosphere and Plasmasphere Imagers of the ISS-IMAP mapping mission from the mission International Space Station (ISS) Observational imagers were installed on the Exposure Facility of Japanese Experimental Module: August 9th, 2012. Initial checkout: August and September, 2012 Nominal observations: October, 2012 - [Pictures: Courtesy of JAXA/NASA] [this issue]. According to characteristics of airglow emissions, wavelength range from 630 to 762 nm. Typical total intensity of such as intensity, emission height, background continuum, etc., we airglow is 100 1000 R as listed in Table 1, and 10 % variation of selected the airglow emissions which will be measured with VISI, the total intensity must be detected in order to investigate the and determined the requirements for instrumental design. The airglow variation pattern. In addition, short exposure cycle less targets and requirements are summarized in Table 1. than several seconds is necessary to measure small-scale airglow Table 1. Scientific Targets of VISI signatures (see Table 1) considering the orbital speed of ISS (~8 km/s). Airglow Required Region Scientific Typical A sectional view of VISI and its specifications are given in (waele- spatial (height) target intensity Figure 4 and Table 2, respectively. -
Dust and Gas in the Disk of Hl Tauri: Surface Density, Dust Settling, and Dust-To-Gas Ratio C
The Astrophysical Journal, 816:25 (12pp), 2016 January 1 doi:10.3847/0004-637X/816/1/25 © 2016. The American Astronomical Society. All rights reserved. DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO C. Pinte1,2, W. R. F. Dent3, F. Ménard1,2, A. Hales3,4, T. Hill3, P. Cortes3,4, and I. de Gregorio-Monsalvo3 1 UMI-FCA, CNRS/INSU, France (UMI 3386), and Dept. de Astronomía, Universidad de Chile, Santiago, Chile; [email protected] 2 Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France CNRS, IPAG, F-38000 Grenoble, France 3 Atacama Large Millimeter/Submillimeter Array, Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura 763-0355, Santiago, Chile 4 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA Received 2015 March 22; accepted 2015 September 8; published 2015 December 29 ABSTRACT The recent ALMA observations of the disk surrounding HL Tau reveal a very complex dust spatial distribution. We present a radiative transfer model accounting for the observed gaps and bright rings as well as radial changes of the emissivity index. We find that the dust density is depleted by at least a factor of 10 in the main gaps compared to the surrounding rings. Ring masses range from 10–100 M⊕ in dust, and we find that each of the deepest gaps is consistent with the removal of up to 40 M⊕ of dust. If this material has accumulated into rocky bodies, these would be close to the point of runaway gas accretion. -
Hubble Space Telescope Primer for Cycle 25
January 2017 Hubble Space Telescope Primer for Cycle 25 An Introduction to the HST for Phase I Proposers 3700 San Martin Drive Baltimore, Maryland 21218 [email protected] Operated by the Association of Universities for Research in Astronomy, Inc., for the National Aeronautics and Space Administration How to Get Started For information about submitting a HST observing proposal, please begin at the Cycle 25 Announcement webpage at: http://www.stsci.edu/hst/proposing/docs/cycle25announce Procedures for submitting a Phase I proposal are available at: http://apst.stsci.edu/apt/external/help/roadmap1.html Technical documentation about the instruments are available in their respective handbooks, available at: http://www.stsci.edu/hst/HST_overview/documents Where to Get Help Contact the STScI Help Desk by sending a message to [email protected]. Voice mail may be left by calling 1-800-544-8125 (within the US only) or 410-338-1082. The HST Primer for Cycle 25 was edited by Susan Rose, Senior Technical Editor and contributions from many others at STScI, in particular John Debes, Ronald Downes, Linda Dressel, Andrew Fox, Norman Grogin, Katie Kaleida, Matt Lallo, Cristina Oliveira, Charles Proffitt, Tony Roman, Paule Sonnentrucker, Denise Taylor and Leonardo Ubeda. Send comments or corrections to: Hubble Space Telescope Division Space Telescope Science Institute 3700 San Martin Drive Baltimore, Maryland 21218 E-mail:[email protected] CHAPTER 1: Introduction In this chapter... 1.1 About this Document / 7 1.2 What’s New This Cycle / 7 1.3 Resources, Documentation and Tools / 8 1.4 STScI Help Desk / 12 1.1 About this Document The Hubble Space Telescope Primer for Cycle 25 is a companion document to the HST Call for Proposals1. -
[OI] 5577 in the Airglow and the Aurora
Journal of Resea rch of the National Bureau of Sta ndards- D. Radio Propagation Vol. 63D, No.1, July-August 1959 Origin of [OlJ 5577 in the Airglow and the Aurora Franklin E. Roach, James W. McCaulley, and Edward Marovich (January 30, 1959) The distribution of 5577 zenith intensities at stations in the subauroral zone iB found to be unimodal with no discontinuity at the visual threshold. This is interpreted as evi dence that 5577 airglow and 5577 aurora may have a common origin. 1. Introduction origin hypothesis, their critical characteristic being the lack of any discontinuity. It i cu tomary to refer to [01] 5577 as airglow if In figure 2, a replot of the histogram of St. Amand it is invisible and as aurora if it is visible. Thus, and Ashburn is shown with a regroupillg of the data the physiological visual threshold (at approximately to correspond to class intervals of 50 R rather than the 10 R that they used. They put an approxi 1,000 myleighs 1 for extended objects) has been assumed to have a physical significance in the upper mately normal curve through the plot on the basis atmosphere with different mechanisms operative of which they were able to state that an intensity above and below the threshold. The purpose of correspondulg to a just visible aurora should occur this paper is to inquil'e into the existence of a only "once or twice in geologic time." Because physical criterion to distinguish between 5577 auroras do occur occasionally, though rarely, in southern California, the implication is that an aurora airglow and 5577 aurora. -
Condensation of the Solar Nebular
Formation of the Sun-like Stars • Collapse of a portion of a molecular cloud 4.5-4.6 Ga – Star dusts in primitive meteorites provide – Fingerprints of neaby stars that preceded our Sun – Stars like our Sun can form in a large number (hundreds to thousands) and close to each other (0.1 pc or ~0.3 lightyear, much closer than the Sun’s neighbor stars) as seen in the Orion Nebular. – Modern molecular clouds also has circumstellar disks, where planets form. – Gas in the molecular clouds is cold (~4K) and relatively dense (104 atoms/cm3). 1 Formation of the Sun-like Stars • Young stars emits more infrared radiation than a blackbody of the same size –Due to dark (opaque) disks around them. –Such disks are dubbed “proplyds” (proto-planetary disks). • Planets in the solar system orbit the Sun in the same direction and the orbits are roughly coplanar. –Suggests the solar system originated from a disk-shaped region of material referred to as the solar nebular. –An old idea conceived at least 2 centuries ago. –Discovery of proplyds now provide strong support. 2 Formation of the Sun-like Stars • Not clear what triggers the collapse of the densest portion of the cloud (“core”) to form stars. – Sequential ages of stars in close proximity in a molecular cloud suggests that formation and evolution of some stars trigger the formation of additional stars. • Gas around the collapsing core of the molecular cloud is moving – Too much angular momentum binary star – Otherwise, a single protostar called a T Tauri star or a pre-main sequence star. -
Annual Report 2017
Koninklijke Sterrenwacht van België Observatoire royal de Belgique Royal Observatory of Belgium Jaarverslag 2017 Rapport Annuel 2017 Annual Report 2017 Cover illustration: Above: One billion star map of our galaxy created with the optical telescope of the satellite Gaia (Credit: ESA/Gaia/DPAC). Below: Three armillary spheres designed by Jérôme de Lalande in 1775. Left: the spherical sphere; in the centre: the geocentric model of our solar system (with the Earth in the centre); right: the heliocentric model of our solar system (with the Sun in the centre). Royal Observatory of Belgium - Annual Report 2017 2 De activiteiten beschreven in dit verslag werden ondersteund door Les activités décrites dans ce rapport ont été soutenues par The activities described in this report were supported by De POD Wetenschapsbeleid De Nationale Loterij Le SPP Politique Scientifique La Loterie Nationale The Belgian Science Policy The National Lottery Het Europees Ruimtevaartagentschap De Europese Gemeenschap L’Agence Spatiale Européenne La Communauté Européenne The European Space Agency The European Community Het Fonds voor Wetenschappelijk Onderzoek – Le Fonds de la Recherche Scientifique Vlaanderen Royal Observatory of Belgium - Annual Report 2017 3 Table of contents Preface .................................................................................................................................................... 6 Reference Systems and Planetology ...................................................................................................... -
Hubbl E Space T El Escope Wfpc2 Imaging of Fs Tauri and Haro 6-5B1 John E.Krist,2 Karl R.Stapelfeldt,3 Christopher J.Burrows,2,4 Gilda E.Ballester,5 John T
THE ASTROPHYSICAL JOURNAL, 501:841È852, 1998 July 10 ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. HUBBL E SPACE T EL ESCOPE WFPC2 IMAGING OF FS TAURI AND HARO 6-5B1 JOHN E.KRIST,2 KARL R.STAPELFELDT,3 CHRISTOPHER J.BURROWS,2,4 GILDA E.BALLESTER,5 JOHN T. CLARKE,5 DAVID CRISP,3 ROBIN W.EVANS,3 JOHN S.GALLAGHER III,6 RICHARD E.GRIFFITHS,7 J. JEFF HESTER,8 JOHN G.HOESSEL,6 JON A.HOLTZMAN,9 JEREMY R.MOULD,10 PAUL A. SCOWEN,8 JOHN T.TRAUGER,3 ALAN M. WATSON,11 AND JAMES A. WESTPHAL12 Received 1997 December 18; accepted 1998 February 16 ABSTRACT We have observed the Ðeld of FS Tauri (Haro 6-5) with the Wide Field Planetary Camera 2 on the Hubble Space Telescope. Centered on Haro 6-5B and adjacent to the nebulous binary system of FS Tauri A there is an extended complex of reÑection nebulosity that includes a di†use, hourglass-shaped structure. H6-5B, the source of a bipolar jet, is not directly visible but appears to illuminate a compact, bipolar nebula which we assume to be a protostellar disk similar to HH 30. The bipolar jet appears twisted, which explains the unusually broad width measured in ground-based images. We present the Ðrst resolved photometry of the FS Tau A components at visual wavelengths. The Ñuxes of the fainter, eastern component are well matched by a 3360 K blackbody with an extinction ofAV \ 8. For the western star, however, any reasonable, reddened blackbody energy distribution underestimates the K-band photometry by over 2 mag. -
+ New Horizons
Media Contacts NASA Headquarters Policy/Program Management Dwayne Brown New Horizons Nuclear Safety (202) 358-1726 [email protected] The Johns Hopkins University Mission Management Applied Physics Laboratory Spacecraft Operations Michael Buckley (240) 228-7536 or (443) 778-7536 [email protected] Southwest Research Institute Principal Investigator Institution Maria Martinez (210) 522-3305 [email protected] NASA Kennedy Space Center Launch Operations George Diller (321) 867-2468 [email protected] Lockheed Martin Space Systems Launch Vehicle Julie Andrews (321) 853-1567 [email protected] International Launch Services Launch Vehicle Fran Slimmer (571) 633-7462 [email protected] NEW HORIZONS Table of Contents Media Services Information ................................................................................................ 2 Quick Facts .............................................................................................................................. 3 Pluto at a Glance ...................................................................................................................... 5 Why Pluto and the Kuiper Belt? The Science of New Horizons ............................... 7 NASA’s New Frontiers Program ........................................................................................14 The Spacecraft ........................................................................................................................15 Science Payload ...............................................................................................................16 -
The Birth of Stars and Planets
Unit 6: The Birth of Stars and Planets This material was developed by the Friends of the Dominion Astrophysical Observatory with the assistance of a Natural Science and Engineering Research Council PromoScience grant and the NRC. It is a part of a larger project to present grade-appropriate material that matches 2020 curriculum requirements to help students understand planets, with a focus on exoplanets. This material is aimed at BC Grade 6 students. French versions are available. Instructions for teachers ● For questions and to give feedback contact: Calvin Schmidt [email protected], ● All units build towards the Big Idea in the curriculum showing our solar system in the context of the Milky Way and the Universe, and provide background for understanding exoplanets. ● Look for Ideas for extending this section, Resources, and Review and discussion questions at the end of each topic in this Unit. These should give more background on each subject and spark further classroom ideas. We would be happy to help you expand on each topic and develop your own ideas for your students. Contact us at the [email protected]. Instructions for students ● If there are parts of this unit that you find confusing, please contact us at [email protected] for help. ● We recommend you do a few sections at a time. We have provided links to learn more about each topic. ● You don’t have to do the sections in order, but we recommend that. Do sections you find interesting first and come back and do more at another time. ● It is helpful to try the activities rather than just read them. -
REMOTE SENSING of SEISMIC ACTIVITY on VENUS USING a SMALL SPACECRAFT: INITIAL MODELING RESULTS, A. Komjathy1, A. Didion1, B. Sutin1, B
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 1731.pdf REMOTE SENSING OF SEISMIC ACTIVITY ON VENUS USING A SMALL SPACECRAFT: INITIAL MODELING RESULTS, A. Komjathy1, A. Didion1, B. Sutin1, B. Nakazono1, A. Karp1, M. Wallace1, G. Lan- toine1, S. Krishnamoorthy1, M. Rud1, J. Cutts, J. Makela2, M. Grawe2, P. Lognonné3, B. Kenda3, M. Drilleau3 and Jörn Helbert4 1Jet Propulsion Laboratory, California Institute of Technology, USA 2University of Illinois at Urbana-Champaign, USA 3Institut de Physique du Globe-Paris Sorbonne, France 4Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR), Germany Introduction: The planetary evolution and struc- other at 4.3 µm (visible on the dayside). The signifi- ture of Venus remain uncertain more than half a centu- cant advantage of observing nightglow on Venus is ry after the first visit by a robotic spacecraft. To under- that it is much brighter on Venus than on Earth [2] and stand how Venus evolved it is necessary to detect the that airglow lifetime (~4,000 sec) is significantly long- signs of seismic activity. Due to the adverse surface er than the period of seismic waves (10-30 sec). This conditions on Venus, with extremely high temperature makes it very attractive for directly detecting surface and pressure, it is infeasible with current technology, waves on Venus. This is in sharp contrast with Earth even using flagship missions, to place seismometers on where the lifetime of airglow is about one order of the surface for an extended period of time. Due to dy- magnitude smaller (~110 sec) than, e.g., the tsunami namic coupling between the solid planet and the at- waves we routinely observe on Earth with 630 nm air- mosphere, the waves generated by quakes propagate glow instruments [4]. -
X-Ray Jets Aneta Siemiginowska
Chandra News Issue 21 Spring 2014 Published by the Chandra X-ray Center (CXC) X-ray Jets Aneta Siemiginowska The Active Galaxy 4C+29.30 Credit: X-ray: NASA/CXC/SAO/A.Siemiginowska et al; Optical: NASA/STScI; Radio: NSF/NRAO/VLA Contents X-ray Jets HETG 3 Aneta Siemiginowska 18 David Huenemoerder (for the HETG team) 10 Project Scientist’s Report 20 LETG Martin Weisskopf Jeremy Drake 11 Project Manager’s Report 23 Chandra Calibration Roger Brissenden Larry David Message of Thanks to Useful Web Addresses 12 Harvey Tananbaum 23 The Chandra Team Belinda Wilkes Appointed as CIAO 4.6 13 Director of the CXC 24 Antonella Fruscione, for the CIAO Team Of Programs and Papers: Einstein Postdoctoral Fellowship 13 Making the Chandra Connection 29 Program Sherry Winkelman & Arnold Rots Andrea Prestwich Chandra Related Meetings Cycle 14 Peer Review Results 14 and Important Dates 30 Belinda Wilkes ACIS Chandra Users’ Committee 14 Paul Plucinsky, Royce Buehler, 34 Membership List Gregg Germain, & Richard Edgar HRC CXC 2013 Science Press 15 Ralph Kraft, Hans Moritz Guenther 35 Releases (SAO), and Wolfgang Pietsch (MPE) Megan Watzke The Chandra Newsletter appears once a year and is edited by Paul J. Green, with editorial assistance and layout by Evan Tingle. We welcome contributions from readers. Comments on the newsletter, or corrections and additions to the hardcopy mailing list should be sent to: [email protected]. Spring, 2014 3 X-ray Jets many unanswered questions, including the nature of relativistic jets, jet energetics, particle content, parti- Aneta Siemiginowska cle acceleration and emission processes. Both statis- tical studies of large samples of jets across the entire The first recorded observation of an extragalac- electromagnetic spectrum and deep broad-band imag- tic jet was made almost a century ago. -
197 6Apjs. . .30. .451H the Astrophysical Journal Supplement Series, 30:451-490, 1976 April © 1976. the American Astronomical S
.451H The Astrophysical Journal Supplement Series, 30:451-490, 1976 April .30. © 1976. The American Astronomical Society. All rights reserved. Printed in U.S.A. 6ApJS. 197 EVOLVED STARS IN OPEN CLUSTERS Gretchen L. H. Harris* David Dunlap Observatory, Richmond Hill, Ontario Received 1974 September 16; revised 1975 June 18 ABSTRACT Radial-velocity observations and MK classifications have been used to study evolved stars in 25 open clusters. Published data on stars in 72 additional clusters are rediscussed and com- bined with the observations friade in this investigation to yield positions in the Hertzsprung- Russell diagram for 559 evolved stars in 97 clusters. Ages for the parent clusters were estimated from the main-sequence turnoff points, earliest spectral types, and bluest stars in the clusters themselves. The evolved stars were sorted into six age groups ranging from 4 x 106 yr to 4 x 108 yr, and the composite H-R diagram for each age group was then used to study the evolutionary tracks for stars of various masses. The observational results were found to be in reasonably good agreement with recent theoretical computations. The composite color-magnitude diagrams were found to be strikingly different from those of the rich open clusters in the Magellanic Clouds. At a given age the red giants in the Small Magellanic Cloud and the Large Magellanic Cloud clusters are brighter and bluer than their galactic counterparts. It is suggested that these effects may be accounted for by differences in metal abundance. Subject headings: clusters: open — galaxies: Magellanic Clouds — radial velocities — stars : evolution — stars : late-type — stars : spectral classification 1.