Some Parameters of Selected Neas
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Alactic Observer
alactic Observer G John J. McCarthy Observatory Volume 14, No. 2 February 2021 International Space Station transit of the Moon Composite image: Marc Polansky February Astronomy Calendar and Space Exploration Almanac Bel'kovich (Long 90° E) Hercules (L) and Atlas (R) Posidonius Taurus-Littrow Six-Day-Old Moon mosaic Apollo 17 captured with an antique telescope built by John Benjamin Dancer. Dancer is credited with being the first to photograph the Moon in Tranquility Base England in February 1852 Apollo 11 Apollo 11 and 17 landing sites are visible in the images, as well as Mare Nectaris, one of the older impact basins on Mare Nectaris the Moon Altai Scarp Photos: Bill Cloutier 1 John J. McCarthy Observatory In This Issue Page Out the Window on Your Left ........................................................................3 Valentine Dome ..............................................................................................4 Rocket Trivia ..................................................................................................5 Mars Time (Landing of Perseverance) ...........................................................7 Destination: Jezero Crater ...............................................................................9 Revisiting an Exoplanet Discovery ...............................................................11 Moon Rock in the White House....................................................................13 Solar Beaming Project ..................................................................................14 -
Jjmonl 1710.Pmd
alactic Observer John J. McCarthy Observatory G Volume 10, No. 10 October 2017 The Last Waltz Cassini’s final mission and dance of death with Saturn more on page 4 and 20 The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue INTERNATIONAL OBSERVE THE MOON NIGHT ...................... 4 SOLAR ACTIVITY ........................................................... 19 MONTE APENNINES AND APOLLO 15 .................................. 5 COMMONLY USED TERMS ............................................... 19 FAREWELL TO RING WORLD ............................................ 5 FRONT PAGE ............................................................... -
Detecting the Yarkovsky Effect Among Near-Earth Asteroids From
Detecting the Yarkovsky effect among near-Earth asteroids from astrometric data Alessio Del Vignaa,b, Laura Faggiolid, Andrea Milania, Federica Spotoc, Davide Farnocchiae, Benoit Carryf aDipartimento di Matematica, Universit`adi Pisa, Largo Bruno Pontecorvo 5, Pisa, Italy bSpace Dynamics Services s.r.l., via Mario Giuntini, Navacchio di Cascina, Pisa, Italy cIMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universits, UPMC Univ. Paris 06, Univ. Lille, 77 av. Denfert-Rochereau F-75014 Paris, France dESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy eJet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109 CA, USA fUniversit´eCˆote d’Azur, Observatoire de la Cˆote d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, Nice, France Abstract We present an updated set of near-Earth asteroids with a Yarkovsky-related semi- major axis drift detected from the orbital fit to the astrometry. We find 87 reliable detections after filtering for the signal-to-noise ratio of the Yarkovsky drift esti- mate and making sure the estimate is compatible with the physical properties of the analyzed object. Furthermore, we find a list of 24 marginally significant detec- tions, for which future astrometry could result in a Yarkovsky detection. A further outcome of the filtering procedure is a list of detections that we consider spurious because unrealistic or not explicable with the Yarkovsky effect. Among the smallest asteroids of our sample, we determined four detections of solar radiation pressure, in addition to the Yarkovsky effect. As the data volume increases in the near fu- ture, our goal is to develop methods to generate very long lists of asteroids with reliably detected Yarkovsky effect, with limited amounts of case by case specific adjustments. -
Asteroids and Comets: U.S
Columbia Law School Scholarship Archive Faculty Scholarship Faculty Publications 1997 Asteroids and Comets: U.S. and International Law and the Lowest-Probability, Highest Consequence Risk Michael B. Gerrard Columbia Law School, [email protected] Anna W. Barber Follow this and additional works at: https://scholarship.law.columbia.edu/faculty_scholarship Part of the Environmental Law Commons, and the International Law Commons Recommended Citation Michael B. Gerrard & Anna W. Barber, Asteroids and Comets: U.S. and International Law and the Lowest- Probability, Highest Consequence Risk, 6 N.Y.U. ENVTL. L. J. 4 (1997). Available at: https://scholarship.law.columbia.edu/faculty_scholarship/697 This Article is brought to you for free and open access by the Faculty Publications at Scholarship Archive. It has been accepted for inclusion in Faculty Scholarship by an authorized administrator of Scholarship Archive. For more information, please contact [email protected]. COLLOQUIUM ARTICLES ASTEROIDS AND COMETS: U.S. AND INTERNATIONAL LAW AND THE LOWEST-PROBABILITY, HIGHEST ICONSEQUENCE RISK MICHAEL B. GERRARD AND ANNA W. BARBER* INTRODUCrION Asteroids' and comets2 pose unique policy problems. They are the ultimate example of a low probability, high consequence event: no one in recorded human history is confirmed to have ever died from an asteroid or a comet, but the odds are that at some time in the next several centuries (and conceivably next year) an asteroid or a comet will cause mass localized destruction and that at some time in the coming half million years (and con- ceivably next year), an asteroid or a comet will kill several billion people. -
The Minor Planet Bulletin, Alan W
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 42, NUMBER 2, A.D. 2015 APRIL-JUNE 89. ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY SOUTHERN SKY OBSERVATORY: 2014 SEPTEMBER Lucas Bohn, Brianna Hibbler, Gregory Stein, Richard Ditteon Rose-Hulman Institute of Technology, CM 171 5500 Wabash Avenue, Terre Haute, IN 47803, USA [email protected] (Received: 24 November) Photometric data were collected over the course of seven nights in 2014 September for eight asteroids: 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 2699 Kalinin, 3197 Weissman, 7837 Mutsumi, 14927 Satoshi, and (29769) 1999 CE28. Eight asteroids were remotely observed from the Oakley Southern Sky Observatory in New South Wales, Australia. The observations were made on 2014 September 12-14, 16-19 using a 0.50-m f/8.3 Ritchey-Chretien optical tube assembly on a Paramount ME mount and SBIG STX-16803 CCD camera, binned 3x3, with a luminance filter. Exposure times ranged from 90 to 180 sec depending on the magnitude of the target. The resulting image scale was 1.34 arcseconds per pixel. Raw images were processed in MaxIm DL 6 using twilight flats, bias, and dark frames. MPO Canopus was used to measure the processed images and produce lightcurves. In order to maximize the potential for data collection, target asteroids were selected based upon their position in the sky approximately one hour after sunset. Only asteroids with no previously published results were targeted. Lightcurves were produced for 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 3197 Weissman, and (29769) 1999 CE28. -
198 5MNRAS.212. .817S Mon. Not. R. Astr. Soc. (1985
Mon. Not. R. astr. Soc. (1985) 212, 817-836 .817S 5MNRAS.212. Collisions in the Solar System -1. 198 Impacts of the Apollo-Amor-Aten asteroids upon the terrestrial planets Duncan I. Steel and W. J. Baggaley Department of Physics, University of Canterbury, Christchurch, New Zealand Accepted 1984 September 26. Received 1984 September 14; in original form 1984 July 11 Summary. The collision probability between each of the presently-known population of four Aten, 34 Apollo and 38 Amor asteroids and each of the terrestrial planets is determined by a new technique. The resulting mean collision rates, coupled with estimates of the total undiscovered population of each class, is useful in calculating the rate of removal of these bodies by the terrestrial planets, and the cratering rate on each planet by bodies of diameter in excess of 1 km. The influx to the Earth is found to be one impact per 160 000 yr, but this figure is biased by the inclusion of four recently-discovered low-inclination Apollos. Excluding these four the rate would be one per 250 000 yr, in line with previous estimates. The impact rate is highest for the Earth, being around twice that of Venus. The rates for Mercury and Mars using the present sample are about one per 5 Myr and one per 1.5 Myr respectively. 1 Introduction Over the past two decades our knowledge of the asteroids has expanded greatly. Physical studies of these bodies, reviewed by Chapman, Williams & Hartman (1978), Chapman (1983) and in Gehrels (1979), have shown that distinct groups of common genesis exist. -
Photometric and Astrometric Analysis of Three Near-Earth Asteroids
University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2021 Photometric And Astrometric Analysis Of Three Near-Earth Asteroids Steven D. Newcomb Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Newcomb, Steven D., "Photometric And Astrometric Analysis Of Three Near-Earth Asteroids" (2021). Theses and Dissertations. 3936. https://commons.und.edu/theses/3936 This Thesis is brought to you for free and open access by the Theses, Dissertations, and Senior Projects at UND Scholarly Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. PHOTOMETRIC AND ASTROMETRIC ANALYSIS OF THREE NEAR-EARTH ASTEROIDS by Steven Duane Newcomb Bachelor of Arts, California State University Sacramento, 2004 A Thesis Submitted to the Graduate Faculty of the University of North Dakota In partial fulfillment of the requirements for the degree of Master of Science Grand Forks, North Dakota May 2021 ii iii PERMISSION Title Photometric and Astrometric Analysis of Three Near-Earth Asteroids Department Space Studies Degree Master of Science In presenting this thesis in partial fulfillment of the requirements for a graduate degree from the University of North Dakota, I agree that the library of this University shall make it freely available for inspection. I further agree that permission for extensive copying for scholarly purposes may be granted by the professor who supervised my thesis work or, in her absence, by the Chairperson of the department or the dean of the School of Graduate Studies. -
1987Aj 93. . 738T the Astronomical Journal
738T . THE ASTRONOMICAL JOURNAL VOLUME 93, NUMBER 3 MARCH 1987 93. DISCOVERY OF M CLASS OBJECTS AMONG THE NEAR-EARTH ASTEROID POPULATION Edward F. TEDEScoa),b) Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109 1987AJ Jonathan Gradie20 Planetary Geosciences Division, Hawaii Institute of Geophysics, University of Hawaii, Honolulu, Hawaii 96822 Received 10 September 1986; revised 17 November 1986 ABSTRACT Broadband colorimetry (0.36 to 0.85 ¡um), visual photometry, near-infrared (JHK) photometry, and 10 and 20 /urn radiometry of the near-Earth asteroids 1986 DA and 1986 EB were obtained during March and April 1986. Model radiometric visual geometric albedos of 0.14 + 0.02 and 0.19 + 0.02 and model radiometric diameters of 2.3 + 0.1 and 2.0 + 0.1 km, respectively, (on the IRAS asteroid ther- mal model system described by Lebofsky et al. 1986) were derived from the thermal infrared and visual fluxes. These albedos, together with the colorimetric and (for 1986 DA) near-infrared data, establish that both objects belong to the M taxonomic class, the first of this kind to be recognized among the near-Earth asteroid population. This discovery, together with previous detections of C and S class objects, establishes that all three of the most common main-belt asteroid classes are represented among this population. The similarity in the corrected distribution of taxonomic classes among the 38 Earth- approaching asteroids for which such classes exist is similar to those regions of the main belt between the 3:1 (2.50 AU) and 5:2 (2.82 AU) orbital resonances with Jupiter, suggesting that they have their origins among asteroids in the vicinity of these resonances. -
Jjmonl 1612.Pmd
alactic Observer GJohn J. McCarthy Observatory Volume 9, No. 12 December 2016 Water - the elusive elixir of life in the cosmos - Is it even closer than we thought? The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky It is through their efforts that the McCarthy Observatory Technical Support has established itself as a significant educational and Bob Lambert recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Allison Tom Heydenburg Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Randy Finden Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue "OUT THE WINDOW ON YOUR LEFT"............................... 3 COMMONLY USED TERMS .............................................. 17 TAURUS-LITTROW .......................................................... 3 EARTH-SUN LAGRANGE POINTS & JAMES WEBB TELESCOPE 17 OVER THE TOP ............................................................... 4 REFERENCES ON DISTANCES ........................................ -
– Near-Earth Asteroid Mission Concept Study –
ASTEX – Near-Earth Asteroid Mission Concept Study – A. Nathues1, H. Boehnhardt1 , A. W. Harris2, W. Goetz1, C. Jentsch3, Z. Kachri4, S. Schaeff5, N. Schmitz2, F. Weischede6, and A. Wiegand5 1 MPI for Solar System Research, 37191 Katlenburg-Lindau, Germany 2 DLR, Institute for Planetary Research, 12489 Berlin, Germany 3 Astrium GmbH, 88039 Friedrichshafen, Germany 4 LSE Space AG, 82234 Oberpfaffenhofen, Germany 5 Astos Solutions, 78089 Unterkirnach, Germany 6 DLR GSOC, 82234 Weßling, Germany ASTEX Marco Polo Symposium, Paris 18.5.09, A. Nathues - 1 Primary Objectives of the ASTEX Study Identification of the required technologies for an in-situ mission to two near-Earth asteroids. ¾ Selection of realistic mission scenarios ¾ Definition of the strawman payload ¾ Analysis of the requirements and options for the spacecraft bus, the propulsion system, the lander system, and the launcher ASTEX ¾ Definition of the requirements for the mission’s operational ground segment Marco Polo Symposium, Paris 18.5.09, A. Nathues - 2 ASTEX Primary Mission Goals • The mission scenario foresees to visit two NEAs which have different mineralogical compositions: one “primitive'‘ object and one fragment of a differentiated asteroid. • The higher level goal is the provision of information and constraints on the formation and evolution history of our planetary system. • The immediate mission goals are the determination of: – Inner structure of the targets – Physical parameters (size, shape, mass, density, rotation period and spin vector orientation) – Geology, mineralogy, and chemistry ASTEX – Physical surface properties (thermal conductivity, roughness, strength) – Origin and collisional history of asteroids – Link between NEAs and meteorites Marco Polo Symposium, Paris 18.5.09, A. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 41, NUMBER 4, A.D. 2014 OCTOBER-DECEMBER 203. LIGHTCURVE ANALYSIS FOR 4167 RIEMANN Amy Zhao, Ashok Aggarwal, and Caroline Odden Phillips Academy Observatory (I12) 180 Main Street Andover, MA 01810 USA [email protected] (Received: 10 June) Photometric observations of 4167 Riemann were made over six nights in 2014 April. A synodic period of P = 4.060 ± 0.001 hours was derived from the data. 4167 Riemann is a main-belt asteroid discovered in 1978 by L. V. Period analysis was carried out by the authors using MPO Canopus Zhuraveya. Observations of the asteroid were conducted at the and its Fourier analysis feature developed by Harris (Harris et al., Phillips Academy Observatory, which is equipped with a 0.4-m f/8 1989). The resulting lightcurve consists of 288 data points. The reflecting telescope by DFM Engineering. Images were taken with period spectrum strongly favors the bimodal solution. The an SBIG 1301-E CCD camera that has a 1280x1024 array of 16- resulting lightcurve has synodic period P = 4.060 ± 0.001 hours micron pixels. The resulting image scale was 1.0 arcsecond per and amplitude 0.17 mag. Dips in the period spectrum were also pixel. Exposures were 300 seconds and taken primarily at –35°C. noted at 8.1200 hours (2P) and at 6.0984 hours (3/2P). A search of All images were guided, unbinned, and unfiltered. Images were the Asteroid Lightcurve Database (Warner et al., 2009) and other dark and flat-field corrected with Maxim DL. -
Instructions and Helpful Info
Target NEOs! Instructions and Helpful Info. (Modified and updated from the OSIRIS-REx Target Asteroids! website at https://www.asteroidmission.org) May 2021 Prerequisites for participation. • An interest in astronomy. • An interest in observing and providing data to the scientific community. • An interest in learning more about asteroids and near-Earth objects. • Appropriate observing equipment or access to equipment. • Membership in the Astronomical League through a member club or as an individual Member- at-Large. Request a registration form from the coordinators. • Complete the Target NEOs! registration form. • Periodically you will receive updated information about the program. Obtain instrumentation. The minimum instrumentation recommended to participate in this project is: • Telescope 8” or larger; • CCD/CMOS Camera, computer with internet connection; and • Data reduction software (available via Target NEOs!) If you have an appropriate telescope and camera, you will be able to observe asteroids on the Target NEOs! list. The asteroids that can be observed depend on the telescope’s aperture (diameter of the mirror or lens), light pollution, geographic location, and asteroid’s location in the sky on a given night. If you do not have a telescope, you can still participate in the program by obtaining access to observing equipment: • Team up and use a telescope owned by a friend, astronomy club, local college or planetarium observatory. • Use a commercial telescope service. • Are you a member of a local astronomy club? If not, we recommend it! Local astronomy clubs provide connections and opportunities for observations. You will meet friendly members who will be happy to help you. Check out the Astronomical League and NASA Night Sky Network to locate a club near you.