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173 produkter
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It is well known, that the Sun as central star of our solar system gravitationally controls the orbits of planets and minor bodies. Much less known is the domain of plasma fields and charged particles, however, in which the Sun with a radius of less than 0.7 Million km governs the heliosphere out to about 15 Billion km, a distance about 20 000 times larger in radius or nearly 1013 times bigger in volume. What forces activates the Sun to maintain this power? Coronal Mass Ejections (CMEs) and their descendants are the troops serving the Sun during high solar activity periods. This volume offers a comprehensive and integrated overview of our present knowledge and understanding of Coronal Mass Ejections (CMEs) and their descendants, Interplanetary CMEs (ICMEs). It results from a series of workshops held between 2000 and 2004. An international team of about sixty experimenters involved e.g. in the SOHO, ULYSSES, VOYAGER, PIONEER, HELIOS, WIND, IMP, and ACE missions, ground observers, and theoreticians worked jointly on interpreting the observations and developing new models for CME initiations, development, and interplanetary propagation.The book is intended to provide scientists active in space physics research a with an up-to-date status of the current understanding of CMEs and ICMEs and their effects in the heliosphere, and also to serve the advanced graduate student with introductory material on this active field of research.
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2 With a global average irradiance of 342 W/m , the Sun is by far the largest source of energy for planet Earth. In comparison, the internal energy produced by Earth 2 itself is only about 0. 087 W/m (Pollack et al. , 1993), which in turn is 3. 5 times 2 larger than the 0. 025 W/m of heat produced by the burning of fossil fuels. About 31% (31 units) of the solar energy which arrives at the top of the - mosphere is re?ected back to space by scattering from clouds, aerosols, and the Earth’s surface. Almost 20 units of solar radiation are absorbed in the atmosphere. The remaining 49 units are absorbed at the surface. Evaporation of water at the Earth’s surface consumes 23 units, and 7 units are transferred to the atmosphere by heat conduction. On balance 19 units are lost from the Earth’s surface as infrared radiation, however consisting of 114 going upward and 95 returning from the - mosphere to the Earth’s surface (see also Rosenfeld, 2006). There is thus a sixfold recycling of energy. This is the greenhouse effect, established by the presence of watervaporandofothergreenhousegases,CO ,CH ,N O,andCFCs,intheatmo- 2 4 2 sphere. Due to human activities the latter have been increasing in the atmosphere, 2 causing climate warming through an energy imbalance of 2. 5–3 W/m , more than 100 times larger than the heat released into the atmosphere by the burning of fossil fuels.
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The SOHO and Cluster missions form a single ESA cornerstone. Yet they observe verydifferentregionsinoursolarsystem:thesolaratmosphereononehandandthe Earth’s magnetosphere on the other. At the same time the Ulysses mission provides observations in the third dimension of the heliosphere, and many others add to the picture from the Lagrangian point L1 to the edge of the heliosphere. It was our aim to tie these observations together in addressing the topic of Solar Dynamics and its Effects on the Heliosphere and Earth with a workshop at the International Space Science Institute (ISSI), under the auspices of the International Living With a Star (ILWS) program. It started out with an assessment and description of the reasons for solar dynamics and how it couples into the heliosphere. The three subsequent sections were each devoted to following one chain of events from the Sun all the way to the Earth’s magnetosphere and ionosphere: The normal solar wind chain, the chain associated with coronal mass ejections, and the solar energetic particles chain. The ?nal section was devoted to common physical processes occurring both at the Sun and in the magnetosphere such as reconnection, shock acceleration, dipolarisation of magnetic ?eld, and others. This volume is the result of an ISSI Workshop held in April 2005. An international group of about forty experimenters, ground-based observers, and theoreticians was invited to present and debate their data, models, and theories in an informal setting.
Composition of Matter
Symposium honouring Johannes Geiss on the occasion of his 80th birthday
Inbunden, Engelska, 2007
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we thank Johannes for providing us with the occasion to gather in his name and for shaping and supporting the careers of so many of us. May 2007 R. von Steiger, G. Gloeckler, G.M. Mason Space Sci Rev (2007) 130: 3–4 DOI 10.1007/s11214-007-9240-0 Acknowledgement Published online: 21 July 2007 © Springer Science+Business Media B.V. 2007 Early in 2006, Edward C. Stone, Principal Investigator of NASA’s Advanced Composition Explorer (ACE); Len A. Fisk, Chair of the Space Studies Board of the US National Research Council; and the Directorate of the International Space Science Institute (ISSI), Roger M. Bonnet, Andre Balogh and Rudolf von Steiger, agreed to hold a joint ACE/ISSI Symposium on the “Composition of Matter”, at the occasion of my 80th birthday. I feel deeply honoured by this exceptional distinction and was thrilled to participate, because for more than 50 years my research has been centred around measurements of the composition of matter of various origins, reaching—in geocentric coordinates—from deep-sea sediments to the limits of solar in uence, where comets come from and where the solar wind meets the interstellar medium. The symposium at Grindelwald, beautifully located at the foot of the Bernese Alps, was organised by Ruedi von Steiger, Silvia Wenger and Barbara Gerber, who created the special atmosphere for which ISSI meetings have become known.
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Given the fundamental importance of and universal interest in whether extraterrestrial life has developed or could eventually develop in our solar system and beyond, it is vital that an examination of planetary habitability go beyond simple assumptions such as, "Where there is water, there is life". This book has resulted from a workshop at the International Space Science Institute (ISSI) in Bern, Switzerland which brought together planetary geologists, geophysicists, atmospheric scientists and biologists to discuss the multi-faceted problem of how the habitability of a planet co-evolves with the geology of the surface and interior, the atmosphere, and the magnetosphere.Each of the six chapters have been written by authors with a range of expertise so that each chapter is itself multi-disciplinary, comprehensive, and accessible to scientists in all disciplines. These chapters delve into what life needs to exist and ultimately to thrive, the early environments of the young terrestrial planets, the role of volatiles in habitability, currently habitable (but possibly not inhabited) geologic environments, the connection between a planet’s inner workings and the habitability of its surface, and the effects on planetary atmospheres of solar evolution and the presence or absence of a magnetosphere.This book serves as an ideal reference for those planning missions that will hunt for biomarkers (especially on Mars), for biologists and geoscientists seeking the other side of the story, and for researchers and upper level students interested in an in-depth review of the geologic evolution of terrestrial planets, from their cores to their magnetospheres, and how that evolution shapes the habitability of the planetary surface.
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The search for life outside the Earth has been one of the biggest quests of mankind. We have reached a level in technology that allows the first steps towards a scientific investigation. The aim of this workshop was to take an interdisciplinary look at the signatures that would be indicative for past or present life on another planet, to compare them to biosignatures on Earth, and to discuss state-of-the-art in-situ instruments that are envisioned to search for these signatures in the exploration of the solar system as well as concepts for the search for habitable planets around other stars.
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Mercury, the planet closest to the Sun, is different in several respects from the other three terrestrial planets. In appearance, it resembles the heavily cratered surface of the Moon, but its density is high, it has a magnetic field and magnetosphere, but no atmosphere or ionosphere. This book reviews the progress made in Mercury studies since the flybys by Mariner 10 in 1974-75, based on the continued research using the Mariner 10 archive, on observations from Earth, and on increasingly realistic models of its interior evolution.
Origin and Early Evolution of Comet Nuclei
Workshop honouring Johannes Geiss on the occasion of his 80th birthday
Inbunden, Engelska, 2008
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Comet nuclei are the most primitive bodies in the solar system. They have been created far away from the early Sun and it is supposed that their material has been altered the least since their formation. The workshop was bringing together representatives of several scientific communities in the fields of interstellar clouds, star-forming regions, the solar nebula, and comets. The intent was to formulate the current understanding and interconnectivity of the various source regions of comet nuclei and their associated compositions and orbital characteristics.The goal was to better understand the survival of cometary materials (grains, molecules, free radicals, and atoms) from extrasolar sources (circumstellar shells and molecular clouds), their modifications in the solar nebula, and the effects of their properties on the formation and early physical and thermal evolution of the macroscopic bodies, the comet nuclei, in the various subnebulae. Closely associated is their transport into the outer solar system, the Kuiper belt and Oort cloud. The distinction between direct measurements, in situ or by remote sensing, of cometary material properties and properties derived from indirect means, deduced from laboratory studies and theoretical deductions, was emphasized with the aim to guide future investigations. The book is intended to serve as guide for researchers and graduate students working in the field of planetology and solar system exploration. It should also help to influence the planning of scientific strategies for the encounter of the Rosetta spacecraft with Comet Churyumov-Gerasimenko.
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Roger-Maurice Bonnet*Michel Blanc Originally published in the journal Space Science Reviews, Volume 137, Nos 1-4. DOI: 10. 1007/s11214-008-9418-0 (c) Springer Science+Business Media B. V. 2008 "Planetary Atmospheric Electricity" is the rst publication of its kind in the Space Science Series of ISSI. It is the result of a new and successful joint venture between ISSI and Eu- planet. Europlanet is a network of over 110 European and U. S. laboratories deeply involved in the development of planetary sciences and support to the European planetary space exp- ration programme. In 2004, the Europlanet consortium obtained support from the European Commission to strengthen the planetary science community worldwide, and to amplify the scienti c output, impact and visibility of the European space programme, essentially the - ropean Space Agency's Horizon 2000, Cosmic Vision programmes and their successors. Its presentcontractwiththeCommissionextendsfrom2005to2008,andincludes7networking activities, including discipline-based working groups covering the main areas of planetary sciences.A new contract with the Commission, presently under negotiation, will extend - roplanet's activities into the period 2009-2012. With the broad community connection made through its Discipline Working Groups and other activities, Europlanet offers an ideal base from which to identify new elds of research for planetary sciences and to stimulate coll- orative work among its member laboratories.
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Andrew F. Nagy Originally published in the journal Space Science Reviews, Volume 139, Nos 1–4. DOI: 10. 1007/s11214-008-9353-0 © Springer Science+Business Media B. V. 2008 Keywords Aeronomy The term “aeronomy” has been used widely for many decades, but its origin has mostly been lost over the years. It was introduced by Sydney Chapman in a Letter to the Editor, entitled “Some Thoughts on Nomenclature”, in Nature in 1946 (Chapman 1946). In that letter he suggested that aeronomy should replace meteorology, writing that the word “meteor is now irrelevant and misleading”. This proposal was apparently not received with much support so in a short note in Weather in 1953 Chapman (1953)wrote: “If, despite its obvious convenience of brevity in itself and its derivatives, it does not commend itself to aeronomers, I think there is a case for modifying my proposal so that instead of the word being used to signify the study of the atmosphere in general, it should be adopted with the restricted sense of the science of the upper atmosphere, for which there is no convenient short word. ” In a chapter, he wrote in a 1960 book (Chapman 1960), he give his nal and de nitive de nition, by stating that “Aeronomy is the science of the upper region of the atmosphere, where dissociation and ionization are important”. The Workshop on “Comparative Aeronomy” was held at ISSI during the week of June 25–29, 2007.
Heliosphere in the Local Interstellar Medium
Proceedings of the First ISSI Workshop 6–10 November 1995, Bern, Switzerland
Inbunden, Engelska, 1996
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This volume gives a comprehensive and integrated overview of current knowledge about the local interstellar medium (LISM) surrounding our heliosphere (HS). It is the result of the first workshop at ISSI, where both space physicists and astronomers presented and discussed their views on the density, velocity, temperature, composition, and morphology of the LISM and how it interacts with the HS. Thevolume is a combination of data obtained by remote UV, EUV, and X-ray observations outside the HS with in situ observations of interstellar atoms, ions, and dust inside the HS. It thus demonstrates a new synergy between these two communities. The book is intended to provide active researchers in space physics and in astronomy with an up-to-date status report of its topic, and also to furnish the advanced graduate student with introductory material into the field.
Cosmic Rays in the Heliosphere
Volume Resulting from an ISSI Workshop 17–20 September 1996 and 10–14 March 1997, Bern, Switzerland
Inbunden, Engelska, 1998
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This text looks at cosmic rays in the heliosphere. It is the result of a workshop at ISSI, where experimental space physicists as well as theorists presented and discussed their views on the behaviour of cosmic rays during the currently prevalent solar minimum conditions, when the heliosphere has a well-ordered and relatively simple configuration. An array of spacecraft - Ulysses, Pioneer, Voyager, IMP-8, Wind, - in conjunction with ever more sophisticated numerical models made this possible by giving a clear view of the three-dimensional heliosphere at solar minimum. The status of the field is first presented in a series of introductory papers; these are followed by four Working Group reports attempting to synthesize this knowledge, make progress in our understanding, and point out directions of future research. A summary of the parameters used in cosmic ray modulation and an epilogue on conditions and consequences expected at the upcoming solar maximum conclude the volume.
Primordial Nuclei and Their Galactic Evolution
Proceedings of an ISSI Workshop, 6-10 May 1997, Bern, Switzerland
Inbunden, Engelska, 1998
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This volume gives an overview of knowledge about the light nuclei created in the Hot Early Universe: H, D, 3He, 4He, and 7Li. It combines observational and theoretical results on the early Universe, the distant galaxies, our Milky Way, the local interstellar cloud, and the solar nebula. The implications for cosmology, galactic and stellar evolution, dark matter research etc. are outlined and directions of future research are indicated.
Solar Composition and its Evolution — from Core to Corona
Proceedings of an ISSI Workshop 26–30 January 1998, Bern, Switzerland
Inbunden, Engelska, 1998
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This volume contains the reviews and contributions on solar composition and its evolution as presented at an ISSI Workshop. Topics include the structures that make up its atmosphere, and solar-wind and other, more energetic, particle streams, giving clues for understanding mass-transport, separation and heating mechanisms in particular. The book is intended to provide both active researchers and advanced graduate students with a comprehensive overview on solar composition.
Magnetospheric Plasma Sources and Losses
Final Report of the ISSI Study Project on Source and Loss Processes
Inbunden, Engelska, 1999
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This sixth volume in the ISSI Space Sciences series is the outcome of a process of carrying out the ISSI study project on source and loss processes of magnetospheric plasma. The goal has been to give an authoritative overview of all aspects of the topic in a well-organized form, for active researchers in the field and for young scientists who are starting their research in space physics. In order to represent the full diversity of experience and perspective that exists in the science community, some 50 leading scientists from all over the world were invited to participate in the project and contribute to the text. This book should be of interest to researchers and graduate students in space physics and astrophysics.
Corotating Interaction Regions
Proceedings of an ISSI Workshop 6–13 June 1998, Bern, Switzerland
Inbunden, Engelska, 2000
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This volume gives a comprehensive and integrated overview of current knowledge and understanding of corotating interaction regions (CIRs) in the solar wind at the beginning of the 21st century. It is the result of a workshop at ISSI, where space scientists involved in the Ulysses, Pioneer, Voyager, IMP-8, Wind, and SOHO missions exchanged their data and interpretations with theorists in the fields of solar and heliospheric physics. The book provides a broad synthesis of current understanding of CIRs, which form at the interface between the fast solar wind originating in the northern and southern coronal holes and the slow solar wind that originates near and within coronal streamers surrounding the heliomagnetic equator. CIRs are the dominant structure in the heliosphere near and beyond Earth on the declining phase and near the minimum of the 11-year solar activity cycle. Particles energized at the shocks that bound CIRs at heliospheric distances beyond the orbit of Earth are the dominant energetic particle population observed in the outer heliosphere at these times.Papers included in this volume cover the subject of CIRs from their dissipation in the outer hemisphere, and include discussions of complexities associated with their evolution with distance from the Sun, their three-dimensional structure, and the myriad effects that CIRs have on energetic particles throughout the heliosphere. The book is intended to provide scientists active in space physics research with an up-to-date status report on current understanding of CIRs and their effects in the heliosphere, and also to serve the advanced graduate student with introductory material on this active field of research.
Composition and Origin of Cometary Materials
Proceedings of an ISSI Workshop, 14–18 September 1998, Bern, Switzerland
Inbunden, Engelska, 2000
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Comet nuclei are the most primitive bodies in the solar system. They have been created far away from the early Sun and their material properties have been altered the least since their formation. Thus, the composition and structure of comet nuclei provide the best information about the chemical and thermodynamic conditions in the nebula from which our solar system formed. In this volume, cometary experts review a broad spectrum of ideas and conclusions based on in situ measurement of Comet Halley and remote sensing observations of the recent bright Comets Hale-Bopp and Hyakutake. The chemical character of comet nuclei suggests many close similarities with the composition of interstellar clouds. It also suggests material mixing from the inner solar nebula and challenges the importance of the accretion shock in the outer nebula. The book is intended to serve as a guide for researchers and graduate students working in the field of planetology and solar system exploration. Several special indexes focus the reader's attention to detailed results and discussions.It concludes with recommendations for laboratory investigations and for advanced modelling of comets, the solar nebula, and the collapse of interstellar clouds.
From Dust to Terrestrial Planets
Proceedings of an ISSI Workshop, 15–19 February 1999, Bern, Switzerland
Inbunden, Engelska, 2000
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This volume gives a comprehensive and integrated overview of current knowledge and understanding of the processes occurring during the first 100 million years of the solar system, when the terrestrial planets formed. It is the result of a workshop at ISSI, where planetary scientists, astrophysicists, and cosmochemists exchanged their data, interpretations, and ideas on theoretical models. The book provides a broad synthesis of ground- and spaced-based observations, laboratory experiments, numerical simulations, and theoretical considerations dealing with the collapse of molecular clouds to proto-planetary disks and their subsequent evolution. Emphasis is given to the evolution of the disk and the relevant timescales characterizing the underlying (magnetohydro)dynamical, (astro)physical, and (geo)chemical processes responsible for the current distribution and composition of the material in the solar system. Papers in this volume cover the topics of proto-solar disk formation and evolution, formation of the most original compounds and first solids and their subsequent accretion into planetesimals, planetary embryos, and ultimately into planets.The book is intended to provide scientists in space physics and geophysical research with an up-to-date status report on current understanding of terrestrial planet formation, and also to serve the advanced graduate student with introductory material on this active field of research.
Del 10 - Space Sciences Series of ISSI
Cosmic Rays and Earth
Proceedings of an ISSI Workshop 21–26 March 1999, Bern, Switzerland
Inbunden, Engelska, 2000
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This volume, the proceedings of an ISSI workshop 21-26 March 1999, Bern, Switzerland summarizes the results from the detection of cosmic rays at the surface and in the lower atmosphere of Earth during the 50 years since the invention of the neutron monitor by John A. Simpson in 1948. The properties of solar and galactic cosmic rays in the heliosphere, such as Forbush decreases, modulations by solar and heliosphere parameters, the physical processes that govern them, and their connection to Space Weather, are reviewed. This interdisciplinary compilation provides links between cosmic ray physics, geophysics, terrestrial climate, and human activity and health.
Solar Variability and Climate
Proceedings of an ISSI Workshop, 28 June–2 July 1999, Bern, Switzerland
Inbunden, Engelska, 2000
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The variability of the Sun is well established, as well as that of the Earth's climate. To what extent the two are connected, in the sense that solar variability drives climate, is the subject of considerable research and, in some cases, controversy. This volume is aimed at obtaining an overview of the current knowledge of the variability of the Sun and of the Earth's climate, and of their possible connections. It is a collection of introductory and contributed papers presented at an ISSI workshop, supplemented by a summary of the discussion sessions and a workshop, thus giving a coherent overviewwhile still conveying the lively spirit that prevailed at the workshop. The volume is intended to provide the active researcher with a status report while at the same time serving the advanced graduate student with introductory material in this field of research.
Chronology and Evolution of Mars
Proceedings of an ISSI Workshop, 10–14 April 2000, Bern, Switzerland
Inbunden, Engelska, 2001
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This title results from a workshop at the International Space Science Institute (ISSI) in Bern, Switzerland, where geochemists, geophysicists, and photogeologists have combined their expertise to constrain the timescales and geological processes in the evolution of Mars. In order to achieve this goal, the ages of cratered lunar surfaces, which are dated precisely by the radiometric ages of returned samples, have been taken as a reference for the inner solar system chronology. The derived ages of cratered geological units on Mars indicate ongoing geological activity from about 4.5 Gyr ago till modern geologic time. Ancient surfaces involve primordial crustal material with strong magnetization that has remained from Mars' core formation within the first 20 Myr of the solar system, whereas other surfaces were created during major geological processing at about 3-4.5 Gyr ago, probably associated with a denser atmosphere and more fluvial environment, and also to exposures of volcanism. The youngest surfaces indicate volcanism, weathering, gullying, exhumation, and modest water release all operating within the last few 100~Myr, with the youngest detected flows at less than 10 Myr ago.Neither Earth nor Moon offers such a complete geological record. This picture is consistent with radiometric age data of Martian meteorites which indicate that Mars has not only ancient crustal material, as represented in the ALH84001 meteorite, but at least some geologically young igneous rocks with ages of a few 100 Myr. Remote sensing of the Martian surface identifies two broad groups of igneous rock units, basaltic and andesitic, as is confirmed by in-situ chemical analyses at the Pathfinder landing site. Based on these results, the book contains an update on the overall stratigraphic system and geologic processes of the Martian surface, and a review on the newest models of the Martian interior structure and on the knowledge about the history of the Martian atmosphere and hydrosphere.
Astrophysics of Galactic Cosmic Rays
Proceedings of two ISSI Workshops, 18–22 October 1999 and 15–19 May 2000, Bern, Switzerland
Inbunden, Engelska, 2002
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This volume, together with those on "Cosmic Rays in the Heliosphere" and on "Cosmic Rays at Earth", rounds off a trilogy devoted to cosmic rays. It specifically deals with the astrophysical sources and acceleration processes of cosmic rays. The principal aims are to examine the cosmic ray phenomenon in the context of our evolving understanding of the Galaxy as an astrophysical system. Observations of cosmic rays, and theoretical models of their origin and propagation, are critically reviewed. The extent to which these reinforce, or conflict with, other astronomical information about the Galaxy is addressed.
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The knowledge of the amount and nature of matter present in the universe is one of the most relevant topics in astrophysics and cosmology. It started with the pioneering work of Zwicky in 1933, who found the need for a large amount of dark matter in the Coma cluster. An important step has been the finding through the observation of distant type Ia supernovae of the presence of a significant vacuum energy density causing an accelerating expansion of the universe. Nevertheless, the nature of most of the matter in the universe is still unknown. Its solution requires the interplay of several fields of astrophysics and cosmology as well as particle physics, all of which are covered in this volume: cosmic microwave background radiation, large scale structures, galaxy clusters, intergalactic absorption, dark matter components of galaxies, globular clusters, supernovae of type Ia distance measurements, gravitational lensing, X-ray observations, Lyman-alpha observations, dark energy, direct detection of weakly interacting massive particles (WIMPS), detection of neutrino oscillations, particle candidates for dark matter and big bang nucleosynthesis of baryonic matter.Therefore, this volume presents a useful synopsis of all constituents of matter in the universe.
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The present 15th volume of the ISSI Space Science Series is devoted to Auroral Plasma Physics. The aurora is arguably the most intriguing phenomenon in space plasma physics. Not only is it the most spectacular manifestation of the Sun-Earth connection chain, but the underlying plasma processes are expected to be ubiqui- tous in the plasma universe. Recognizing the enormous progress made over the last decade in the understanding of the physics of the auroral acceleration processes, it seemed timely to write a comprehensive and integrated book on the subject. Re- cent advances concern the clarification of the nature of the acceleration process of the electrons that are responsible for the visible aurora, the recognition of the fundamental role of the large-scale current systems in organizing the auroral mor- phology, and of the interplay between particles and electromagnetic fields. The project began in March 1999, as a natural follow-up of the project on Magnetospheric Plasma Sources and Losses that resulted in volume 6 of this se- ries, with a planning meeting by a core-group that coordinated the project. The group consisted of J. E. Borovsky, Los Alamos National Laboratory; C. W.Carl- son, University of California, Berkeley; G. Haerendel, Max-Planck-Institut fur ex- traterrestrische Physik, Garching; B. Hultqvist, Swedish Intitute ofSpace Physics, H. E. J. Koskinen, Finnish Meteorological Institute, Helsinki; W. Lotko, Kiruna; Dartmouth College, Hanover, New Hampshire; K. A. Lynch, University of New Hampshire, Durham and G. Marklund, Royal Institute ofTechnology, Stockholm. G. Paschmann, ISSI, Bern, was the project leader.
Solar System History from Isotopic Signatures of Volatile Elements
Volume Resulting from an ISSI Workshop 14–18 January 2002, Bern, Switzerland
Inbunden, Engelska, 2003
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This volume, number 16 in the Space Sciences Series of ISSI, reviews the present knowledgeonmanyaspectsofthehistoryofthesolarsystem. Itfocuses onisotopic signatures ofvolatile elements as tracers for the evolutionary processes during the formation of the Sun and the planets from an interstellar molecular cloud and, in tum, illuminates how the isotopic compositions of present-day solar system ob- jects had been established. This integrated collection of articles complements the information provided by previous ISSI volumes such as From Dust to Terrestrial Planets and Chronology and Evolution of Mars, expanding the time scale for the history ofthe solar system. The convenors, Therese Encrenaz, Observatoire de Paris, Meudon; Johannes Geiss, ISSI, Bern; Reinald Kallenbach, ISSI, Bern; Konrad Mauersberger, Max- Planck-Institut fUr Kernphysik, Heidelberg; Tobias Owen, University of Hawaii, Honolulu; and Fran~ois Robert, CNRS-Museum d'Histoire Naturelle, Paris, in- vited experts in planetary science, solar and heliospheric physics, astrophysics, mineralogy, and chemistry to an interdisciplinary workshop in Bern, 14-18 Jan- uary 2002.The resulting review articles are grouped into four sections 'Sun and Protosolar Nebula', 'Outer Solar System', 'Earth, Terrestrial Planets, and Moon', and 'Isotopic FractionationProcesses'.
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This volume in the Space Sciences Series of ISSI is dedicated to the detennination of the Earth's gravity field, which was the topic of a workshop organized by ISSI from 11 to 15 March 2002 in Bern. The aim of the meeting was to gather active researchers from various fields (satellite geodesy, gravity field modelling, solid Earth physics, oceanography, etc.) to assess the exciting new developments that are made possible by space missions currently in orbit or about to be launched. Following some general enquiries with the scientific community concerning the desirability of organising a workshop on the proposed topic, a group of four con- venors (Gerhard Beutler, Univ. of Bern; Mark Drinkwater, ESA-ESTEC, Noord- wijk; Reiner Rummel, Techn. Univ. Miinchen; Rudolf von Steiger, ISS I, Bern) for- mulated the aims and goals of the workshop, structured the workshop into six sec- tions, nominated a list of session chairs (Georges Balmino, GRGS-CNES, Toulouse; Roberto Sabadini, Univ. of Milano, Christian Le Provost, Obs. Midi-Pyrenees, Toulouse; Philip Woodworth, Bidston Observatory, Birkenhead; Miguel Aguirre, ESA-ESTEC, Noordwijk), who in turn set up a programme of introductory talks.The workshop was organized such as to have only plenary sessions with typically half-hour presentations and ample time for discussions. The last day was devoted to conclusions and future objectives.
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Given that the question of an internal magnetic field is of fundamental importance to the understanding of Mars' formation and thermal evolution, and of the evolution of Mars' atmosphere, surprisingly few of the many spacecraft sent to Mars were equipped with instrumentation for such investigations. Of the 9 or so orbiters that have successfully archived Mars orbit, even if for a short period of time, only two have returned useful data about the magnetic field and about the plasma environment near Mars: The Phobos 2 spacecraft, and more recently, Mars Global Surveyor (MGS). With the discovery by MGS that Mars has large remnant magnetic field structures indicating an internal dynamo long extinct, the true nature of the past and present interaction between Mars and the solar wind comes, for the first time, into sharp focus. This work, detailing the integration and new interpretation of the MGS and Phobos results, is a primary reference for the researcher studying solar wind/planet interactions.
Outer Planets and their Moons
Comparative Studies of the Outer Planets prior to the Exploration of the Saturn System by Cassini-Huygens
Inbunden, Engelska, 2005
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Representatives of several scientific communities, such as planetary scientists, astronomers, space physicists, chemists and astrobiologists have met with the aim to review the knowledge on four major themes: (1) the study of the formation and evolution processes of the outer planets and their satellites, beginning with the formation of compounds and planetesimals in the solar nebula, and the subsequent evolution of the interiors of the outer planets, (2) a comparative study of the atmospheres of the outer planets and Titan, (3) the study of the planetary magnetospheres and their interactions with the solar wind, and (4) the formation and properties of satellites and rings, including their interiors, surfaces, and their interaction with the solar wind and the magnetospheres of the outer planets. Beyond these topics, the implications for the prebiotic chemical evolution on Europa and Titan are reviewed.At the time of publication, the study of the outer planets is particularly motivated by the fact that the Saturn system is being investigated by the Cassini-Huygens mission.
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8. 8 Boundary Layer Structure and Detached Plasma 305 8. 8. 1 Background 305 8. 8. 2 Structure inside the boundary layer 306 8. 8. 3 Observation of detached plasma 308 8. 8. 4 Summary 309 8. 9 Summary and Conclusions 310 References 312 9. CLUSTER AT THE MAGNETOSPHERIC CUSPS 321 9. 1 Introduction 321 9. 1. 1 Previous work 323 9. 1. 2 How Cluster investigates the cusp 325 9. 2 The High-Altitude Cusp 326 9. 2. 1 March 17, 2001 328 9. 2. 2 February 4, 2001 332 9. 2. 3 February 13, 2001 337 9. 2. 4 Statistical survey 340 9. 2. 5 Waves and turbulence 343 9. 3 The Mid-Altitude Cusp 352 9. 3. 1 Structure: Case study 352 9. 3. 2 Structure: Statistical survey 354 9. 3. 3 Ionospheric ions 354 9. 3. 4 Mid-altitude signatures of the LLBL 357 9. 4 Discussion 359 References 360 10. MAGNETOPAUSE PROCESSES 367 10. 1 Magnetopause Reconnection 368 10. 1. 1 Intermittent vs. quasi-steady reconnection 368 10. 1. 2 Component vs. anti-parallel reconnection 382 10. 1. 3 Tailward-of-the-cusp reconnection 385 10. 1. 4 Quantitative tests of reconnection occurrence 388 10. 1. 5 Summary 391 10. 2 Kelvin-Helmholtz Instability at the Flank Magnetopause 391 10. 3 Microphysics of Magnetopause Processes 396 10. 3. 1 Collisionless generalised Ohm’s law 397 10. 3. 2 Ion di?usion region observations 398 10. 3. 3 High-frequency waves 402 10. 3. 4 Lower-hybrid waves 405 10. 3.
1 062 kr
Skickas inom 10-15 vardagar
Starting in 1995 numerical modeling of the Earth’s dynamo has ourished with remarkable success. Direct numerical simulation of convection-driven MHD- ow in a rotating spherical shell show magnetic elds that resemble the geomagnetic eld in many respects: they are dominated by the axial dipole of approximately the right strength, they show spatial power spectra similar to that of Earth, and the magnetic eld morphology and the temporal var- tion of the eld resembles that of the geomagnetic eld (Christensen and Wicht 2007). Some models show stochastic dipole reversals whose details agree with what has been inferred from paleomagnetic data (Glatzmaier and Roberts 1995; Kutzner and Christensen 2002; Wicht 2005). While these models represent direct numerical simulations of the fundamental MHD equations without parameterized induction effects, they do not match actual pla- tary conditions in a number of respects. Speci cally, they rotate too slowly, are much less turbulent, and use a viscosity and thermal diffusivity that is far too large in comparison to magnetic diffusivity. Because of these discrepancies, the success of geodynamo models may seem surprising. In order to better understand the extent to which the models are applicable to planetary dynamos, scaling laws that relate basic properties of the dynamo to the fundamental control parameters play an important role. In recent years rst attempts have been made to derive such scaling laws from a set of numerical simulations that span the accessible parameter space (Christensen and Tilgner 2004; Christensen and Aubert 2006).