The British Astronomical Association Handbook 2017
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Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes. -
The Minor Planet Bulletin and How the Situation Has Gone from One Mt Tarana Observatory of Trying to Fill Pages to One of Fitting Everything In
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 2, A.D. 2006 APRIL-JUNE 29. PHOTOMETRY OF ASTEROIDS 133 CYRENE, adjusted up or down to line up with the V-band data). The near- 454 MATHESIS, 477 ITALIA, AND 2264 SABRINA perfect overlay of V- and R-band data show no evidence of color change as the asteroid rotates. This result replicates the lightcurve Robert K. Buchheim period reported by Harris et al. (1984), and matches the period and Altimira Observatory lightcurve shape reported by Behrend (2005) at his website. 18 Altimira, Coto de Caza, CA 92679 USA [email protected] (Received: 4 November Revised: 21 November) Photometric studies of asteroids 133 Cyrene, 454 Mathesis, 477 Italia and 2264 Sabrina are reported. The lightcurve period for Cyrene of 12.707±0.015 h (with amplitude 0.22 mag) confirms prior studies. The lightcurve period of 8.37784±0.00003 h (amplitude 0.32 mag) for Mathesis differs from previous studies. For Italia, color indices (B-V)=0.87±0.07, (V-R)=0.48±0.05, and phase curve parameters H=10.4, G=0.15 have been determined. For Sabrina, this study provides the first reported lightcurve period 43.41±0.02 h, with 0.30 mag amplitude. Altimira Observatory, located in southern California, is equipped with a 0.28-m Schmidt-Cassegrain telescope (Celestron NexStar- 454 Mathesis. DiMartino et al. (1994) reported a rotation period of 11 operating at F/6.3), and CCD imager (ST-8XE NABG, with 7.075 h with amplitude 0.28 mag for this asteroid, based on two Johnson-Cousins filters). -
Alexandre Amorim -.:: GEOCITIES.Ws
Alexandre Amorim (org) 2 3 PREFÁCIO O Boletim Observe! é uma iniciativa da Coordenação de Observação Astronômica do Núcleo de Estudo e Observação Astronômica “José Brazilício de Souza” (NEOA-JBS). Durante a reunião administrativa do NEOA-JBS em maio de 2010 foi apresentada a edição de Junho de 2010 para apreciação dos demais coordenadores do Núcleo onde houve aprovação unânime em usar o Boletim Observe! como veículo de informação das atividades e, principalmente, observações astronômicas. O Boletim Observe! é publicado mensalmente em formato eletrônico ou impresso separadamente, prezando pela simplicidade das informações e encorajando os leitores a observar, registrar e publicar os eventos astronômicos. Desde a sua primeira edição o Boletim Observe! conta com a colaboração espontânea de diversos astrônomos amadores e profissionais. Toda edição do Observe! do mês de dezembro é publicado um índice dos artigos do respectivo ano. Porém, desde aquela edição de Junho de 2010 foram publicados centenas de artigos e faz-se necessário consultar assuntos que foram tratados nas edições anteriores do Observe! e seus respectivos autores. Para isso publicaremos anualmente esse Índice de Assuntos, permitindo a consulta rápida dos temas abordados. Florianópolis, 1º de dezembro de 2018 Alexandre Amorim Coordenação de Observação Astronômica do NEOA-JBS 4 Ano I (2010) Nº 1 – Junho 2010 Eclipse da Lua em 26 de junho de 2010 Amorim, A. Júpiter sem a Banda Equatorial Sul Amorim, A. Conjunção entre Júpiter e Urano Amorim, A. Causos do Avelino Alves, A. A. Quem foi Eugênia de Bessa? Amorim, A. Nº 2 – Julho 2010 Aprendendo a dimensionar as distâncias angulares no céu Neves, M. -
The Asteroid Florence 3122
The Asteroid Florence 3122 By Mohammad Hassan BACKGROUND • Asteroid 3122 Florence is a stony trinary asteroid of the Amor group. • It was discovered on March 2nd 1981 by Astronomer Schelte J. ”Bobby” Bus at Siding Spring Observatory. It was named in honor of Florence Nightingdale, the founder of modern nursing. • It has an approximate diameter of 5 kilometers. It also orbits the Sun at a distance of 1.0-2.5 astronomical unit once every 2 years and 4 months (859 days). • Florence rotates once every 2.4 hours, a result that was determined previously from optical measurements of the asteroid’s brightness variations. • THE MOST FASINATING THING IS THAT IT HAS TWO MOONS, HENCE WHY IT IS A PART OF THE AMOR GROUP. • The reason why this Asteroid 3122 Florence is important is because it is a near-earth object with the potential of hitting the earth in the future time. Concerns? • Florence 3122 was classified as a potentially hazardous object because of its minimum orbit intersection distance (less than 0.05 AU). This means that Florence 3122 has the potential to make close approaches to the Earth. • Another thing to keep in mind was that Florence 3122 minimum distance from us was 7 millions of km, about 20 times farthest than our moon. What actually happened? • On September 1st, 2017, Florence passed 0.047237 AU from Earth. That is about 7,000 km or 4,400 miles. • From Earth’s perspective, it brightened to apparent magnitude 8.5. It was also visible in small telescopes for several nights as it moved from south to north through the constellations. -
Modelling and Scaling Neglected Asteroids
Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Modelling and scaling neglected asteroids A. Marciniak1 with V. Alí-Lagoa, T. Müller, P. Bartczak, R. Behrend, M. Butkiewicz-B ˛ak, G. Dudzinski,´ R. Duffard, K. Dziadura, S. Fauvaud, M. Ferrais, S. Geier, J. Grice, R. Hirsch, J. Horbowicz, K. Kaminski,´ P. Kankiewicz, D.-H. Kim, M.-J. Kim, I. Konstanciak, V. Kudak, L. Molnár, F. Monteiro, W. Ogłoza, D. Oszkiewicz, A. Pál, N. Parley, F. Pilcher, E. Podlewska - Gaca, T. Polakis, J. J. Sanabria, T. Santana-Ros, B. Skiff, K. Sobkowiak, R. Szakáts, S. Urakawa, M. Zejmo,˙ K. Zukowski˙ 1. Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Poznan,´ Poland ESOP XXXIX, 29 August 2020 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Asteroid lightcurves (219) Thusnelda P = 59.74 h 487 Venetia P = 13.355h 2014 -2,1 Oct 11.1 Suhora 2012/2013 -2,2 Oct 12.1 Suhora Oct 29.0 Bor Oct 24.1 Bor. -2,05 Nov 10.2 Suh Oct 28.1 Bor. Nov 11.1 Suh CCCCCC Nov 4.0 Bor. CCCCCCCCC CC C C Nov 7.4 Organ M. Dec 28.8 Bor C Mar 2.8 Bor C Nov 8.4 Organ M. AAAA -2 Mar 3.8 Bor AAAAAA C Nov 13.4 Organ M. AAAA C CCC Nov 14.4 Organ M. A -2,1 AAA CCC A Nov 15.4 Organ M. A AA Nov 21.4 Winer -1,95 Dec 2.1 OAdM Dec 3.0 OAdM Dec 5.0 Bor. -
The Minor Planet Bulletin 44 (2017) 142
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 2, A.D. 2017 APRIL-JUNE 87. 319 LEONA AND 341 CALIFORNIA – Lightcurves from all sessions are then composited with no TWO VERY SLOWLY ROTATING ASTEROIDS adjustment of instrumental magnitudes. A search should be made for possible tumbling behavior. This is revealed whenever Frederick Pilcher successive rotational cycles show significant variation, and Organ Mesa Observatory (G50) quantified with simultaneous 2 period software. In addition, it is 4438 Organ Mesa Loop useful to obtain a small number of all-night sessions for each Las Cruces, NM 88011 USA object near opposition to look for possible small amplitude short [email protected] period variations. Lorenzo Franco Observations to obtain the data used in this paper were made at the Balzaretto Observatory (A81) Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Rome, ITALY Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Exposures were 60 seconds, unguided, with a clear filter. All Petr Pravec measurements were calibrated from CMC15 r’ values to Cousins Astronomical Institute R magnitudes for solar colored field stars. Photometric Academy of Sciences of the Czech Republic measurement is with MPO Canopus software. To reduce the Fricova 1, CZ-25165 number of points on the lightcurves and make them easier to read, Ondrejov, CZECH REPUBLIC data points on all lightcurves constructed with MPO Canopus software have been binned in sets of 3 with a maximum time (Received: 2016 Dec 20) difference of 5 minutes between points in each bin. -
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. -
Clasificación Taxonómica De Asteroides
Clasificación Taxonómica de Asteroides Cercanos a la Tierra por Ana Victoria Ojeda Vera Tesis sometida como requisito parcial para obtener el grado de MAESTRO EN CIENCIAS EN CIENCIA Y TECNOLOGÍA DEL ESPACIO en el Instituto Nacional de Astrofísica, Óptica y Electrónica Agosto 2019 Tonantzintla, Puebla Bajo la supervisión de: Dr. José Ramón Valdés Parra Investigador Titular INAOE Dr. José Silviano Guichard Romero Investigador Titular INAOE c INAOE 2019 El autor otorga al INAOE el permiso de reproducir y distribuir copias parcial o totalmente de esta tesis. II Dedicatoria A mi familia, con gran cariño. A mis sobrinos Ian y Nahil, y a mi pequeña Lia. III Agradecimientos Gracias a mi familia por su apoyo incondicional. A mi mamá Tere, por enseñarme a ser perseverante y dedicada, y por sus miles de muestras de afecto. A mi hermana Fernanda, por darme el tiempo, consejos y cariño que necesitaba. A mi pareja Odi, por su amor y cariño estos tres años, por su apoyo, paciencia y muchas horas de ayuda en la maestría, pero sobre todo por darme el mejor regalo del mundo, nuestra pequeña Lia. Gracias a mis asesores Dr. José R. Valdés y Dr. José S. Guichard, promotores de esta tesis, por su paciencia, consejos y supervisión, y por enseñarme con sus clases divertidas y motivadoras todo lo que se refiere a este trabajo. A los miembros del comité, Dra. Raquel Díaz, Dr. Raúl Mújica y Dr. Sergio Camacho, por tomarse el tiempo de revisar y evaluar mi trabajo. Estoy muy agradecida con todos por sus críticas constructivas y sugerencias. -
Ground-Based Visible Spectroscopy of Asteroids to Support the Development of an Unsupervised Gaia Asteroid Taxonomy A
Ground-based visible spectroscopy of asteroids to support the development of an unsupervised Gaia asteroid taxonomy A. Cellino, Ph. Bendjoya, M. Delbo’, Laurent Galluccio, J. Gayon-Markt, P. Tanga, E.F. Tedesco To cite this version: A. Cellino, Ph. Bendjoya, M. Delbo’, Laurent Galluccio, J. Gayon-Markt, et al.. Ground-based visible spectroscopy of asteroids to support the development of an unsupervised Gaia asteroid tax- onomy. Astronomy and Astrophysics - A&A, EDP Sciences, 2020, 10.1051/0004-6361/202038246. hal-02942763 HAL Id: hal-02942763 https://hal.archives-ouvertes.fr/hal-02942763 Submitted on 12 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astronomy & Astrophysics manuscript no. TNGspectra2ndrev c ESO 2020 July 28, 2020 Ground-based visible spectroscopy of asteroids to support development of an unsupervised Gaia asteroid taxonomy A. Cellino1, Ph. Bendjoya2, M. Delbo’3, L. Galluccio3, J. Gayon-Markt3, P. Tanga3, and E. F. Tedesco4 1 INAF, Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy e-mail: [email protected] 2 Université de la Côte d’Azur - Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Campus Valrose Nice, Nice Cedex 4, France e-mail: [email protected] 3 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, CS34229, 06304, Nice Cedex 4, France e-mail: [email protected], [email protected], [email protected] 4 Planetary Science Institute, Tucson, AZ, USA e-mail: [email protected] Received ..., 2020; accepted ..., 2020 ABSTRACT Context. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
Appendix 1 1311 Discoverers in Alphabetical Order
Appendix 1 1311 Discoverers in Alphabetical Order Abe, H. 28 (8) 1993-1999 Bernstein, G. 1 1998 Abe, M. 1 (1) 1994 Bettelheim, E. 1 (1) 2000 Abraham, M. 3 (3) 1999 Bickel, W. 443 1995-2010 Aikman, G. C. L. 4 1994-1998 Biggs, J. 1 2001 Akiyama, M. 16 (10) 1989-1999 Bigourdan, G. 1 1894 Albitskij, V. A. 10 1923-1925 Billings, G. W. 6 1999 Aldering, G. 4 1982 Binzel, R. P. 3 1987-1990 Alikoski, H. 13 1938-1953 Birkle, K. 8 (8) 1989-1993 Allen, E. J. 1 2004 Birtwhistle, P. 56 2003-2009 Allen, L. 2 2004 Blasco, M. 5 (1) 1996-2000 Alu, J. 24 (13) 1987-1993 Block, A. 1 2000 Amburgey, L. L. 2 1997-2000 Boattini, A. 237 (224) 1977-2006 Andrews, A. D. 1 1965 Boehnhardt, H. 1 (1) 1993 Antal, M. 17 1971-1988 Boeker, A. 1 (1) 2002 Antolini, P. 4 (3) 1994-1996 Boeuf, M. 12 1998-2000 Antonini, P. 35 1997-1999 Boffin, H. M. J. 10 (2) 1999-2001 Aoki, M. 2 1996-1997 Bohrmann, A. 9 1936-1938 Apitzsch, R. 43 2004-2009 Boles, T. 1 2002 Arai, M. 45 (45) 1988-1991 Bonomi, R. 1 (1) 1995 Araki, H. 2 (2) 1994 Borgman, D. 1 (1) 2004 Arend, S. 51 1929-1961 B¨orngen, F. 535 (231) 1961-1995 Armstrong, C. 1 (1) 1997 Borrelly, A. 19 1866-1894 Armstrong, M. 2 (1) 1997-1998 Bourban, G. 1 (1) 2005 Asami, A. 7 1997-1999 Bourgeois, P. 1 1929 Asher, D. -
ABSTRACT Title of Dissertation: WATER in the EARLY SOLAR
ABSTRACT Title of Dissertation: WATER IN THE EARLY SOLAR SYSTEM: INFRARED STUDIES OF AQUEOUSLY ALTERED AND MINIMALLY PROCESSED ASTEROIDS Margaret M. McAdam, Doctor of Philosophy, 2017. Dissertation directed by: Professor Jessica M. Sunshine, Department of Astronomy This thesis investigates connections between low albedo asteroids and carbonaceous chondrite meteorites using spectroscopy. Meteorites and asteroids preserve information about the early solar system including accretion processes and parent body processes active on asteroids at these early times. One process of interest is aqueous alteration. This is the chemical reaction between coaccreted water and silicates producing hydrated minerals. Some carbonaceous chondrites have experienced extensive interactions with water through this process. Since these meteorites and their parent bodies formed close to the beginning of the Solar System, these asteroids and meteorites may provide clues to the distribution, abundance and timing of water in the Solar nebula at these times. Chapter 2 of this thesis investigates the relationships between extensively aqueously altered meteorites and their visible, near and mid-infrared spectral features in a coordinated spectral-mineralogical study. Aqueous alteration is a parent body process where initially accreted anhydrous minerals are converted into hydrated minerals in the presence of coaccreted water. Using samples of meteorites with known bulk properties, it is possible to directly connect changes in mineralogy caused by aqueous alteration with spectral features. Spectral features in the mid-infrared are found to change continuously with increasing amount of hydrated minerals or degree of alteration. Building on this result, the degrees of alteration of asteroids are estimated in a survey of new asteroid data obtained from SOFIA and IRTF as well as archived the Spitzer Space Telescope data.