Cosmic Rays and Super Nova Remnants
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Perturbations in the Motion of the Quasicomplanar Minor Planets For
Publications of the Department of Astronom} - Beograd, N2 ID, 1980 UDC 523.24; 521.1/3 osp PERTURBATIONS IN THE MOTION OF THE QUASICOMPLANAR MI NOR PLANETS FOR THE CASE PROXIMITIES ARE UNDER 10000 KM J. Lazovic and M. Kuzmanoski Institute of Astronomy, Faculty of Sciences, Beograd Received January 30, 1980 Summary. Mutual gravitational action during proximities of 12 quasicomplanar minor pla nets pairs have been investigated, whose minimum distances were under 10000 km. In five of the pairs perturbations of several orbital elements have been stated, whose amounts are detectable by observations from the Earth. J. Lazovic, M. Kuzmanoski, POREMECAJI ELEMENATA KRETANJA KVAZIKOM PLANARNIH MALIH PLANETA U PROKSIMITETIMA NJIHOVIH PUTANJA SA DA LJINAMA MANJIM OD 10000 KM - Ispitali smo medusobna gravitaciona de;stva pri proksi mitetima 12 parova kvazikomplanarnih malih planeta sa minimalnim daljinama ispod 10000 km. Kod pet parova nadeni su poremecaji u vi~e putanjskih elemenata, ~iji bi se iznosi mogli ustano viti posmatranjima sa Zemlje. Earlier we have found out 13 quasicomplanar minor planets pairs (the angle I between their orbital planes less than O~500), whose minimum mutual distances (pmin) were less than 10000 km (Lazovic, Kuzmanoski, 1978). The shortest pro ximity distance of only 600 km among these pairs has been stated with minor planet pair (215) Oenone and 1851 == 1950 VA. The corresponding perturbation effects in this pair have been calculated (Lazovic, Kuzmanoski, 1979a). This motivated us to investigate the mutual perturbing actions in the 12 remaining minor planets pairs for the case they found themselves within the proximities of their correspon ding orbits. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved. -
The Minor Planet Bulletin Lost a Friend on Agreement with That Reported by Ivanova Et Al
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 3, A.D. 2006 JULY-SEPTEMBER 49. LIGHTCURVE ANALYSIS FOR 19848 YEUNGCHUCHIU Kwong W. Yeung Desert Eagle Observatory P.O. Box 105 Benson, AZ 85602 [email protected] (Received: 19 Feb) The lightcurve for asteroid 19848 Yeungchuchiu was measured using images taken in November 2005. The lightcurve was found to have a synodic period of 3.450±0.002h and amplitude of 0.70±0.03m. Asteroid 19848 Yeungchuchiu was discovered in 2000 Oct. by the author at Desert Beaver Observatory, AZ, while it was about one degree away from Jupiter. It is named in honor of my father, The amplitude of 0.7 magnitude indicates that the long axis is Yeung Chu Chiu, who is a businessman in Hong Kong. I hoped to about 2 times that of the shorter axis, as seen from the line of sight learn the art of photometry by studying the lightcurve of 19848 as at that particular moment. Since both the maxima and minima my first solo project. have similar “height”, it’s likely that the rotational axis was almost perpendicular to the line of sight. Using a remote 0.46m f/2.8 reflector and Apogee AP9E CCD camera located in New Mexico Skies (MPC code H07), images of Many amateurs may have the misconception that photometry is a the asteroid were obtained on the nights of 2005 Nov. 20 and 21. very difficult science. After this learning exercise I found that, at Exposures were 240 seconds. -
Cumulative Index to Volumes 1-45
The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) .................. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 3, A.D. 2007 JULY-SEPTEMBER 53. CCD PHOTOMETRY OF ASTEROID 22 KALLIOPE Kwee, K.K. and von Woerden, H. (1956). Bull. Astron. Inst. Neth. 12, 327 Can Gungor Department of Astronomy, Ege University Trigo-Rodriguez, J.M. and Caso, A.S. (2003). “CCD Photometry 35100 Bornova Izmir TURKEY of asteroid 22 Kalliope and 125 Liberatrix” Minor Planet Bulletin [email protected] 30, 26-27. (Received: 13 March) CCD photometry of asteroid 22 Kalliope taken at Tubitak National Observatory during November 2006 is reported. A rotational period of 4.149 ± 0.0003 hours and amplitude of 0.386 mag at Johnson B filter, 0.342 mag at Johnson V are determined. The observation of 22 Kalliope was made at Tubitak National Observatory located at an elevation of 2500m. For this study, the 410mm f/10 Schmidt-Cassegrain telescope was used with a SBIG ST-8E CCD electronic imager. Data were collected on 2006 November 27. 305 images were obtained for each Johnson B and V filters. Exposure times were chosen as 30s for filter B and 15s for filter V. All images were calibrated using dark and bias frames Figure 1. Lightcurve of 22 Kalliope for Johnson B filter. X axis is and sky flats. JD-2454067.00. Ordinate is relative magnitude. During this observation, Kalliope was 99.26% illuminated and the phase angle was 9º.87 (Guide 8.0). Times of observation were light-time corrected. -
The Visible Spectroscopic Survey of 820 Asteroids ✩
Icarus 172 (2004) 179–220 www.elsevier.com/locate/icarus S3OS2: the visible spectroscopic survey of 820 asteroids ✩ D. Lazzaro a,∗,C.A.Angelia,J.M.Carvanoa, T. Mothé-Diniz a,R.Duffarda, M. Florczak b a Observatório Nacional, R. Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil b CEFET, Departamento Física, Av. Sete de Setembro 3165, 8230-091 Curitiba, Brazil Received 15 January 2004; revised 18 May 2004 Available online 4 August 2004 Abstract We present the results of a visible spectroscopic survey of 820 asteroids carried on between November 1996 and September 2001 at the 1.52 m telescope at ESO (La Silla). The instrumental set-up allowed an useful spectral range of about 4900 Å <λ<9200 Å. The global spatial distribution of the observed asteroids covers quite well all the region between 2.2 and 3.3 AU though some concentrations are apparent. These are due to the fact that several sub-sets of asteroids, such as families and groups, have been selected and studied during the development of the survey. The observed asteroids have been classified using the Tholen and the Bus taxonomies which, in general, agree quite well. 2004 Elsevier Inc. All rights reserved. Keywords: Asteroids; Asteroids, composition; Spectroscopy; Surfaces, asteroids 1. Introduction 1995; Bus, 1999; Burbine, 2000; Bus and Binzel, 2002a; Burbine and Binzel, 2002). Spectrophotometric observations It has long been realized the importance of a precise com- of nearly 600 asteroids were obtained by the ECAS while positional characterization of the asteroid belt to model the SMASS obtained spectroscopic observations of about 1400 Solar System origin and evolution. -
December 1996 the Official Publication of the Hamilton Centre of the Royal Astronomical Society of Canada
PRINTED MATTER RBIT December 1996 Vol. 29, Issue 11 Light Pollution - Toronto, Hamilton, and Buffalo The Official Publication of the Hamilton Centre of The Royal Astronomical Society of Canada Cover Image - Digitally Processed from International Dark Sky Association Image EDITORIAL MEMBERSHIP APPLICATION BY COLIN A. HAIG Application for Membership in the Hamilton Centre of the RASC. Annual membership officially commences October 1. We welcome people of all oliday time and still cloudy skies! Yikes! We have had a record of ages, skills, and interests in things Astronomical. Please make your cheque rotten weather for observing, but that has just meant its time to focus payable to: “RASC Hamilton Centre” and mail to the Treasurer c/o the energies elsewhere, into the Hamilton Centre, instead of into the address on the back. Associate membership is for those in other Astronomy skies. Please welcome a number of new members that have arrived, and let Clubs. Please state the club. Full members receive: The Observer’s them know when you will be out observing, so they can experience our Handbook ($20 value), Journal of RASC ($70 value), SkyNews ($22 value), facilities. I’d also like to extend a hearty welcome to our Trial Members, and and many other great privileges, including discounts on popular magazines, hope that they are finding what they are looking for. As always, if there is supplies and cool stuff. There is a Free 3 month Trial available - send no something of particular interest to you, you are most welcome to mention it to money! Info: Leave a message at: (905) 689-0266. -
The Minor Planet Bulletin Are Indexed in the Astrophysical Data System (ADS) and So Can Be Referenced by Others in Subsequent Papers
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 4, A.D. 2017 OCTOBER-DECEMBER 287. PHOTOMETRIC OBSERVATIONS OF MAIN-BELT were operated at sensor temperature of –15°C and images were ASTEROIDS 1990 PILCHER AND 8443 SVECICA calibrated with dark and flat-field frames. Stephen M. Brincat Both telescopes and cameras were controlled remotely from a Flarestar Observatory (MPC 171) nearby location via Sequence Generator Pro (Binary Star Fl.5/B, George Tayar Street Software). Photometric reduction, lightcurve construction, and San Gwann SGN 3160, MALTA period analyses were done using MPO Canopus software (Warner, [email protected] 2017). Differential aperture photometry was used and photometric measurements were based on the use of comparison stars of near- Winston Grech solar colour that were selected by the Comparison Star Selector Antares Observatory (CSS) utility available through MPO Canopus. Asteroid 76/3, Kent Street magnitudes were based on MPOSC3 catalog supplied with MPO Fgura FGR 1555, MALTA Canopus. (Received: 2017 June 8) 1990 Pilcher is an inner main-belt asteroid that was discovered on 1956 March 9 by K. Reinmuth at Heidelberg. Also known as 1956 We report on photometric observations of two main-belt EE, this asteroid was named in honor of Frederick Pilcher, asteroids, 1990 Pilcher and 8443 Svecica, that were associate professor of physics at Illinois College, Jacksonville acquired from 2017 March to May. We found the (Illinois), who has promoted extensively, the interest in minor synodic rotation period of 1990 Pilcher as 2.842 ± planets among amateur astronomers (Schmadel & Schmadel, 0.001 h and amplitude of 0.08 ± 0.03 mag and of 8443 1992). -
Moon Search Algorithms for NASA's Dawn Mission to Asteroid Vesta
Moon Search Algorithms for NASA’s Dawn Mission to Asteroid Vesta Nargess Memarsadeghi*a, Lucy A. McFaddena, David R. Skillmana, Brian McLeanb, Max Mutchlerb, Uri Carsenty c, Eric E. Palmer d, and the Dawn Mission’s Satellite Working Group aNASA Goddard Space Flight Center, Greenbelt, Maryland, USA bSpace Telescope Science Institute, Baltimore, Maryland, USA cDLR, Institute of the Planetary Research, Berlin, Germany dPlanetary Science Institute, Tucson, Arizona, USA ABSTRACT A moon or natural satellite is a celestial body that orbits a planetary body such as a planet, dwarf planet, or an asteroid. Scientists seek understanding the origin and evolution of our solar system by studying moons of these bodies. Additionally, searches for satellites of planetary bodies can be important to protect the safety of a spacecraft as it approaches or orbits a planetary body. If a satellite of a celestial body is found, the mass of that body can also be calculated once its orbit is determined. Ensuring the Dawn spacecraft’s safety on its mission to the asteroid (4) Vesta primarily motivated the work of Dawn’s Satellite Working Group (SWG) in summer of 2011. Dawn mission scientists and engineers utilized various computational tools and techniques for Vesta’s satellite search. The objectives of this paper are to 1) introduce the natural satellite search problem, 2) present the computational challenges, approaches, and tools used when addressing this problem, and 3) describe applications of various image processing and computational algorithms for performing satellite searches to the electronic imaging and computer science community. Furthermore, we hope that this communication would enable Dawn mission scientists to improve their satellite search algorithms and tools and be better prepared for performing the same investigation in 2015, when the spacecraft is scheduled to approach and orbit the dwarf planet (1) Ceres. -
The Minor Planet Bulletin It Would Be Very Helpful to Have Clearly More Realistic Period
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 1, A.D. 2007 JANUARY-MARCH 1. A ROTATION PERIOD FOR 1493 SIGRID -0.2 Colin Bembrick 1493 SIGRID Mt Tarana Observatory -0.1 PO Box 1537, Bathurst, NSW, Australia 0 [email protected] 0.1 Jeff Byron 0.2 Cecil Sayers Observatory 22-Jul 0.3 18 Albuera Rd, Epping, NSW, Australia 26-Jul 27-Jul 0.4 29-Jul (Received: 9 October Revised: 30 October) 1-Aug 0.5 6-Aug 7-Aug 0.6 22-Aug Minor planet 1493 Sigrid was observed over 8 nights in 0.7 2006. The synodic period was found to be 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 43.296±0.048hr with a peak-to-peak amplitude of at least 0.6 magnitudes. The axial ratio a/b implied by the peak to peak variation is 1.74. compared with most asteroids of less than 50km diameter, which have mean rotation rates of 2-3 revs/day (Binzel et al, 1989). Minor planet 1493 Sigrid was observed over a period of 32 days References from two sites in NSW, Australia, Mt Tarana Observatory (S 33d 26.1m E 149d 45.4m +880m) and Cecil Sayers Observa- Barbera, R. (2004). “AVE” Analisis de Variabilidad Estelar, tory (S 33d 46.9m E 151d 05.1m +80m). The Cecil Sayers version 2.51. Grup d’Estudis Astronomics. -
Moon Search Algorithms for NASA's Dawn Mission to Asteroid Vesta
Moon Search Algorithms for NASA’s Dawn Mission to Asteroid Vesta Nargess Memarsadeghi*a, Lucy A. McFaddena, David R. Skillmana, Brian McLeanb, Max Mutchlerb, Uri Carsenty c, Eric E. Palmer d, and the Dawn Mission’s Satellite Working Group aNASA Goddard Space Flight Center, Greenbelt, Maryland, USA bSpace Telescope Science Institute, Baltimore, Maryland, USA cDLR, Institute of the Planetary Research, Berlin, Germany dPlanetary Science Institute, Tucson, Arizona, USA ABSTRACT A moon or natural satellite is a celestial body that orbits a planetary body such as a planet, dwarf planet, or an asteroid. Scientists seek understanding the origin and evolution of our solar system by studying moons of these bodies. Additionally, searches for satellites of planetary bodies can be important to protect the safety of a spacecraft as it approaches or orbits a planetary body. If a satellite of a celestial body is found, the mass of that body can also be calculated once its orbit is determined. Ensuring the Dawn spacecraft’s safety on its mission to the asteroid (4) Vesta primarily motivated the work of Dawn’s Satellite Working Group (SWG) in summer of 2011. Dawn mission scientists and engineers utilized various computational tools and techniques for Vesta’s satellite search. The objectives of this paper are to 1) introduce the natural satellite search problem, 2) present the computational challenges, approaches, and tools used when addressing this problem, and 3) describe applications of various image processing and computational algorithms for performing satellite searches to the electronic imaging and computer science community. Furthermore, we hope that this communication would enable Dawn mission scientists to improve their satellite search algorithms and tools and be better prepared for performing the same investigation in 2015, when the spacecraft is scheduled to approach and orbit the dwarf planet (1) Ceres. -
Minor Planet Names: Alphabetical List
ASTEROIDS Minor Planet Names: Alphabetical List This is an alphabetical listing of the names of the numbered minor planets. It was last updated on 2011, June 17 The available asteroids are now well over 16,000. Here’s the reference site: http://www.astro.com/swisseph/astlist.htm You will notice the respective asteroid number in parenthesis to the immediate left of each asteroid. To find out where any asteroid is in your chart, consult below the AstroDienst site below: http://www.astro.com/cgi/genchart.cgi?&cid=rtbfilepar7OA-u1056512981&nhor=1 Once you have imput your own chart data, insert the asteroid numbers of those asteroids you are interested in finding out (specific location in your chart) at the bottom left of the page. It will state “additional asteroids or "hypothetical" planets (please enter the numbers from the respective lists, e.g. "433,1221,h48").” Then click to the right, “Click Here To Show The Chart.” ***************************** [Bill Wrobel] Note: References below to zodiacal placements are to my own chart: Born July 1, 1950, Syracuse, New York, USA, 2:22 pm EDT [Born July, 1, 1950 at 2:22 PDT, Syracuse, New York, 43 N2.9, 76 W 8.9. Ascendant is 22 Libra 7, MC 26 Cancer 34, 11th house is 0 Virgo 8, 12th house cusp is 28 Virgo 47, 2nd house 19 Scorpio 32, 3rd house 21 Sagittarius 29. Mars is 8 Libra 23 widely conjunct Neptune is 14 Libra35—Neptune in its own house and Mars, as a natural key to identity & personal action, in the 12th-Pisces-neptune (Letter Twelve) house.