DOCSLIB.ORG

Downloaded Freely from the Google Play Portal (

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

1 2 Spiral Galaxy M51. Herrero, E. Image from Montsec Astronomical Observatory (OAdM) 3 4 5 CONTENTS The Institute 6 Board of trustees 8 Scientific advisory board 9 Board of Directors 9 Staff 10 Scientific Research 16 Scientific results 25 Publications SCI 31 Papers in which only one institute is participating 31 Papers published by two institutes in collaboration 39 Papers published by three institutes in collaboration 40 Publications non SCI 40 Papers in which only one institute is participating 40 Papers published by two institutes in collaboration 46 Books edited 47 Courses 47 Contribution to conferences and seminars 48 Contribution to conferences 48 Seminars 59 Internal seminars 59 External seminars 59 Theses 61 Finished Theses 61 PhD Theses 61 Master theses 62 On going theses 62 PhD Theses 62 Master theses 62 Visiting scientists 64 Technological development activities 65 Technical reports and documents 65 Technical reports and documents developed by only one institute 65 Technical reports and documents developed by three institutes in collaboration 69 Technological development activities 69 Finished activities 69 Ongoing activities 69 Projects managed by the IEEC 69 Finished projects 69 Ongoing projects 70 Other scientific activities 72 Space missions 73 Mission proposals 82 Ground instrument projects 89 Montsec Astronomical Observatoyy (OAdM) 95 European Projects 99 Workshops organized by the IEEC 103 Outreach activities 107 Objectives, indicators and achievement 114 6 IEEC ▪ THE INSTITUTE The Institute of Space Studies of Catalonia (IEEC) was founded in February of 1996 as an initiative of the Fundació Catalana per a la Recerca (FCR), in collaboration with the University of Barcelona (UB), the Autonomous University of Barcelona (UAB), the Polytechnic University of Catalonia (UPC) and the Spanish Research Council (CSIC) with the objective of creating a multi-disciplinary and multi-institutional institute devoted to space research and their applications. In 2006 the FCR was reformed (currently its name is Fundació Catalana per a la Recerca i la innovació -FCRi) and its role was assumed by the Department of the Catalan Government responsible of scientific affairs. From the administrative point of view, the IEEC is a private, non—profit foundation. The reason why this administrative form was adopted was to dispose a versatile tool able to deal with the private industries and companies that finally are responsible of the construction of the systems and subsystems that eventually will fly. Outdoor view of Nexus building, IEEC’s location The agreements between the IEEC (a private institution) and the scientific institutions participating in the creation and governance of the institute (all of them public) allow the exchange of personnel and funds. To properly separate the private and public affairs, each one of these institutions created a scientific unit according their own bylaws in such a way that scientists can simultaneously act as member of their institutions or as a members of the IEEC. 7 These units are: The Institute of Cosmos Sciences [ACE (ICCUB)] is a university institute created by the UB devoted to high energy physics, gravitation, cosmology and astrophysics. Only the section of space sciences is affiliated to the IEEC. The Specific Center for Space Research [CERES (UAB)] is an “institute without walls” created by the UAB grouping physicists and engineers involved in space research. The Aeronautics and Space Research Center (formerly devoted to aeronautics and space – [CRAE-CTE (UPC)]) is an “institute without walls” created by the UPC grouping astronomers, physicists and engineers devoted to space research. The Institute for Space Sciences [ICE (CSIC)]. It is an institute of the CSIC just created to manage its support to the IEEC. The institute is governed by a Board of Directors composed by the directors of each unit. One of them, nominated by the Board of Trustees, acts as the chair of the Director’s Board. The administrative affairs are managed by the Head of Administration. As it corresponds to a confederate structure, the organization of each Research Unit is completely independent. 8 BOARD OF TRUSTEES The IEEC is governed by the Board of Trustees, composed by the Minister of the Department responsible of Research, the General Director of Research, the General Secretary of Industry, from the Catalan Government, the Rectors of the Barcelona University, Barcelona Autonomous University and Catalonia Polytechnic University, and the President of the Spanish Research Council. The Board of Trustees is chaired by the Minister of the Department of Research. President Hble. Sr. Andreu Mas-Colell Minister of Economy and Knowledge Government of Catalonia Secretary Sr. Josep Maria Martorell i Rodon General Research Director Government of Catalonia Members Excm. i Mg. Sr. Enric Fossas President Polytechnic University of Catalonia (UPC) Excm. Sr. Emilio Lora-Tamayo D’Ocon President Spanish Research Council (CSIC) Excm. i Mg. Sr. Dídac Ramírez Sarrió President University of Barcelona (UB) Excm. i Mg. Sr. Ferran Sancho Pifarré President Autonomous University of Barcelona (UAB) 9 INTERNATIONAL SCIENTIFIC ADVISORY BOARD The Scientific Advisory Committee is nominated by the Board of Trustees and its task is to inform about the quality of the scientific and technical production of the institute, the adequacy of the strategic plans and to advise about the acceptance of new members and the permanence of the older ones. Dr. Stephen S. Eikenberry University of Florida Dr. Álvaro Giménez European Space Agency (ESA). Chairman Dr. Manuel Martin-Neira European Space Agency (ESA) Dr. Tsevi Mazeh University of Tel Aviv Dr. Yannick Mellier Institut d'Astrophysiques de Paris BOARD OF DIRECTORS Dr. Carles Ferrer Director of CERES (UAB) Dr. Jordi Isern Director of ICE (CSIC). Chair Dr. J.J. Ramos Director of CRAE-CTE (UPC) Dr. E. Salvador Dierctor of ACE (ICCUB) Organization Chart 10 STAFF IEEC Surname, Name Category 1. Bertolín, Anna Administration 2. Guerrero, Josep IT Services 3. Minguell, Marta Administration 4. Montes, Pilar Manager 5. Notario, Eva Administration 6. Solís, Marta Science Communication MONTSEC ASTRONOMICAL OBSERVATORY (OAdM) STAFF Surname, Name Category 1. Gil, Pere Technician 2. Sanz, Josep Technician 3. Vilardell, Francesc Astronomer ACE (ICCUB) Surname, Name Category 1. Abedi, Hoda PhD Student 2. Àgueda Costafreda, Neus PostDoc 3. Antiche Garzón, Erika Engineer 4. Aran Sensat, Àngels PostDoc 5. Ariño Prats, Andreu PhD Student 6. Baena Gallé, Roberto PhD Student 7. Balaguer Núñez, Dolores PostDoc // Project manager 8. Borrachero Sánchez, Raúl Engineer 9. Bosch Ramon, Valentí Ramon y Cajal PostDoc 10. Canal Masgoret, Ramon Professor 11. Carrasco Martínez, José M. PostDoc 12. Casamiquela Floriach, Laia PhD Student 13. Casademunt Viader, Jaume Professor 14. Castañeda Pons, Javier Engineer 15. Clotet Altarriba, Marcial Engineer 16. Crusats Aliguer, Joaquim Professor 17. Cuesta Vázquez, Antonio José PostDoc 18. El-Hachemi Metni, Zoubir Professor 19. Estalella Boadella, Robert Professor 20. Fabricius, Claus Vilhelm Researcher 21. Figueras Siñol, Francesca Professor 11 22. Galindo Fernández, Daniel Master Student 23. Garralda Torres, Nora Engineer 24. Gracia, Gonzalo PostDoc 25. Gómez Cama, Jose M. Professor 26. Gómez Muntané, Gerard Professor 27. Gontcho A Gontcho, Satya PhD Student 28. González Vidal, Juan José Engineer 29. Iwasawa, Kazushi ICREA Professor 30. Jimenez Tellado, Raúl ICREA Professor 31. Jordi Nebot, Carme Professor 32. Juan Rovira, Enric PhD Student 33. Julbe López, Francesc Engineer 34. López Hermoso, Rosario Professor 35. Luri Carrascoso, F. Xavier Professor 36. Manrique Oliva, Alberto Professor 37. Marcote Martin, Benito PhD Student 38. Mas Ribas, Lluís PhD Student 39. Masana Fresno, Eduard PostDoc 40. Merino Espasa, M. Teresa PhD Student 41. Migliari, Simone Ramon y Cajal PostDoc 42. Miralda Escudé, Jordi ICREA Professor 43. Molina Martínez, Daniel Engineer 44. Monguió Montells, Maria PhD Student 45. Moreno de la Cita, Víctor PhD Student 46. Munar Adrover, Pere PhD Student 47. Núñez de Murga, Jorge C. Professor 48. Olikara, Zubin Philip PhD Student 49. Oriol Bitaubé, Pablo PhD Student 50. Padoan, Paolo ICREA Professor 51. Paita, Fabrizio PhD Student 52. Palmer, Max PhD Student 53. Paredes Fortuny, Xavier PhD Student 54. Paredes Poy, Josep Maria Professor 55. Pérez Palau, Daniel PhD Student 56. Pérez Ràfols, Ignasi PhD Student 57. Portell i de Mora, Jordi PostDoc 58. Ribó Gomis, Marc Professor 59. Ribó Trujillo, Josep M. Professor Emeritous 60. Roca Fàbrega, Santiago PhD Student 61. Romero Gómez, Mercè PostDoc 12 62. Ruiz Lapuente, Pilar Professor 63. Ruiz Martí, J.Xavier Professor 64. Sabater Morros, Josep Engineer 65. Sala Mirabet, Ferran Professor 66. Salvador Solé, Eduard Professor 67. Sanahuja Parera, Blai Professor 68. Sestayo de la Cerra, Yolanda PostDoc 69. Solanes Majua, José M. Professor 70. Torra Roca, Jordi Professor 71. Verde, Licia ICREA Professor 72. Voss, Holger PostDoc 73. Weiler, Michael PostDoc 74. Zanin, Roberta PostDoc CERES (UAB) Surname, Name Category 1. Campanella Pineda, Humberto Associated Professor 2. Cardona Cardona, Luis Andrés PhD Student 3. del Peral Rosado, José Antonio PhD Student 4. Doro, Michele Guest researcher 5. Ferrer Ramis, Carles Professor 6. Font Guiteras, Lluis Professor 7. García Carril, Vanessa Support 8. García Quinchía, Alex PhD Student 9. Garrido Terrats, Daniel PhD Student 10. Gaug, Markus PostDoc 11. Gòdia Casablancas, Francesc Professor 12. Godignon,
Recommended publications
  • Comet C/2018 V1 (Machholz-Fujikawa-Iwamoto): Data Ulate About Past Visits of Interstellar Comets on the Basis of Available Using a 0.47-M Reflector, D

    Comet C/2018 V1 (Machholz-Fujikawa-Iwamoto): Data Ulate About Past Visits of Interstellar Comets on the Basis of Available Using a 0.47-M Reflector, D

    MNRAS 000, 1–11 (2019) Preprint 30 August 2019 Compiled using MNRAS LATEX style file v3.0 Comet C/2018 V1 (Machholz-Fujikawa-Iwamoto): dislodged from the Oort Cloud or coming from interstellar space? C. de la Fuente Marcos1⋆ and R. de la Fuente Marcos2 1 Universidad Complutense de Madrid, Ciudad Universitaria, E-28040 Madrid, Spain 2AEGORA Research Group, Facultad de Ciencias Matemáticas, Universidad Complutense de Madrid, Ciudad Universitaria, E-28040 Madrid, Spain Accepted 2019 August 3. Received 2019 July 26; in original form 2019 February 17 ABSTRACT The chance discovery of the first interstellar minor body, 1I/2017 U1 (‘Oumuamua), indicates that we may have been visited by such objects in the past and that these events may repeat in the future. Unfortunately, minor bodies following nearly parabolic or hyperbolic paths tend to receive little attention: over 3/4 of those known have data-arcs shorter than 30 d and, con- sistently, rather uncertain orbit determinations. This fact suggests that we may have observed interstellar interlopers in the past, but failed to recognize them as such due to insufficient data. Early identification of promising candidates by using N-body simulations may help in improv- ing this situation, triggering follow-up observations before they leave the Solar system. Here, we use this technique to investigate the pre- and post-perihelion dynamical evolution of the slightly hyperbolic comet C/2018 V1 (Machholz-Fujikawa-Iwamoto) to understand its origin and relevance within the context of known parabolic and hyperbolic minor bodies. Based on the available data, our calculations suggest that although C/2018 V1 may be a former mem- ber of the Oort Cloud, an origin beyond the Solar system cannot be excluded.
  • Dust Near the Sun

    Dust Near the Sun

    Dust Near The Sun Ingrid Mann and Hiroshi Kimura Institut f¨urPlanetologie, Westf¨alischeWilhelms-Universit¨at,M¨unster,Germany Douglas A. Biesecker NOAA, Space Environment Center, Boulder, CO, USA Bruce T. Tsurutani Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA Eberhard Gr¨un∗ Max-Planck-Institut f¨urKernphysik, Heidelberg, Germany Bruce McKibben Department of Physics and Space Science Center, University of New Hampshire, Durham, NH, USA Jer-Chyi Liou Lockheed Martin Space Operations, Houston, TX, USA Robert M. MacQueen Rhodes College, Memphis, TN, USA Tadashi Mukai† Graduate School of Science and Technology, Kobe University, Kobe, Japan Lika Guhathakurta NASA Headquarters, Washington D.C., USA Philippe Lamy Laboratoire d’Astrophysique Marseille, France Abstract. We review the current knowledge and understanding of dust in the inner solar system. The major sources of the dust population in the inner solar system are comets and asteroids, but the relative contributions of these sources are not quantified. The production processes inward from 1 AU are: Poynting- Robertson deceleration of particles outside of 1 AU, fragmentation into dust due to particle-particle collisions, and direct dust production from comets. The loss processes are: dust collisional fragmentation, sublimation, radiation pressure acceler- ation, sputtering, and rotational bursting. These loss processes as well as dust surface processes release dust compounds in the ambient interplanetary medium. Between 1 and 0.1 AU the dust number densities and fluxes can be described by inward extrapolation of 1 AU measurements, assuming radial dependences that describe particles in close to circular orbits. Observations have confirmed the general accuracy of these assumptions for regions within 30◦ latitude of the ecliptic plane.
  • Ice& Stone 2020

    Ice& Stone 2020

    Ice & Stone 2020 WEEK 51: DECEMBER 13-19 Presented by The Earthrise Institute # 51 Authored by Alan Hale COMET OF THE WEEK: The Great Comet of 1680 Perihelion: 1680 December 18.49, q = 0.006 AU The Great Comet of 1680 over Rotterdam in The Netherlands, during late December 1680 as painted by the Dutch artist Lieve Verschuier. This particular comet was undoubtedly one of the brightest comets of the 17th Century, but it is also one of the most important comets in history from a scientific perspective, and perhaps even from the perspective of overall human history. While there were certainly plenty of superstitions attached to the comet’s appearance, the scientific investigations made of it were among the beginnings of the era in European history we now call The Enlightenment, and indeed, in a sense the Great Comet of 1680 can perhaps be considered as one of the sparks of that era. The significance began with the comet’s discovery, which was made on the morning of November 14, 1680, by a German astronomer residing in Coburg, Gottfried Kirch – the first comet ever to be discovered by means of a telescope. It was already around 4th magnitude at that time, and located near the star Regulus in the constellation Leo; from that point it traveled eastward and brightened rapidly, being closest to Earth (0.42 AU) on November 30. By that time it was a conspicuous naked-eye object with a tail 20 to 30 degrees long, and it remained visible for another week before disappearing into morning twilight.
  • The Minor Planet Bulletin 44 (2017) 142

    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.
  • An Anisotropic Distribution of Spin Vectors in Asteroid Families

    An Anisotropic Distribution of Spin Vectors in Asteroid Families

    Astronomy & Astrophysics manuscript no. families c ESO 2018 August 25, 2018 An anisotropic distribution of spin vectors in asteroid families J. Hanuš1∗, M. Brož1, J. Durechˇ 1, B. D. Warner2, J. Brinsfield3, R. Durkee4, D. Higgins5,R.A.Koff6, J. Oey7, F. Pilcher8, R. Stephens9, L. P. Strabla10, Q. Ulisse10, and R. Girelli10 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holešovickáchˇ 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 Via Capote Observatory, Thousand Oaks, CA 91320, USA 4 Shed of Science Observatory, 5213 Washburn Ave. S, Minneapolis, MN 55410, USA 5 Hunters Hill Observatory, 7 Mawalan Street, Ngunnawal ACT 2913, Australia 6 980 Antelope Drive West, Bennett, CO 80102, USA 7 Kingsgrove, NSW, Australia 8 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 9 Center for Solar System Studies, 9302 Pittsburgh Ave, Suite 105, Rancho Cucamonga, CA 91730, USA 10 Observatory of Bassano Bresciano, via San Michele 4, Bassano Bresciano (BS), Italy Received x-x-2013 / Accepted x-x-2013 ABSTRACT Context. Current amount of ∼500 asteroid models derived from the disk-integrated photometry by the lightcurve inversion method allows us to study not only the spin-vector properties of the whole population of MBAs, but also of several individual collisional families. Aims. We create a data set of 152 asteroids that were identified by the HCM method as members of ten collisional families, among them are 31 newly derived unique models and 24 new models with well-constrained pole-ecliptic latitudes of the spin axes.
  • 7 X 11 Long.P65

    7 X 11 Long.P65

    Cambridge University Press 978-0-521-85349-1 - Meteor Showers and their Parent Comets Peter Jenniskens Index More information Index a – semimajor axis 58 twin shower 440 A – albedo 111, 586 fragmentation index 444 A1 – radial nongravitational force 15 meteoroid density 444 A2 – transverse, in plane, nongravitational force 15 potential parent bodies 448–453 A3 – transverse, out of plane, nongravitational a-Centaurids 347–348 force 15 1980 outburst 348 A2 – effect 239 a-Circinids (1977) 198 ablation 595 predictions 617 ablation coefficient 595 a-Lyncids (1971) 198 carbonaceous chondrite 521 predictions 617 cometary matter 521 a-Monocerotids 183 ordinary chondrite 521 1925 outburst 183 absolute magnitude 592 1935 outburst 183 accretion 86 1985 outburst 183 hierarchical 86 1995 peak rate 188 activity comets, decrease with distance from Sun 1995 activity profile 188 Halley-type comets 100 activity 186 Jupiter-family comets 100 w 186 activity curve meteor shower 236, 567 dust trail width 188 air density at meteor layer 43 lack of sodium 190 airborne astronomy 161 meteoroid density 190 1899 Leonids 161 orbital period 188 1933 Leonids 162 predictions 617 1946 Draconids 165 upper mass cut-off 188 1972 Draconids 167 a-Pyxidids (1979) 199 1976 Quadrantids 167 predictions 617 1998 Leonids 221–227 a-Scorpiids 511 1999 Leonids 233–236 a-Virginids 503 2000 Leonids 240 particle density 503 2001 Leonids 244 amorphous water ice 22 2002 Leonids 248 Andromedids 153–155, 380–384 airglow 45 1872 storm 380–384 albedo (A) 16, 586 1885 storm 380–384 comet 16 1899
  • Asteroid Regolith Weathering: a Large-Scale Observational Investigation

    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.
  • WG Photometry and Polarimetry of Asteroids

    WG Photometry and Polarimetry of Asteroids

    PHOTOMETRY AND POLARIMETRY OF ASTEROIDS: IMPACT ON COLLABORATION Abstracts The International Workshop -2 80 0 60 2 40 4 20 6 Relative Magnitude Polarization Degree 0 8 10 -20 0 20 40 60 80 100 120 140 160 180 Phase Angle June 15–18, 2003, Kharkiv, Ukraine Organized by Research Institute of Astronomy of V. N. Karazin Kharkiv National University, Ukrainian Astronomical Association Ministry of Education and Science of Ukraine Sponsored by Kharkiv City Charity Fund “AVEC” PHOTOMETRY AND POLARIMETRY OF ASTEROIDS: IMPACT ON COLLABORATION The International Workshop June 15–18, 2003 Kharkiv, Ukraine A B S T R A C T S The Organizing Committee: Lupishko Dmitrij (co-Chairman), Kiselev Nikolai (co-Chairman), Belskaya Irina, Krugly Yurij, Shevchenko Vasilij, Velichko Fiodor, Luk’yanyk Igor Kharkiv - 2003 2 Contents Belskaya I.N., Shevchenko V.G., Efimov Yu.S., Shakhovskoj N.M., Gaftonyuk N.M., Krugly Yu.N., Chiorny V.G. Opposition Polarimetry and Photometry of Asteroids 5 Bochkov V.V., Prokof’eva V.V. Spectrophotometric Observations of Asteroids in the Crimean Astrophysical Observatory 6 Butenko G., Gerashchenko O., Ivashchenko Yu., Kazantsev A., Koval’chuk G., Lokot V. Estimates of Rotation Periods of Asteroids Derived from CCD- Observations in Andrushivka Astronomical Observatory 7 Bykov O.P., L'vov V.N. Method of accuracy estimation of asteroid positional CCD observations and results its application with EPOS Software 7 Cellino A., Gil Hutton R., Di Martino M., Tedesco E.F., Bendjoya Ph. Polarimetric Observations of Asteroids with the Torino UBVRI Photopolarimeter 9 Chiorny V.G., Shevchenko V.G., Krugly Yu.N., Velichko F.P., Gaftonyuk N.M.
  • Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1

    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.
  • Asteroid Observations at Low Phase Angles. IV. Average Parameters for the New H, G1, G2 Magnitude System Vasilij G

    Asteroid Observations at Low Phase Angles. IV. Average Parameters for the New H, G1, G2 Magnitude System Vasilij G

    Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎ Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Asteroid observations at low phase angles. IV. Average parameters for the new H, G1, G2 magnitude system Vasilij G. Shevchenko a,b,n, Irina N. Belskaya a, Karri Muinonen c,d, Antti Penttilä c, Yurij N. Krugly a, Feodor P. Velichko a, Vasilij G. Chiorny a, Ivan G. Slyusarev a,b, Ninel M. Gaftonyuk e, Igor A. Tereschenko a a Institute of Astronomy of Kharkiv Karazin National University, Sumska str. 35, Kharkiv 61022, Ukraine b Department of Astronomy and Space Informatics of Kharkiv Karazin National University, Svobody sqr. 4, Kharkiv 61022, Ukraine c Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Finland d Finnish Geospatial Research Institute, P.O. Box 15, Masala, FI-02431, Finland e Crimean Astrophysical Observatory, Crimea, Simeiz 98680, Ukraine article info abstract Article history: We present new observational data for selected main-belt asteroids of different compositional types. The Received 21 January 2015 detailed magnitude–phase dependences including small phase angles (o1°) were obtained for these Received in revised form asteroids, namely: (10) Hygiea (down to the phase angle of 0.3°, C-type), (176) Iduna (0.2°, G-type), (214) 6 September 2015 Aschera (0.2°, E-type), (218) Bianca (0.3°, S-type), (250) Bettina (0.3°, M-type), (419) Aurelia (0.1°, F-type), Accepted 19 November 2015 (596) Scheila (0.2°, D-type), (635) Vundtia (0.2°, B-type), (671) Carnegia (0.2°, P-type), (717) Wisibada (0.1°, T-type), (1021) Flammario (0.6°, B-type), and (1279) Uganda (0.5°, E-type).
  • The Handbook of the British Astronomical Association

    The Handbook of the British Astronomical Association

    THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2012 Saturn’s great white spot of 2011 2011 October ISSN 0068-130-X CONTENTS CALENDAR 2012 . 2 PREFACE. 3 HIGHLIGHTS FOR 2012. 4 SKY DIARY . .. 5 VISIBILITY OF PLANETS. 6 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S. 7-8 ECLIPSES . 9-15 TIME. 16-17 EARTH AND SUN. 18-20 MOON . 21 SUN’S SELENOGRAPHIC COLONGITUDE. 22 MOONRISE AND MOONSET . 23-27 LUNAR OCCULTATIONS . 28-34 GRAZING LUNAR OCCULTATIONS. 35-36 PLANETS – EXPLANATION OF TABLES. 37 APPEARANCE OF PLANETS. 38 MERCURY. 39-40 VENUS. 41 MARS. 42-43 ASTEROIDS AND DWARF PLANETS. 44-60 JUPITER . 61-64 SATELLITES OF JUPITER . 65-79 SATURN. 80-83 SATELLITES OF SATURN . 84-87 URANUS. 88 NEPTUNE. 89 COMETS. 90-96 METEOR DIARY . 97-99 VARIABLE STARS . 100-105 Algol; λ Tauri; RZ Cassiopeiae; Mira Stars; eta Geminorum EPHEMERIDES OF DOUBLE STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 INTERNET RESOURCES. 110-111 GREEK ALPHABET. 111 ERRATA . 112 Front Cover: Saturn’s great white spot of 2011: Image taken on 2011 March 21 00:10 UT by Damian Peach using a 356mm reflector and PGR Flea3 camera from Selsey, UK. Processed with Registax and Photoshop. British Astronomical Association HANDBOOK FOR 2012 NINETY-FIRST YEAR OF PUBLICATION BURLINGTON HOUSE, PICCADILLY, LONDON, W1J 0DU Telephone 020 7734 4145 2 CALENDAR 2012 January February March April May June July August September October November December Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day of of of of of of of of of of of of of of of of of of of of of of of of of Month Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year 1 Sun.
  • The Minor Planet Bulletin Is Open to Papers on All Aspects of 6500 Kodaira (F) 9 25.5 14.8 + 5 0 Minor Planet Study

    The Minor Planet Bulletin Is Open to Papers on All Aspects of 6500 Kodaira (F) 9 25.5 14.8 + 5 0 Minor Planet Study

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 32, NUMBER 3, A.D. 2005 JULY-SEPTEMBER 45. 120 LACHESIS – A VERY SLOW ROTATOR were light-time corrected. Aspect data are listed in Table I, which also shows the (small) percentage of the lightcurve observed each Colin Bembrick night, due to the long period. Period analysis was carried out Mt Tarana Observatory using the “AVE” software (Barbera, 2004). Initial results indicated PO Box 1537, Bathurst, NSW, Australia a period close to 1.95 days and many trial phase stacks further [email protected] refined this to 1.910 days. The composite light curve is shown in Figure 1, where the assumption has been made that the two Bill Allen maxima are of approximately equal brightness. The arbitrary zero Vintage Lane Observatory phase maximum is at JD 2453077.240. 83 Vintage Lane, RD3, Blenheim, New Zealand Due to the long period, even nine nights of observations over two (Received: 17 January Revised: 12 May) weeks (less than 8 rotations) have not enabled us to cover the full phase curve. The period of 45.84 hours is the best fit to the current Minor planet 120 Lachesis appears to belong to the data. Further refinement of the period will require (probably) a group of slow rotators, with a synodic period of 45.84 ± combined effort by multiple observers – preferably at several 0.07 hours. The amplitude of the lightcurve at this longitudes. Asteroids of this size commonly have rotation rates of opposition was just over 0.2 magnitudes.