A CASE STUDY 96 4.1 Introduction 96 4.2 Thermo-X Limited: a UK Small Business 96

Total Page:16

File Type:pdf, Size:1020Kb

A CASE STUDY 96 4.1 Introduction 96 4.2 Thermo-X Limited: a UK Small Business 96 Successful technology management : cultural and organisational dimensions of MIS implementation in SMEs BALI, Rajeev Kumar Available from the Sheffield Hallam University Research Archive (SHURA) at: http://shura.shu.ac.uk/4053/ A Sheffield Hallam University thesis This thesis is protected by copyright which belongs to the author. The content must not be changed in any way or sold commercially in any format or medium without the formal permission of the author. When referring to this work, full bibliographic details including the author, title, awarding institution and date of the thesis must be given. Please visit http://shura.shu.ac.uk/4053/ and http://shura.shu.ac.uk/information.html for further details about copyright and re-use permissions. Fines are charged at 50p per hour 0 9 mak 2002 0 6 3FP 2005 OP a \ . 3 1 JAN 2008 < W L X .^ Oi\o5~lo z_ (fefCJZei^CE- cxjoy 2 5 JUN 2002 5 OO jam 2 3 OCT M °3 . ( o 5 b 1 0 DEC 2003 Key Text REFERENCE ProQuest Number: 10695704 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a com plete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest ProQuest 10695704 Published by ProQuest LLC(2017). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States C ode Microform Edition © ProQuest LLC. ProQuest LLC. 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106- 1346 Successful Technology Management: Cultural and Organisational Dimensions of MIS implementation in SMEs Rajeev Kumar Bali A thesis submitted in partial fulfilment of the requirements of Sheffield Hallam University for the degree of Doctor of Philosophy November 1999 ) Successful Technology Management: Cultural and Organisational Dimensions of MIS Implementation in SMEs RAJEEV KUMAR BALI ABSTRACT The aim of this thesis is to provide an original interpretative rationale of the role and effect of culture which may influence the development of a modern Small to Medium sized Enterprise (SME). Substantively, the research is two-fold: firstly, to examine organisational culture and, secondly, its relationship with IT implementations, specifically computer-based Management Information Systems (MIS). An extensive literature review has revealed a lack of synthesis between organisational culture and computer-based implementations, particularly in the SME environment. The research uses an approach based on ethnographic methods from qualitative research within inductivist confines. A thirty-month ethnographic study at a small engineering firm, verified and validated by triangulation techniques, has been used to form a Conceptual Model for successful MIS implementation. This new Model has been validated in several, unconnected, external organisations. The main case-study is supported by smaller studies which has provided a holistic (and therefore more realistic) view of the complexity of organisational culture. It is emphasised that achieving a change in organisational culture is a deeply political and turbulent process. Due regard must be given to managerial, cultural, organisational, human, technical, psychological and political issues. The research takes full account of these factors and discusses the importance of core competency, both from the organisation and its actors, to facilitate and realise effective cultural change. The Model proposed is one methodology for implementation in organisations with cultural and organisational difficulties. Due to the intricacies and complexity of culture, the implementation strategy is potentially a lengthy process. Contributions are made to knowledge in a number of different arenas. Firstly, a contribution is made in the area of IT change management by proposing a new Model for MIS implementation. The Model is given credibility having been verified and validated at several external organisations. Secondly, a contribution is made in the area of organisational theory as the SME focus provides this vital sector of the business community with additional, pertinent, information when undergoing IT implementations. Finally, the research contributes to knowledge in the area of research methodology as the novel combination of diverse paradigms has resulted in a new research approach for use in the SME environment. Contents Abstract Acknowledgements i List of Figures Hi List of Tables iv Abbreviations v Research papers published vi PREFACE vii 1.0 INTRODUCTION 1 1.1 Background 1 1.2 Research Hypotheses and Justification 4 1.3 Research Objectives 7 1.4 Research Methodology 8 1.5 Research Outline 8 1.6 Conclusion 11 2.0 LITERATURE REVIEW AND RESEARCH ISSUES 12 2.1 Introduction 12 2.2 Definitions 12 2.2.1 Culture 13 2.2.2 Organisational Culture 16 2.2.3 Competence and Culture 29 2.3 Attitudes, Beliefs and Values: How Organisational Culture is formed 31 2.4 Changing Organisational Culture 32 2.4.1 Lewin 34 2.4.2 Schein 37 2.4.3 Lundberg 41 2.4.4 Dyer 44 2.4.5 Gagliardi 46 2.5 Critique of the Cultural Models: Personal Perspectives on Change 48 2.6 The impact of Technology 51 2.7 A Brief History of Computing 55 2.7.1 Cultural and Organisational Changes through the years 55 2.7.2 Discussion 60 2.7.3 Impact and use of Management Information Systems (MIS) 62 2.8 Conclusions 66 3.0 RESEARCH METHODOLOGY 68 3.1 Introduction 68 3.2 Methodology Selection and Justification 68 3.3 The Qualitative-Quantitative Debate 69 3.4 Organisational Observations 72 3.5 A Question of Ethics 92 3.6 Choice of Methodology 94 3.7 Returning to the Research Question 95 3.8 Conclusion 95 4.0 ORGANISATIONAL CULTURE CHANGE: A CASE STUDY 96 4.1 Introduction 96 4.2 Thermo-X Limited: A UK Small Business 96 4.2.1 Small to Medium sized Enterprises (SMEs) 97 4.2.2 SME Management Styles 98 4.2.3 Thermo-X Management Techniques: A Sympathetic View 99 4.2.4 Thermo-X: Defining the Vision 100 4.2.5 Thermo-X Timeline: An Overview of Change 101 4.3 Thermo-X Limited: Inside the Organisation 104 4.3.1 Geographical and Physical Layout 107 4.3.2 IT and IS Environment 111 4.3.3 Sales Order and Works Order Processing 114 4.3.4 The Quality Perspective 117 4.3.5 The Calibration and Service Departments 122 4.3.6 The Accounts Department 123 4.3.7 Technology as a catalyst for change 124 4.4 Organisational Structure and Organisational Initiatives 138 4.4.1 The Thermo-X Exhibition 139 4.4.2 NAMAS Accreditation 140 4.4.3 Investors In People (IIP) 141 4.4.4 Modem Apprenticeships 142 4.5 Thermo-X Organisational and Cultural Issues 142 4.6 Changing the Thermo-X Organisational Culture 147 4.6.1 Diagnostic Activities 151 4.6.2 Team-Building and Process Consultation 153 4.6.3 Introducing more efficient Technology 155 4.6.4 Extending existing Information Systems 160 4.6.5 Restructuring work, roles and tasks 162 4.7 Formation of the model: feedback from colleagues 164 4.8 The new Thermo-X organisational culture and structure 164 4.9 Conclusion 166 5.0 CONCEPTUAL MODEL FOR MIS IMPLEMENTATION 169 5.1 Introduction 169 5.2 The Thermo-X Case Study: Implications, Theory and Practice 169 5.3 The Justification for a New Model 176 5.4 The Formulation of the Model 180 5.5 The Role of Soft Systems Methodology (SSM) 180 5.6 Building Blocks of the Model 186 5.7 MIS-induced Culture Change: MISCO Conceptual Model 190 5.7.1 Recognition 191 5.7.2 Penetrating the Cultural Barrier 192 5.7.3 Change from within: A blueprint for success 194 5.7.4 The Road to Acceptance 200 5.7.5 Stability 201 5.8 Conclusion 202 6.0 CASE STUDIES: VALIDATING THE MISCO MODEL 204 6.1 Introduction 204 6.2 Testing the Wider Applicability of the Model 204 6.2.1 Fact-finding 205 6.2.2 Literature Search 206 6.2.3 Organisation Selection: Rationale and Justification 206 6.3 Structure of the Case Study Investigations 207 6.4 Case Studies 209 6.4.1 Case Study: Company A 209 6.4.2 Case Study: Company B 215 6.4.3 Case Study: Company C 221 6.4.4 Case Study: Company D 231 6.5 MISCO Framework Validation 237 6.6 Discussion 241 6.7 Revisiting the MISCO Conceptual Model 243 6.8 Conclusion 247 7.0 CONCLUSION 248 7.1 Introduction 248 7.2 Reflecting on the Research Aim 248 7.3 MIS Implementations: The Complexity of Culture 249 7.4 Originality 253 7.5 Contribution 255 7.6 Impact of the Research Experience and the MISCO Model 256 7.7 Areas for Further Research 258 LIST OF REFERENCES 260 BIBLIOGRAPHY 266 APPENDICES Appendix A: Conceptual Model, Original Version, Full Page Conceptual Model, Revised Version, Full Page Interview Schedule Conceptual Model Notes Geographical Location of Organisations Appendix B: Interview Schedules, Completed Originals Appendix C: Analysis and Design Diagrams Thermo-X: SSADM Schematics Thermo-X: SSM Schematics Appendix D: Thermo-X documents Appendix E: Research Papers published Appendix F: MISCO Model: A User Guide for SMEs Acknowledgements The very presence of this thesis means that a long-standing ambition has finally been realised. This document pieces together the disjecta membra of numerous references, interviews, journals, books, seminars, conferences, transcripts, trial-projects and countless experiences and thoughts, both mine and those of external contributors. When originally seeking suitable research opportunities, I was mindful not to chase another qualification in lieu of industrial experience.
Recommended publications
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 2, A.D. 2011 APRIL-JUNE 71. LIGHTCURVES OF 10452 ZUEV, (14657) 1998 YU27, AND (15700) 1987 QD Gary A. Vander Haagen Stonegate Observatory, 825 Stonegate Road Ann Arbor, MI 48103 [email protected] (Received: 28 October) Lightcurve observations and analysis revealed the following periods and amplitudes for three asteroids: 10452 Zuev, 9.724 ± 0.002 h, 0.38 ± 0.03 mag; (14657) 1998 YU27, 15.43 ± 0.03 h, 0.21 ± 0.05 mag; and (15700) 1987 QD, 9.71 ± 0.02 h, 0.16 ± 0.05 mag. Photometric data of three asteroids were collected using a 0.43- meter PlaneWave f/6.8 corrected Dall-Kirkham astrograph, a SBIG ST-10XME camera, and V-filter at Stonegate Observatory. The camera was binned 2x2 with a resulting image scale of 0.95 arc- seconds per pixel. Image exposures were 120 seconds at –15C. Candidates for analysis were selected using the MPO2011 Asteroid Viewing Guide and all photometric data were obtained and analyzed using MPO Canopus (Bdw Publishing, 2010). Published asteroid lightcurve data were reviewed in the Asteroid Lightcurve Database (LCDB; Warner et al., 2009). The magnitudes in the plots (Y-axis) are not sky (catalog) values but differentials from the average sky magnitude of the set of comparisons. The value in the Y-axis label, “alpha”, is the solar phase angle at the time of the first set of observations. All data were corrected to this phase angle using G = 0.15, unless otherwise stated.
    [Show full text]
  • The British Astronomical Association Handbook 2014
    THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2015 2014 October ISSN 0068–130–X CONTENTS CALENDAR 2015 . 2 PREFACE . 3 HIGHLIGHTS FOR 2015 . 4 SKY DIARY . .. 5 VISIBILITY OF PLANETS . 6 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S . 7-8 ECLIPSES . 9-14 TIME . 15-16 EARTH AND SUN . 17-19 LUNAR LIBRATION . 20 MOON . 21 MOONRISE AND MOONSET . 21-25 SUN’S SELENOGRAPHIC COLONGITUDE . 26 LUNAR OCCULTATIONS . 27-33 GRAZING LUNAR OCCULTATIONS . 34-35 APPEARANCE OF PLANETS . 36 MERCURY . 37-38 VENUS . 39 MARS . 40-41 ASTEROIDS . 42 ASTEROID EPHEMERIDES . 43-47 ASTEROID OCCULTATIONS .. 48-50 NEO CLOSE APPROACHES TO EARTH . 51 ASTEROIDS: FAVOURABLE OBSERVING OPPORTUNITIES . 52-54 JUPITER . 55-59 SATELLITES OF JUPITER . 59-63 JUPITER ECLIPSES, OCCULTATIONS AND TRANSITS . 64-73 SATURN . 74-77 SATELLITES OF SATURN . 78-81 URANUS . 82 NEPTUNE . 83 TRANS–NEPTUNIAN & SCATTERED DISK OBJECTS . 84 DWARF PLANETS . 85-88 COMETS . 89-96 METEOR DIARY . 97-99 VARIABLE STARS (RZ Cassiopeiae; Algol; λ Tauri) . 100-101 MIRA STARS . 102 VARIABLE STAR OF THE YEAR (V Bootis) . 103-105 EPHEMERIDES OF DOUBLE STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 PLANETS – EXPLANATION OF TABLES . 110 ELEMENTS OF PLANETARY ORBITS . 111 ASTRONOMICAL AND PHYSICAL CONSTANTS . 111-112 INTERNET RESOURCES . 113-114 GREEK ALPHABET . 115 ACKNOWLEDGEMENTS . 116 ERRATA . 116 Front Cover: The Moon at perigee and apogee – highlighting the clear size difference when the Moon is closest and farthest away from the Earth. Perigee on 2009/11/08 at 23:24UT, distance
    [Show full text]
  • 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) ..................
    [Show full text]
  • Inversion of HIPPARCOS and Gaia Photometric Data for Asteroids A
    Inversion of HIPPARCOS and Gaia photometric data for asteroids A. Cellino, D. Hestroffer, X.-P. Lu, K. Muinonen, P. Tanga To cite this version: A. Cellino, D. Hestroffer, X.-P. Lu, K. Muinonen, P. Tanga. Inversion of HIPPARCOS andGaia photometric data for asteroids. Astronomy and Astrophysics - A&A, EDP Sciences, 2019, 631, pp.A67. 10.1051/0004-6361/201936059. hal-03137882 HAL Id: hal-03137882 https://hal.archives-ouvertes.fr/hal-03137882 Submitted on 11 Feb 2021 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. A&A 631, A67 (2019) https://doi.org/10.1051/0004-6361/201936059 Astronomy & © ESO 2019 Astrophysics Inversion of HIPPARCOS and Gaia photometric data for asteroids Asteroid rotational properties from sparse photometric data A. Cellino1, D. Hestroffer2, X.-P. Lu3, K. Muinonen4,5, and P. Tanga6 1 INAF, Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese, Italy e-mail: [email protected] 2 IMCCE, Observatoire de Paris, Université PSL, CNRS, Sorbonne University, Université Lille, 75014 Paris, France e-mail: [email protected] 3 Macau University of Science and Technology, Macau, PR China e-mail: [email protected] 4 Department of Physics, University of Helsinki, Gustaf Hällströmin katu 2a, PO Box 64, 00014 U.
    [Show full text]
  • TRAPPIST Asteroid Lightcurves
    http://lib.uliege.ac.be http://matheo.uliege.be TRAPPIST asteroid lightcurves Auteur : Ferrais, Marin Promoteur(s) : Jehin, Emmanuel Faculté : Faculté des Sciences Diplôme : Master en sciences spatiales, à finalité approfondie Année académique : 2017-2018 URI/URL : www.trappist.ulg.ac.be; http://hdl.handle.net/2268.2/5023 Avertissement à l'attention des usagers : Tous les documents placés en accès ouvert sur le site le site MatheO sont protégés par le droit d'auteur. Conformément aux principes énoncés par la "Budapest Open Access Initiative"(BOAI, 2002), l'utilisateur du site peut lire, télécharger, copier, transmettre, imprimer, chercher ou faire un lien vers le texte intégral de ces documents, les disséquer pour les indexer, s'en servir de données pour un logiciel, ou s'en servir à toute autre fin légale (ou prévue par la réglementation relative au droit d'auteur). Toute utilisation du document à des fins commerciales est strictement interdite. Par ailleurs, l'utilisateur s'engage à respecter les droits moraux de l'auteur, principalement le droit à l'intégrité de l'oeuvre et le droit de paternité et ce dans toute utilisation que l'utilisateur entreprend. Ainsi, à titre d'exemple, lorsqu'il reproduira un document par extrait ou dans son intégralité, l'utilisateur citera de manière complète les sources telles que mentionnées ci-dessus. Toute utilisation non explicitement autorisée ci-avant (telle que par exemple, la modification du document ou son résumé) nécessite l'autorisation préalable et expresse des auteurs ou de leurs ayants droit. UNIVERSITY OF LIÈGE FACULTY OF SCIENCES DEPARTMENT OF ASTROPHYSICS,GEOPHYSICS AND OCEANOGRAPHY MASTER THESIS TRAPPIST ASTEROID LIGHTCURVES Composite lightcurve of (20) Massalia A thesis presented for the degree of Master in Space Sciences by MARIN FERRAIS Under the supervision of Emmanuël Jehin Academic Year 2017 − 2018 Contents Contents 2 1 Introduction 5 2 About asteroids 7 2.1 Introduction...........................................
    [Show full text]
  • The Minor Planet Bulletin 40 (2013) 207
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 40, NUMBER 4, A.D. 2013 OCTOBER-DECEMBER 187. LIGHTCURVE ANALYSIS OF EXTREMELY CLOSE Canopus package (Bdw Publishing). NEAR-EARTH ASTEROID – 2012 DA14 Asteroid 2012 DA14 is a near-Earth object (Aten category, q = Leonid Elenin 0.8289, a = 0.9103, e = 0.0894, i = 11.6081). Before the current Keldysh Institute of Applied Mathematics RAS close approach, 2012 DA14 had orbital elements within the Apollo ISON-NM Observatory (MPC H15), ISON category (q = 0.8894, a = 1.0018, e = 0.1081, i = 10.3372). 140007, Lyubertsy, Moscow region, 8th March str., 47-17 Parameters of the orbit make this asteroid an interesting target for a [email protected] possible space mission. Asteroid 202 DA14 was discovered on Feb 23 2012 by the La Sagra Sky Survey, LSSS (MPC code J75). Igor Molotov Keldysh Institute of Applied Mathematics RAS An extremely close approach to the Earth (0.00022 AU or ~34 000 ISON km) occurred 2013 Feb 15.80903. We observed this asteroid after its close approach, 2013 Feb 16, from 02:11:35 UT to 12:17:43 UT (Received: 20 February*) (Table1). Our total observational interval was 10 h 16 min, i.e. ~108% of the rotation period. In this paper we present one of the first lightcurves of near-Earth asteroid 2012 DA14. This is a very interesting near-Earth asteroid, which approached the Earth at a very close distance on Feb. 15 2013. From our UT Δ r phase mag measurements we find a rotational period of 9.485 ± 02:11:35 0.0011 0.988 73.5 11.8 0.144 h with an amplitude of 1.79 mag.
    [Show full text]
  • 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).
    [Show full text]
  • Encyclopedia of Astrology Nicholas Devore
    Encyclopedia of Astrology Nicholas deVore The Philosophical Library, June 1947. Retyped with additional 'Apolo notes' and reconstructed tables by Philip Graves. By kind permission of current publisher David Roell of Astrology Classic A B C D E F G H I J K L M N O P Q R S T U V W Y Z A Accidental Ascendant. A device employed by Evangeline Adams whereby to draw Horary interpretations from a natal Figure. In applying this method one determines the Ascendant for the moment the question is propounded, and rotates the Figure until this degree occupies the East point. Accidental Dignity. See 'Dignities' Acronycal. Said of the rising after sunset, or setting before sunrise, of a planet that is in opposition to the Sun, hence in a favorable position for astronomical observation. Acronycal place. The degree the planet will occupy when it is in opposition to the Sun. Active Influence. That which results from an aspect between two or more astrological factors or sensitive points, thereby producing the action that can materialize in an event. Adept. One who has attained to proficiency in any art or science. It may be said of a skilled astrologer who, through spiritual development, has attained to superior powers and transcendental knowledge concerning the origins and destiny of mankind. Formerly said of an alchemist who had attained the 'great secret' - presumably that concerning the 'transmutation of metals'. Its modern application is to the transmutation of unfavorable cosmic stimuli and the baser emotions into nobler impulses - thereby achieving the triumph of mind over matter, and of the spiritual over the carnal.
    [Show full text]
  • XXXIII. the Spin Rate of M-Type Asteroids?
    ASTRONOMY & ASTROPHYSICS JULY 1998,PAGE55 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 131, 55–62 (1998) Physical studies of asteroids XXXIII. The spin rate of M-type asteroids? C.-I. Lagerkvist1,I.Belskaya2, A. Erikson3, V. Schevchenko2, S. Mottola3, V. Chiorny2, P. Magnusson1, A. Nathues3, and J. Piironen4 1 Astronomiska Observatoriet, Box 515, S-752 20 Uppsala, Sverige 2 Astronomical Observatory, 35 Sumskaya Str., 310022 Kharkiv, Ukraine 3 Institute of Planetary Exploration, DLR, Rudower Chaussee 5, 12489 Berlin, Germany 4 Observatory, P.O. Box 14, FIN–00014, University of Helsinki, Finland Received December 12, 1997; accepted January 30, 1998 Abstract. The results from photometric lightcurve obser- number of M-type asteroids with known rotation periods. vations of nine M-type asteroids are presented. New rota- In this paper we present observations of nine M-type as- tion periods were determined for 6 asteroids: 217 Eudora teroids, resulting in new determinations of spin rates for (12.54 h), 322 Phaeo (17.56 h), 572 Rebekka (5.65 h), six of these. This gives an increase of more than 15% of 757 Portland (6.58 h), 857 Glasenappia (8.23 h) and 872 the known spin rates of asteroids of taxonomic type M. Holda (7.20 h). B − V colour measurements of seventeen In order to increase the known population of M-type as- previously unclassified asteroids add seven asteroids to the teroids we have determined B − V colour indices for 17 known M-type population. asteroids with moderate albedos. The second problem is An excess of fast rotators among M-type asteroids the inconsistent classification of some asteroids between compared to asteroids of other taxonomic types is evident.
    [Show full text]
  • Rosamunde on Three Nights in 1989 and Obtained a Period of 5489 Oberkochen
    92 ASTEROIDS OBSERVED FROM CS3: 607 Jenny. Brian Warner observed this asteroid in 2002 and 2007. 2013 OCTOBER - DECEMBER His 2007 observations resulted in a rotational period of 8.524 h (Warner 2003). Upon re-measuring the 2002 images, he revised Robert D. Stephens that rotational period to be 8.526 h (Warner 2011). Pierre Antonini Center for Solar System Studies (CS3) / MoreData! (Behrend 2013) observed Jenny in 2007 finding a period of 8.5221 11355 Mount Johnson Ct., Rancho Cucamonga, CA 91737 USA h. The period found this year is in good agreement with those [email protected] results. (Received: 7 January Revised: 13 January) 734 Benda. This asteroid was observed by Rene Roy for three nights in March 2004 (Behrend 2013) who reported the rotational period to be 7.11 h. Buchheim (2009) observed it on 10 nights in Results from CCD photometric observations are reported October 2007 reporting a period of 7.106 h. This result is in good for eleven asteroids. These data were obtained from the agreement with those works. Center for Solar System Studies (CS3) during 2013 October to December. 804 Hispania. Hispania has been observed numerous times over the years. Harris and Young (Harris 1983) found a period of 14.851 h, Axel Martin (Behrend 2013) found a period of 14.844 h, The Center for Solar System Studies (CS3, MPC U81) started and the author (Stephens 2004) found a period of 14.845 h. The operations in late 2012. Its participants have a history of studying rotational period found this year is in good agreement with those asteroid families such as Jovian Trojans, Hungarias or NEOs.
    [Show full text]
  • The Minor Planet Bulletin 34, 113-119
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 4, A.D. 2011 OCTOBER-DECEMBER 179. THE LIGHTCURVE ANALYSIS OF FIVE ASTEROIDS 933 Susi. Data were collected from 2011 Mar 7 to 9. A period of 4.621 ± 0.002 h was determined with an amplitude of 0.52 ± 0.01 Li Bin mag. The results are consistent with that reported by Higgins Purple Mountain Observatories, Nanjing, CHINA (2011). Graduate School of Chinese Academy of Sciences 2903 Zhuhai. This S-type asteroid belonging to the Maria family was worked by Alvarez et al. (2004), who were looking for Zhao Haibin possible correlations between rotational periods, amplitudes, and Purple Mountain Observatories, Nanjing, CHINA sizes. Based on their observations, they reported a period of 6.152 h. Our new observations on two nights (2010 Dec 28 and 29) show Yao Jingshen a period of 5.27 ± 0.01 h with amplitude 0.55 ± 0.02 mag. The data Purple Mountain Observatories, Nanjing, CHINA were checked against the period of 6.152 h reported by Alvarez but this produced a very unconvincing fit. (Received: 25 May Revised: 12 August) Acknowledgements Photometric data for five asteroids were collected at the We wish to thank the support by the National Natural Science Xuyi Observatory: 121 Hermione, 620 Drakonia, 877 Foundation of China (Grant Nos. 10503013 and 10933004), and Walkure, 933 Susi, and 2903 Zhuhai. A new period of the Minor Plant Foundation of Purple Mountain Observatory for 5.27 h is reported for 2903 Zhuhai.
    [Show full text]
  • 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.
    [Show full text]