Author name code: vonsteiger ADS astronomy entries on 2022-09-14 author:"von Steiger, Rudolf E." ------------------------------------------------------------------------ Title: Observations of the Outer Heliosphere, Heliosheath, and Interstellar Medium Authors: Richardson, J. D.; Burlaga, L. F.; Elliott, H.; Kurth, W. S.; Liu, Y. D.; von Steiger, R. Bibcode: 2022SSRv..218...35R Altcode: The Voyager spacecraft have left the heliosphere and entered the interstellar medium, making the first observations of the termination shock, heliosheath, and heliopause. New Horizons is observing the solar wind in the outer heliosphere and making the first direct observations of solar wind pickup ions. This paper reviews the observations of the solar wind plasma and magnetic fields throughout the heliosphere and in the interstellar medium. Title: The Early History of Heliospheric Science and the Spacecraft That Made It Possible Authors: Zank, G. P.; Sterken, V.; Giacalone, J.; Möbius, E.; von Steiger, R.; Stone, E. S.; Krimigis, S. M.; Richardson, J. D.; Linsky, J.; Izmodenov, V.; Heber, B. Bibcode: 2022SSRv..218...34Z Altcode: Our understanding of the interaction of the large-scale heliosphere with the local interstellar medium (LISM) has undergone a profound change since the very earliest analyses of the problem. In part, the revisions have been a consequence of ever-improving and widening observational results, especially those that identified the entrance of interstellar material and gas into the heliosphere. Accompanying these observations was the identification of the basic underlying physics of how neutral interstellar gas and interstellar charged particles of different energies, up to and including interstellar dust grains, interacted with the temporal flows and electromagnetic fields of the heliosphere. The incorporation of these various basic effects into global models of the interaction, whether focused on neutral interstellar gas and pickup ions, energetic particles such as anomalous and galactic cosmic rays, or magnetic fields and large-scale flows, has profoundly changed our view of how the heliosphere and LISM interact. This article presents a brief history of the conceptual and observation evolution of our understanding of the interaction of the heliosphere with the local interstellar medium, up until approximately 1996. Title: Linking the Sun to the Heliosphere Using Composition Data and Modelling Authors: Parenti, Susanna; Chifu, Iulia; Del Zanna, Giulio; Edmondson, Justin; Giunta, Alessandra; Hansteen, Viggo H.; Higginson, Aleida; Laming, J. Martin; Lepri, Susan T.; Lynch, Benjamin J.; Rivera, Yeimy J.; von Steiger, Rudolf; Wiegelmann, Thomas; Wimmer-Schweingruber, Robert F.; Zambrana Prado, Natalia; Pelouze, Gabriel Bibcode: 2021SSRv..217...78P Altcode: 2021arXiv211006111P Our understanding of the formation and evolution of the corona and the heliosphere is linked to our capability of properly interpret the data from remote sensing and in-situ observations. In this respect, being able to correctly connect in-situ observations with their source regions on the Sun is the key for solving this problem. In this work we aim at testing a diagnostics method for this connectivity. Title: Editorial to the Topical Collection on Star Formation Authors: Bykov, A. M.; Charbonnel, C.; Hennebelle, P.; Marcowith, A.; Meynet, G.; Falanga, M.; von Steiger, R. Bibcode: 2020SSRv..216...53B Altcode: No abstract at ADS Title: Small satellites for space science. A COSPAR scientific roadmap Authors: Millan, Robyn M.; von Steiger, Rudolf; Ariel, Meir; Bartalev, Sergey; Borgeaud, Maurice; Campagnola, Stefano; Castillo-Rogez, Julie C.; Fléron, René; Gass, Volker; Gregorio, Anna; Klumpar, David M.; Lal, Bhavya; Macdonald, Malcolm; Park, Jong Uk; Sambasiva Rao, V.; Schilling, Klaus; Stephens, Graeme; Title, Alan M.; Wu, Ji Bibcode: 2019AdSpR..64.1466M Altcode: This is a COSPAR roadmap to advance the frontiers of science through innovation and international collaboration using small satellites. The world of small satellites is evolving quickly and an opportunity exists to leverage these developments to make scientific progress. In particular, the increasing availability of low-cost launch and commercially available hardware provides an opportunity to reduce the overall cost of science missions. This in turn should increase flight rates and encourage scientists to propose more innovative concepts, leading to scientific breakthroughs. Moreover, new computer technologies and methods are changing the way data are acquired, managed, and processed. The large data sets enabled by small satellites will require a new paradigm for scientific data analysis. In this roadmap we provide several examples of long-term scientific visions that could be enabled by the small satellite revolution. For the purpose of this report, the term "small satellite" is somewhat arbitrarily defined as a spacecraft with an upper mass limit in the range of a few hundred kilograms. The mass limit is less important than the processes used to build and launch these satellites. The goal of this roadmap is to encourage the space science community to leverage developments in the small satellite industry in order to increase flight rates, and change the way small science satellites are built and managed. Five recommendations are made; one each to the science community, to space industry, to space agencies, to policy makers, and finally, to COSPAR. Title: Linking the Sun to the heliosphere using composition data and modelling: coronal jets as a test case Authors: Wimmer-Schweingruber, Robert F.; Parenti, Susanna; Del Zanna, G.; Edmondson, J.; Giunta, A.; Hansteen, V. H.; Higginson, A.; Lepri, S.; Laming, M.; Lynch, B. J.; von Steiger, R. E.; Wiegelmann, T.; Zambrana Prado, N. Bibcode: 2019shin.confE.231W Altcode: Understanding the formation and evolution of the solar wind is still a priority in the Solar and Heliospheric communities. We expect a significant progress in terms of observations with the upcoming Solar Orbiter mission (launch in 2020), which will provide detailed in-situ measurements of the solar wind and several remote-sensing observations. However, real progress will only be possible if we improve our understanding of the physical link between what measured in-situ and its source regions on the Sun. In this respect, the plasma chemical and charge-state compositions are considered good diagnostic tools. In this paper we present results obtained from an extensive team work aiming at providing solid diagnostics for linking the in-situ and the remote sensing measurements. For our test cases, we selected two periods when a single active region produced, close to its sunspot, jets which had a counterpart signature in the Heliosphere in the form of type-III radio bursts. These jets therefore marked magnetically open regions expanding in the heliosphere. Firstly, we looked for signatures of the open field associated with the active regions in in-situ data from ACE and WIND, finding potential tracers. Secondly, we studied the magnetic topology of the full Sun and Heliosphere with extrapolations of photospheric data and MHD modeling. We found that the open field area is consistent with the source and evolution of the jets, as observed with EUV imagers (SDO/AIA, STEREO/EUVI). Thirdly, we analysed remote sensing EUV spectroscopic observations to measure the plasma conditions (densities, temperatures and chemical composition) whenever available. We then modeled the solar wind and charge state evolution with the solar distance along the open fields to establish a link between the in-situ signatures and the remote sensing observations. We discuss the various difficulties associated with such studies, and highlight how Solar Orbiter measurements can improve them. Title: The Scientific Foundation of Space Weather Authors: Baker, Daniel; Balogh, André; Gombosi, Tamas; Koskinen, Hannu E. J.; Veronig, Astrid; von Steiger, Rudolf Bibcode: 2019sfsw.book.....B Altcode: No abstract at ADS Title: Supernovae Authors: Bykov, Andrei; Roger, Chevalier; Raymond, John; Thielemann, Friedrich-Karl; Falanga, Maurizio; von Steiger, Rudolf Bibcode: 2019supe.book.....B Altcode: No abstract at ADS Title: Achievements and Challenges in the Science of Space Weather Authors: Koskinen, Hannu E. J.; Baker, Daniel N.; Balogh, André; Gombosi, Tamas; Veronig, Astrid; von Steiger, Rudolf Bibcode: 2019sfsw.book....1K Altcode: No abstract at ADS Title: Geoeffective Properties of Solar Transients and Stream Interaction Regions Authors: Kilpua, E. K. J.; Balogh, A.; von Steiger, R.; Liu, Y. D. Bibcode: 2019sfsw.book..295K Altcode: No abstract at ADS Title: Determination of Plasma, Pickup Ion, and Suprathermal Particle Spectrum in the Solar Wind Frame of Reference Authors: Zhang, Ming; Zhao, Lulu; von Steiger, R.; Wimmer-Schweingruber, R. F.; Gloeckler, G. M.; Desai, M.; Pogorelov, N. V. Bibcode: 2019ApJ...871...60Z Altcode: Particle spectra directly measured by a plasma or low-energy particle experiment on spacecraft often contain instrumental effects due to a limited field of view or angular resolution. It is because the particle distribution function at low energies is highly anisotropic in the spacecraft frame of reference, in which the measurements are made. In this paper, we present a new mathematical method of transforming the particle spectrum to the solar wind frame of reference, where the particle distribution can be assumed to be nearly isotropic. The transformed particle spectrum allows us to investigate the properties of the solar wind, pickup ions, and suprathermal particles without concern for instrumental effects. We apply the method to the measurements made by the Solar Wind Ion Composition Spectrometer on Ulysses. Our results demonstrate that the transformed spectrum can improve the determination of the solar wind density and temperature from the previously published methods. A brief survey of Ulysses data shows that suprathermal ions in the slow solar wind frequently display a velocity distribution very close to the v -5 power law. Title: Preface Authors: Bykov, A. M.; Chevalier, R. A.; Raymond, J. C.; Thielemann, F. -K.; Falanga, M.; von Steiger, R. Bibcode: 2019supe.book....1B Altcode: No abstract at ADS Title: Small Satellites for Space Science (4S) COSPAR Roadmap Authors: Millan, Robyn; Von Steiger, Rudolf; Castillo-Rogez, Julie; Lal, Bhavya Bibcode: 2018cosp...42E2286M Altcode: In 2016, COSPAR commissioned an international scientific roadmap on Small Satellites for Space Science (4S), focusing particularly on CubeSats and CubeSat-technology enabled small satellites. The report is motivated by recent progress and results summarized in a published paper (Zurbuchen, von Steiger et al., Performing High-Quality Science on CubeSats, Space Research Today, Vol. 196, pp. 10-30, August 2016) and a study by the US National Academies (Zurbuchen, Lal, et al., Achieving Science with CubeSats: Thinking Inside the Box, The National Academies Press, Washington, DC, 2016). The roadmap has been developed by a study team that covers a broad range of scientific and technological disciplines, from Earth to planetary science, and from solar system science to astronomy. The team is composed of scientists and engineers working in universities, public research institutions and industry. The report is structured into three main parts: I. Our Neighborhood: current status of technology and scientific potential of small satellites and CubeSatsII. Visions for the Future: potential ideas for what small satellites could be used for in the futureIII. Challenges to Further Development and Progress, and Ways to Overcome Them: roles of agencies, industry, policies, international collaboration and exchange In this presentation, members of the study team will give an overview of the roadmap and summarize the findings of the study team, concentrating on the parts relating to planetary science in particular. The final report is intended to be of value to space agencies internationally and their supporting governments, as well as non-profits and other private sector organizations that would be interested in promoting global smallsat-based missions. Title: Long-term evolution of solar wind elemental and charge state composition Authors: Von Steiger, Rudolf; Gilbert, Jason A. Bibcode: 2018cosp...42E3559V Altcode: Before the 1990s observations of heavy elements in the solar wind (A>4) were limited to a small number of brief periods with favorable conditions. This has changed with the launch of the Ulysses mission in October 1990 and the ACE mission in August 1997, whose SWICS sister instruments are providing us with composition data covering all charge states of C, N, O, Ne, N, Mg, Si, S, and Fe. The nearly uninterrupted data sets combined now cover almost three full decades: Ulysses was operating until June 2009 and ACE continues to operate until today, although with some limitations of SWICS since August 2011. We will present an overview of these unique data sets and the interpretation of the elemental and charge state composition therein. Title: Small Satellites for Space Science (4S) COSPAR Roadmap Authors: Von Steiger, Rudolf; Millan, Robyn; Schilling, Klaus; Borgeaud, Maurice Bibcode: 2018cosp...42E3560V Altcode: In 2016 COSPAR commissioned an international scientific roadmap on Small Satellites for Space Science (4S), focusing particularly on CubeSats and CubeSat-technology enabled small satellites. The report is motivated by recent progress and results summarized in a published paper (Zurbuchen, von Steiger et al., Performing High-Quality Science on CubeSats, Space Research Today, Vol. 196, pp. 10-30, August 2016) and a study by the US National Academies (Zurbuchen, Lal, et al., Achieving Science with CubeSats: Thinking Inside the Box, The National Academies Press, Washington, DC, 2016).The roadmap has been developed by a study team that covers a broad range of scientific disciplines, from Earth to planetary science and from solar system science to astronomy. The team is composed of scientists and engineers working in universities, public research institutions and industry. The report is structured into three main parts:I. Our Neighborhood: current status and scientific potential of small satellites and CubeSatsII. Visions for the Future: potential ideas for what small satellites could be in the futureIII. Challenges to Further Development and Progress, and Ways to Overcome Them: roles of agencies, industry, policies, international collaboration and exchangeIn this presentation, members of the study team will give an overview of the roadmap and summarize the findings of the study team with emphasis on the parts relating to Earth observation in particular. The final report is intended to be of value to space agencies, key actors, industries, and governments involved in Small Satellites Title: Editorial to the Topical Collection on Supernovae Authors: Bykov, A. M.; Chevalier, R. A.; Raymond, J. C.; Thielemann, F. -K.; Falanga, M.; von Steiger, R. Bibcode: 2018SSRv..214...73B Altcode: No abstract at ADS Title: Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals Authors: Sibeck, David G.; Allen, R.; Aryan, H.; Bodewits, D.; Brandt, P.; Branduardi-Raymont, G.; Brown, G.; Carter, J. A.; Collado-Vega, Y. M.; Collier, M. R.; Connor, H. K.; Cravens, T. E.; Ezoe, Y.; Fok, M. -C.; Galeazzi, M.; Gutynska, O.; Holmström, M.; Hsieh, S. -Y.; Ishikawa, K.; Koutroumpa, D.; Kuntz, K. D.; Leutenegger, M.; Miyoshi, Y.; Porter, F. S.; Purucker, M. E.; Read, A. M.; Raeder, J.; Robertson, I. P.; Samsonov, A. A.; Sembay, S.; Snowden, S. L.; Thomas, N. E.; von Steiger, R.; Walsh, B. M.; Wing, S. Bibcode: 2018SSRv..214...79S Altcode: Both heliophysics and planetary physics seek to understand the complex nature of the solar wind's interaction with solar system obstacles like Earth's magnetosphere, the ionospheres of Venus and Mars, and comets. Studies with this objective are frequently conducted with the help of single or multipoint in situ electromagnetic field and particle observations, guided by the predictions of both local and global numerical simulations, and placed in context by observations from far and extreme ultraviolet (FUV, EUV), hard X-ray, and energetic neutral atom imagers (ENA). Each proposed interaction mechanism (e.g., steady or transient magnetic reconnection, local or global magnetic reconnection, ion pick-up, or the Kelvin-Helmholtz instability) generates diagnostic plasma density structures. The significance of each mechanism to the overall interaction (as measured in terms of atmospheric/ionospheric loss at comets, Venus, and Mars or global magnetospheric/ionospheric convection at Earth) remains to be determined but can be evaluated on the basis of how often the density signatures that it generates are observed as a function of solar wind conditions. This paper reviews efforts to image the diagnostic plasma density structures in the soft (low energy, 0.1-2.0 keV) X-rays produced when high charge state solar wind ions exchange electrons with the exospheric neutrals surrounding solar system obstacles.

The introduction notes that theory, local, and global simulations predict the characteristics of plasma boundaries such the bow shock and magnetopause (including location, density gradient, and motion) and regions such as the magnetosheath (including density and width) as a function of location, solar wind conditions, and the particular mechanism operating. In situ measurements confirm the existence of time- and spatial-dependent plasma density structures like the bow shock, magnetosheath, and magnetopause/ionopause at Venus, Mars, comets, and the Earth. However, in situ measurements rarely suffice to determine the global extent of these density structures or their global variation as a function of solar wind conditions, except in the form of empirical studies based on observations from many different times and solar wind conditions. Remote sensing observations provide global information about auroral ovals (FUV and hard X-ray), the terrestrial plasmasphere (EUV), and the terrestrial ring current (ENA). ENA instruments with low energy thresholds (∼1 keV) have recently been used to obtain important information concerning the magnetosheaths of Venus, Mars, and the Earth. Recent technological developments make these magnetosheaths valuable potential targets for high-cadence wide-field-of-view soft X-ray imagers.

Section 2 describes proposed dayside interaction mechanisms, including reconnection, the Kelvin-Helmholtz instability, and other processes in greater detail with an emphasis on the plasma density structures that they generate. It focuses upon the questions that remain as yet unanswered, such as the significance of each proposed interaction mode, which can be determined from its occurrence pattern as a function of location and solar wind conditions. Section 3 outlines the physics underlying the charge exchange generation of soft X-rays. Section 4 lists the background sources (helium focusing cone, planetary, and cosmic) of soft X-rays from which the charge exchange emissions generated by solar wind exchange must be distinguished. With the help of simulations employing state-of-the-art magnetohydrodynamic models for the solar wind-magnetosphere interaction, models for Earth's exosphere, and knowledge concerning these background emissions, Sect. 5 demonstrates that boundaries and regions such as the bow shock, magnetosheath, magnetopause, and cusps can readily be identified in images of charge exchange emissions. Section 6 reviews observations by (generally narrow) field of view (FOV) astrophysical telescopes that confirm the presence of these emissions at the intensities predicted by the simulations. Section 7 describes the design of a notional wide FOV "lobster-eye" telescope capable of imaging the global interactions and shows how it might be used to extract information concerning the global interaction of the solar wind with solar system obstacles. The conclusion outlines prospects for missions employing such wide FOV imagers. Title: Minimal Magnetic States of the Sun and the Solar Wind: Implications for the Origin of the Slow Solar Wind Authors: Cliver, E. W.; von Steiger, R. Bibcode: 2018smf..book..227C Altcode: No abstract at ADS Title: Jets and Winds in Pulsar Wind Nebulae, Gamma-Ray Bursts and Blazars Authors: Bykov, Andrei; Amato, Elena; Arons, Jonathan; Falanga, Maurizio; Lemoine, Martin; Stella, Luigi; von Steiger, Rudolf Bibcode: 2018jwpw.book.....B Altcode: No abstract at ADS Title: Solar Magnetic Fields Authors: Balogh, André; Cliver, Edward; Petrie, Gordon; Solanki, Sami; Thompson, Michael; von Steiger, Rudolf Bibcode: 2018smf..book.....B Altcode: No abstract at ADS Title: Editorial: Measuring Solar Magnetic Fields—An Outline of History, Current Status and Challenges Authors: Balogh, André; von Steiger, Rudolf Bibcode: 2018smf..book....1B Altcode: No abstract at ADS Title: Editorial: Topical Collection on Jets and Winds in Pulsar Wind Nebulae, Gamma-Ray Bursts and Blazars Authors: Bykov, A.; Amato, E.; Arons, J.; Falanga, M.; Lemoine, M.; Stella, L.; von Steiger, R. Bibcode: 2018jwpw.book....1B Altcode: No abstract at ADS Title: Achievements and Challenges in the Science of Space Weather Authors: Koskinen, Hannu E. J.; Baker, Daniel N.; Balogh, André; Gombosi, Tamas; Veronig, Astrid; von Steiger, Rudolf Bibcode: 2017SSRv..212.1137K Altcode: 2017SSRv..tmp...80K In June 2016 a group of 40 space weather scientists attended the workshop on Scientific Foundations of Space Weather at the International Space Science Institute in Bern. In this lead article to the volume based on the talks and discussions during the workshop we review some of main past achievements in the field and outline some of the challenges that the science of space weather is facing today and in the future. Title: Geoeffective Properties of Solar Transients and Stream Interaction Regions Authors: Kilpua, E. K. J.; Balogh, A.; von Steiger, R.; Liu, Y. D. Bibcode: 2017SSRv..212.1271K Altcode: 2017SSRv..tmp..161K Interplanetary Coronal Mass Ejections (ICMEs), their possible shocks and sheaths, and co-rotating interaction regions (CIRs) are the primary large-scale heliospheric structures driving geospace disturbances at the Earth. CIRs are followed by a faster stream where Alfvénic fluctuations may drive prolonged high-latitude activity. In this paper we highlight that these structures have all different origins, solar wind conditions and as a consequence, different geomagnetic responses. We discuss general solar wind properties of sheaths, ICMEs (in particular those showing the flux rope signatures), CIRs and fast streams and how they affect their solar wind coupling efficiency and the resulting magnetospheric activity. We show that there are two different solar wind driving modes: (1) Sheath-like with turbulent magnetic fields, and large Alfvén Mach (MA) numbers and dynamic pressure, and (2) flux rope-like with smoothly varying magnetic field direction, and lower MA numbers and dynamic pressure. We also summarize the key properties of interplanetary shocks for space weather and how they depend on solar cycle and the driver. Title: Editorial: Measuring Solar Magnetic Fields—An Outline of History, Current Status and Challenges Authors: Balogh, André; von Steiger, Rudolf Bibcode: 2017SSRv..210....1B Altcode: 2017SSRv..tmp..163B No abstract at ADS Title: Minimal Magnetic States of the Sun and the Solar Wind: Implications for the Origin of the Slow Solar Wind Authors: Cliver, E. W.; von Steiger, R. Bibcode: 2017SSRv..210..227C Altcode: 2015SSRv..tmp..116C During the last decade it has been proposed that both the Sun and the solar wind have minimum magnetic states, lowest order levels of magnetism that underlie the 11-yr cycle as well as longer-term variability. Here we review the literature on basal magnetic states at the Sun and in the heliosphere and draw a connection between the two based on the recent deep 2008-2009 minimum between cycles 23 and 24. In particular, we consider the implications of the low solar activity during the recent minimum for the origin of the slow solar wind. Title: Editorial: Topical Collection on Jets and Winds in Pulsar Wind Nebulae, Gamma-Ray Bursts and Blazars. Physics of Extreme Energy Release Authors: Bykov, A.; Amato, E.; Arons, J.; Falanga, M.; Lemoine, M.; Stella, L.; von Steiger, R. Bibcode: 2017SSRv..207....1B Altcode: 2017SSRv..tmp...45B No abstract at ADS Title: Fundamental Physics of the Slow Solar Wind - What do we Know? Authors: Ofman, L.; Abbo, L.; Antiochos, S. K.; Hansteen, V. H.; Harra, L.; Ko, Y. K.; Lapenta, G.; Li, B.; Riley, P.; Strachan, L.; von Steiger, R.; Wang, Y. M. Bibcode: 2016AGUFMSH42A..01O Altcode: Fundamental physical properties of the slow solar wind (SSW), such as density, temperature, outflow speed, heavy ion abundances and charges states were obtained from in-situ measurements at 1AU in the past from WIND, ACE, and other spacecraft. Plasma and magnetic field measurement are available as close as 0.3 AU from Helios data, Spektr-R, and MESSENGER spacecraft. Remote sensing spectroscopic measurements are available in the corona and below from SOHO/UVCS, Hinode, and other missions. One of the major objectives of the Solar Orbiter and Solar Probe Plus missions is to study the sources of the SSW close to the Sun. The present state of understanding of the physics of the SSW is based on the combination of the existing observations, theoretical and numerical 3D MHD and multi-fluid models, that connect between the SSW sources in the corona and the heliosphere. Recently, hybrid models that combine fluid electrons and kinetic ions of the expanding solar wind were developed, and provide further insights of the local SSW plasma heating processes that related to turbulent magnetic fluctuations spectra and kinetic ion instabilities observed in the SSW plasma. These models produce the velocity distribution functions (VDFs) of the protons and heavier ions as well as the ion anisotropic temperatures. I will discuss the results of the above observations and models, and review the current status of our understanding of the fundamental physics of the SSW. I will review the open questions, and discuss how they could be addressed with near future observations and models. Title: Solar Metallicity Derived from In-Situ Solar Wind Composition Authors: von Steiger, R.; Zurbuchen, T. Bibcode: 2016AGUFMSH51B2578V Altcode: Solar metallicity — the fraction per unit mass that is composed of elements heavier than He — is a critical and fundamental quantity indicative of the history and future evolution of the Sun. Over the last decade spectroscopic observations of the solar photosphere using inversion techniques of increasing sophistication have led to a downward revision of the abundances of heavy elements, specifically C, N, and O, and thus of the solar metallicity. This in turn has led to a crisis of solar models, which became inconsistent with the results of helioseismology as a consequence of the missing opacity from these elements. We present recently released solar wind compositional data to determine the metallicity of the Sun. We focus on a present-day solar sample available to us, which is the least fractionated solar wind from coronal holes near the poles of the Sun. Using these data, we derive a metallicity of Z = 0.0196 ± 0.0014, which is signicantly larger than recent published values based on photospheric spectroscopy, but consistent with results from helioseismology. Title: Slow Solar Wind: Observations and Modeling Authors: Abbo, L.; Ofman, L.; Antiochos, S. K.; Hansteen, V. H.; Harra, L.; Ko, Y. -K.; Lapenta, G.; Li, B.; Riley, P.; Strachan, L.; von Steiger, R.; Wang, Y. -M. Bibcode: 2016SSRv..201...55A Altcode: 2016SSRv..tmp...34A While it is certain that the fast solar wind originates from coronal holes, where and how the slow solar wind (SSW) is formed remains an outstanding question in solar physics even in the post-SOHO era. The quest for the SSW origin forms a major objective for the planned future missions such as the Solar Orbiter and Solar Probe Plus. Nonetheless, results from spacecraft data, combined with theoretical modeling, have helped to investigate many aspects of the SSW. Fundamental physical properties of the coronal plasma have been derived from spectroscopic and imaging remote-sensing data and in situ data, and these results have provided crucial insights for a deeper understanding of the origin and acceleration of the SSW. Advanced models of the SSW in coronal streamers and other structures have been developed using 3D MHD and multi-fluid equations. Title: Composition of Coronal Mass Ejections Authors: Zurbuchen, T. H.; Weberg, M.; von Steiger, R.; Mewaldt, R. A.; Lepri, S. T.; Antiochos, S. K. Bibcode: 2016ApJ...826...10Z Altcode: We analyze the physical origin of plasmas that are ejected from the solar corona. To address this issue, we perform a comprehensive analysis of the elemental composition of interplanetary coronal mass ejections (ICMEs) using recently released elemental composition data for Fe, Mg, Si, S, C, N, Ne, and He as compared to O and H. We find that ICMEs exhibit a systematic abundance increase of elements with first ionization potential (FIP) < 10 eV, as well as a significant increase of Ne as compared to quasi-stationary solar wind. ICME plasmas have a stronger FIP effect than slow wind, which indicates either that an FIP process is active during the ICME ejection or that a different type of solar plasma is injected into ICMEs. The observed FIP fractionation is largest during times when the Fe ionic charge states are elevated above Q Fe > 12.0. For ICMEs with elevated charge states, the FIP effect is enhanced by 70% over that of the slow wind. We argue that the compositionally hot parts of ICMEs are active region loops that do not normally have access to the heliosphere through the processes that give rise to solar wind. We also discuss the implications of this result for solar energetic particles accelerated during solar eruptions and for the origin of the slow wind itself. Title: Solar Metallicity Derived from in situ Solar Wind Composition Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2016ApJ...816...13V Altcode: We use recently released solar wind compositional data to determine the metallicity of the Sun—the fraction per unit mass that is composed of elements heavier than He. We focus on a present-day solar sample available to us, which is the least fractionated solar wind from coronal holes near the poles of the Sun. Using these data, we derive a metallicity of Z = 0.0196 ± 0.0014, which is significantly larger than recent published values based on photospheric spectroscopy, but consistent with results from helioseismology. Title: Slow Solar Wind: Observable Characteristics for Constraining Modelling Authors: Ofman, L.; Abbo, L.; Antiochos, S. K.; Hansteen, V. H.; Harra, L.; Ko, Y. K.; Lapenta, G.; Li, B.; Riley, P.; Strachan, L.; von Steiger, R.; Wang, Y. M. Bibcode: 2015AGUFMSH11F..03O Altcode: The Slow Solar Wind (SSW) origin is an open issue in the post SOHO era and forms a major objective for planned future missions such as the Solar Orbiter and Solar Probe Plus.Results from spacecraft data, combined with theoretical modeling, have helped to investigate many aspects of the SSW. Fundamental physical properties of the coronal plasma have been derived from spectroscopic and imaging remote-sensing data and in-situ data, and these results have provided crucial insights for a deeper understanding of the origin and acceleration of the SSW.Advances models of the SSW in coronal streamers and other structures have been developed using 3D MHD and multi-fluid equations.Nevertheless, there are still debated questions such as:What are the source regions of SSW? What are their contributions to the SSW?Which is the role of the magnetic topology in corona for the origin, acceleration and energy deposition of SSW?Which are the possible acceleration and heating mechanisms for the SSW?The aim of this study is to present the insights on the SSW origin and formationarisen during the discussions at the International Space Science Institute (ISSI) by the Team entitled ''Slowsolar wind sources and acceleration mechanisms in the corona'' held in Bern (Switzerland) in March2014--2015. The attached figure will be presented to summarize the different hypotheses of the SSW formation. Title: New insights in the interstellar dust properties and its interaction with the heliosphere from data, simulations and experiments Authors: Sterken, V. J.; Strub, P.; Krüger, H.; von Steiger, R.; Frisch, P. C.; Moragas-Klostermeyer, G. Bibcode: 2015AGUFMSH53C..07S Altcode: Interstellar dust moves through the heliosphere at velocities of ca. 26 km/s due to the relative motion of the local interstellar cloud and the solar system. On their way through the solar system, these charged particles' trajectories are affected by solar radiation pressure force, gravity and Lorentz force, causing them to deviate in a temporal and in a spatial way that depends on the particle properties and on the interplanetary magnetic field. Combining 16 years of Ulysses interstellar dust data with Monte Carlo simulations of these particle trajectories in the inner heliosphere have unveiled new insights in the interstellar dust flow, the dust properties and it can be used to explore the nature of the outer heliosphere.We start the talk with an overview of the current state of the art of the local interstellar dust research. We then explain the simulations and put them in the context of the Ulysses data. Using these, we demonstrate that the particles are likely to be porous, and we show why a model of dust propagation through the outer heliosphere is needed to provide a final proof. Also, we discuss the steps needed to determine from the simulations, data, and experiments how porous or fluffy the interstellar dust is. Finally, we explain how ISD data can be used as an extra 'measureable' to explore the structure of the outer heliosphere and we conclude the talk with a summary of how this enhances our knowledge of ISD and the LIC. Title: Variations in Solar Wind Fractionation as Seen by ACE/SWICS Over a Full Solar Cycle and the Implications for Genesis Mission Results Authors: Reisenfeld, D. B.; Pilleri, P.; Zurbuchen, T.; Lepri, S. T.; Shearer, P.; Gilbert, J. A.; von Steiger, R.; Wiens, R. C. Bibcode: 2015AGUFMSH22B..06R Altcode: We use ACE/SWICS elemental composition data to compare the variations in solar wind fractionation as measured by SWICS during the previous solar maximum (1999-2001), solar minimum (2006-2009) and the period in which the Genesis spacecraft was collecting solar wind (late 2001 - early 2004). We differentiate our analysis in terms of solar wind regimes (i.e. solar wind originating from interstream or coronal hole flows, or coronal mass ejecta). Abundances are normalized to the low-FIP ion magnesium to uncover correlations that are not apparent when normalizing to high-FIP ions. We find that relative to magnesium, the other low-FIP elements are measurably fractionated, but the degree of fractionation does not vary significantly over the solar cycle. For the high-FIP ions, variation in fractionation over the solar cycle is significant: greatest for Ne/Mg and C/Mg, less so for O/Mg, and the least for He/Mg. When abundance ratios are examined as a function of solar wind speed, we find a strong correlation, with the remarkable observation that the degree of fractionation follows a mass-dependent trend. We will discuss the implications for correcting the Genesis sample return results to photospheric abundances. Title: Variations in Solar Wind Fractionation as Seen by ACE/SWICS and the Implications for Genesis Mission Results Authors: Pilleri, P.; Reisenfeld, D. B.; Zurbuchen, T. H.; Lepri, S. T.; Shearer, P.; Gilbert, J. A.; von Steiger, R.; Wiens, R. C. Bibcode: 2015ApJ...812....1P Altcode: 2015arXiv150804566P We use Advanced Composition Explorer (ACE)/Solar Wind Ion Composition Spectrometer (SWICS) elemental composition data to compare the variations in solar wind (SW) fractionation as measured by SWICS during the last solar maximum (1999-2001), the solar minimum (2006-2009), and the period in which the Genesis spacecraft was collecting SW (late 2001—early 2004). We differentiate our analysis in terms of SW regimes (i.e., originating from interstream or coronal hole flows, or coronal mass ejecta). Abundances are normalized to the low-first ionization potential (low-FIP) ion magnesium to uncover correlations that are not apparent when normalizing to high-FIP ions. We find that relative to magnesium, the other low-FIP elements are measurably fractionated, but the degree of fractionation does not vary significantly over the solar cycle. For the high-FIP ions, variation in fractionation over the solar cycle is significant: greatest for Ne/Mg and C/Mg, less so for O/Mg, and the least for He/Mg. When abundance ratios are examined as a function of SW speed, we find a strong correlation, with the remarkable observation that the degree of fractionation follows a mass-dependent trend. We discuss the implications for correcting the Genesis sample return results to photospheric abundances. Title: Sixteen Years of Ulysses Interstellar Dust Measurements in the Solar System. III. Simulations and Data Unveil New Insights into Local Interstellar Dust Authors: Sterken, Veerle J.; Strub, Peter; Krüger, Harald; von Steiger, Rudolf; Frisch, Priscilla Bibcode: 2015ApJ...812..141S Altcode: Interstellar dust (ISD) in the solar system was detected in situ for the first time in 1993 by the Ulysses dust detector. The study of ISD is important for understanding its role in star and solar system formation. The goal of this paper is to understand the variability in the ISD observations from the Ulysses mission by using a Monte Carlo simulation of ISD trajectories, with the final aim to constrain the ISD particle properties from simulations and the data. The paper is part of a series of three: Strub et al. describe the variations of the ISD flow from the Ulysses data set, and Krüger et al. focus on its ISD mass distribution. We describe and interpret the simulations of the ISD flow at Ulysses orbit for a wide range of particle properties and discuss four open issues in ISD research: the existence of very big ISD particles, the lack of smaller ISD particles, the shift in dust flow direction in 2005, and particle properties. We conclude that the shift in the dust flow direction in 2005 can best be explained by Lorentz force in the inner heliosphere, but that an extra filtering mechanism is needed to fit the fluxes. A time-dependent filtering in the outer regions of the heliosphere is proposed for this. Also, the high charge-to-mass ratio values found for the heavier particles after 2003 indicate that these particles are lower in density than previously assumed. This method gives new insights into the ISD properties and paves the way toward getting a complete view on the ISD from the local interstellar cloud. We conclude that in combination with the data and simulations, also impact ionization experiments are necessary using low-density dust, in order to constrain the density of the particles. Title: Introduction to the Solar Activity Cycle: Overview of Causes and Consequences Authors: Balogh, A.; Hudson, H. S.; Petrovay, K.; von Steiger, R. Bibcode: 2015sac..book....1B Altcode: No abstract at ADS Title: The Solar Activity Cycle Authors: Balogh, André; Hudson, Hugh; Petrovay, Kristóf; von Steiger, Rudolf Bibcode: 2015sac..book.....B Altcode: No abstract at ADS Title: The role of the heliosphere for interstellar dust trajectories - revisited Authors: Sterken, V. J.; Strub, P.; Krüger, H.; von Steiger, R.; Grün, E. Bibcode: 2014AGUFMSH13B4124S Altcode: Interstellar dust (ISD) moves through the solar system due to the relative motion of the solar system and the local interstellar cloud, at a speed of about 26 km/s. Most of the knowledge on these ISD trajectories and their interplay with the interplanetary magnetic field come from dust impact measurements using the Ulysses dust detector in combination with modelling of the ISD trajectories. In this talk we explain the dynamics of interstellar dust in the heliosphere, we discuss in detail the resulting fluxes and directions of the ISD flow at the location of Ulysses, we put this in context with existing data, review the influence of three different descriptions of the IMF on the modelling, and finally we conclude with the role of the boundary region of the heliosphere on the ISD flux. Title: Introduction to the Solar Activity Cycle: Overview of Causes and Consequences Authors: Balogh, A.; Hudson, H. S.; Petrovay, K.; von Steiger, R. Bibcode: 2014SSRv..186....1B Altcode: 2014SSRv..tmp...60B The 11-year activity cycle is a dominant characteristic of the Sun. It is the result of the evolution in time the solar dynamo that generates the solar magnetic field. The nearly periodic variation in the sunspot number has been known since the mid-1800s; as the observations of the Sun broadened to cover an increasing number of phenomena, the same 11-year periodicity was noted in most of them. The discovery of solar magnetic fields introduced a 22-year periodicity, as the magnetic polarities of the polar regions change sign every 11 years. Correlations have been identified and quantified among all the measured parameters, but in most cases such correlations remain empirical rather than grounded in physical processes. This introductory paper and the reviews in the volume describe and discuss the current state of understanding of the causal chains that lead from the variable nature of the solar magnetic fields to the variability of solar phenomena. The solar activity cycle is poorly understood: predictions made for the current Cycle 24 have proved to be generally wrong. However, the re-evaluation of the relationships in the light of unexpected shortcomings is likely to lead to a better physical understanding of solar physics. This will help in the systematic reassessment of solar activity indices and their usefulness in describing and predicting the solar activity cycle. Title: Solar Wind C, N, and O Abundances and the Solar Metallicity Authors: von Steiger, R.; Zurbuchen, T.; Shearer, P.; Gilbert, J. A. Bibcode: 2014AGUFMSH33A4127V Altcode: Solar wind composition provides important constraints to solar composition and to the processes that modify such compositional patterns in the atmospheres of the Sun and of active stars. There are a number of ways that composition can be observed, including spectroscopy, helioseismology, and the collection of solar samples either in the form of solar wind or energetic particles. In either case, models are needed to infer compositional constraints from observations. For example, models are needed to interpret solar spectroscopy results, and the evolution of these has recently led to significant changes to the previously accepted solar composition. The collection of solar samples requires a different type of consideration. Most solar wind and energetic particle samples are fractionated according to first ionization potential (FIP) as first pointed out by Hovestadt et al. in the seventies - elements with FIP below 10 eV are enhanced relative to elements at higher FIP, and He and possibly Ne are further depleted. Besides FIP fractionation there are indications from both isotopic and elemental data that mass fractionation, either through gravitational and/or collisional processes, may also play a role. Based on comparisons of in situ data with coronal spectroscopy it is evident that most of these processes occur at the interface between the photosphere and the corona. However, the high-latitude corona near solar minimum appears to undergo much less fractionation, if any at all. Thus it provides a heliospheric sample that is - to within our observational constraints - photospheric in nature. The low-latitude heliosphere further provides direct access to plasmas that have the fractionation pattern qualitatively and quantitatively similar to the one observed in the corona. We present a recent reanalysis of the SWICS observations on both Ulysses and ACE using modern statistical tools. Concentrating on C, N, and O, which together with the recently published Ne (Shearer et al., ApJ, 2014) contribute 96% of the solar metallicity, we find that the solar wind metallicity is significantly higher than the recent compilation of spectroscopic abundances (Asplund et al., ARAA, 2009). It is more in line with earlier spectroscopic results and, more importantly, not incompatible with helioseismology results of the solar interior. Title: Solar Corona/Wind Composition and Origins of the Solar Wind Authors: Lepri, S. T.; Gilbert, J. A.; Landi, E.; Shearer, P.; von Steiger, R.; Zurbuchen, T. Bibcode: 2014AGUFMSH33A4129L Altcode: Measurements from ACE and Ulysses have revealed a multifaceted solar wind, with distinctly different kinetic and compositional properties dependent on the source region of the wind. One of the major outstanding issues in heliophysics concerns the origin and also predictability of quasi-stationary slow solar wind. While the fast solar wind is now proven to originate within large polar coronal holes, the source of the slow solar wind remains particularly elusive and has been the subject of long debate, leading to models that are stationary and also reconnection based - such as interchange or so-called S-web based models. Our talk will focus on observational constraints of solar wind sources and their evolution during the solar cycle. In particular, we will point out long-term variations of wind composition and dynamic properties, particularly focused on the abundance of elements with low First Ionization Potential (FIP), which have been routinely measured on both ACE and Ulysses spacecraft. We will use these in situ observations, and remote sensing data where available, to provide constraints for solar wind origin during the solar cycle, and on their correspondence to predictions for models of the solar wind. Title: Tracking the direction of the interstellar wind over a full solar cycle using pickup ions detected by ACE SWICS Authors: Gilbert, J. A.; Gershman, D. J.; Gloeckler, G.; Shearer, P.; Stakhiv, M.; von Steiger, R.; Zurbuchen, T. Bibcode: 2014AGUFMSH11C4059G Altcode: Recent studies regarding the flow direction of interstellar wind through the heliosphere have determined the longitudinal evolution using neutral Helium as an indicator. Ionized interstellar helium that is picked up by the solar wind has also been used to measure the helium focusing cone and determine its longitudinal orientation. This study expands previous pickup ion measurements and provides, for the first time, more than a full solar cycle of continuous pickup ion tracking of the interstellar wind direction. We discuss these results from ACE-SWICS and show how they fit within the context of previous investigations. Title: The Solar Wind Neon Abundance Observed with ACE/SWICS and Ulysses/SWICS Authors: Shearer, Paul; von Steiger, Rudolf; Raines, Jim M.; Lepri, Susan T.; Thomas, Jonathan W.; Gilbert, Jason A.; Landi, Enrico; Zurbuchen, Thomas H. Bibcode: 2014ApJ...789...60S Altcode: Using in situ ion spectrometry data from ACE/SWICS, we determine the solar wind Ne/O elemental abundance ratio and examine its dependence on wind speed and evolution with the solar cycle. We find that Ne/O is inversely correlated with wind speed, is nearly constant in the fast wind, and correlates strongly with solar activity in the slow wind. In fast wind streams with speeds above 600 km s-1, we find Ne/O = 0.10 ± 0.02, in good agreement with the extensive polar observations by Ulysses/SWICS. In slow wind streams with speeds below 400 km s-1, Ne/O ranges from a low of 0.12 ± 0.02 at solar maximum to a high of 0.17 ± 0.03 at solar minimum. These measurements place new and significant empirical constraints on the fractionation mechanisms governing solar wind composition and have implications for the coronal and photospheric abundances of neon and oxygen. The results are made possible by a new data analysis method that robustly identifies rare elements in the measured ion spectra. The method is also applied to Ulysses/SWICS data, which confirms the ACE observations and extends our view of solar wind neon into the three-dimensional heliosphere. Title: The Solar EUV flux in the 3D Heliosphere Authors: Auchere, Frederic; Von Steiger, Rudolf; McMullin, Donald; Newmark, Jeffrey Bibcode: 2014cosp...40E.150A Altcode: The absolute measurement of solar EUV flux and its time dependence provide critical data on the solar driven photo chemistry which results in solar system objects. For example, the Solar HeII 30.4 nm emission is a major contributor to photo-ionization in the heliosphere, and thus 30.4 nm measurements provide the data required to determine the absolute photoionization rate of neutral interstellar helium flowing into our solar system. However, because of the orbit characteristics of the vast majority of spacecraft, the solar irradiance has mostly been measured at Earth or at least in the plane of the ecliptic. Therefore, the existing data ignore the fact that the angular distribution of the solar flux is largely anisotropic. Indeed, in the far and extreme ultraviolet, the chromosphere and the corona display very contrasted structures. At solar minimum, the polar regions are darkened by large coronal holes, and in the most active part of the solar cycle, bright active regions are scattered around the solar globe at low heliocentric latitudes. To date, due to the small number of off- ecliptic measurements, very few attempts have been made to investigate these variations. The implications of the anisotropy of the solar irradiance are diverse. For example, in the case of the 121.6 nm line of H I, the latitudinal anisotropy must be taken into account when modeling the Lyman alpha resonantly backscattered sky background. Identically, the anisotropy must be included in the modeling of the intensity of the HI 121.6 nm and He II 30.4 nm resonantly scattered coronal lines. We present here a generalization of an earlier work on the anisotropy of the 30.4 nm EUV flux. Our empirical model, is now able to synthethize solar spectra as seen from any point in the heliosphere in the 10 to 50 nm wavelength range. The model is based on a Differential Emission Measure resonstruction of the spectrum from reprojected EUV Carrington maps of the Sun. We present the results obtained on the 3D distribution of the Solar EUV flux during solar cycle 23. We discuss their consequences on the GAS/Ulysses measurements of the Helium abundance in the Local Interstellar Medium. Title: Cosmic Rays in the Heliosphere Authors: Heber, Bernd; Kóta, József; von Steiger, Rudolf Bibcode: 2014crh..book.....H Altcode: No abstract at ADS Title: Foreword Authors: Heber, Bernd; Kóta, József; von Steiger, Rudolf Bibcode: 2014crh..book....1H Altcode: No abstract at ADS Title: Sources of the solar wind - the heliospheric point of view Authors: Von Steiger, Rudolf; Shearer, Paul; Zurbuchen, Thomas Bibcode: 2014cosp...40E3557V Altcode: The solar wind as observed in the heliosphere has several properties that can be interpreted as signatures of conditions and processes at its source in the solar atmosphere. Traditionally it has been customary to distinguish between solar wind types solely based on its speed, "fast" and "slow" wind. Over the last couple of decades new instruments resolving not only the main constituents (protons and alpha particles) but also heavy ions from C to Fe have added new observables, in particular the charge state and elemental composition of these ions. The charge states are indicators of the coronal temperature at the source region; they have confirmed that the "fast" wind emanates from the relatively cool coronal hole regions, while the "slow" wind originates from hotter sources such as the streamer belt and active regions. Thus they are more reliable indicators of solar wind source than the speed alone could be because they readily discriminate between "fast" wind from coronal holes and fast coronal mass ejections (CMEs). The elemental composition in the solar wind compared to the abundances in the photosphere shows a typical fractionation that depends on the first ionization potential (FIP) of the elements. Since that fractionation occurs beneath the corona, in the chromosphere, its strength is indicative of the conditions in that layer. While the "fast" wind is very similar to photospheric composition, the fractionation of the "slow" wind and of CMEs is higher and strongly variable. We will review the observations of the SWICS composition instruments on both the ACE and the Ulysses missions, which have made composition observations between 1 and 5 AU and at all latitudes in the heliosphere over the last two decades. Specifically, analysis of the "slow" wind observations at all time scales, from hours to complete solar cycles, will be used to better characterize its source regions. Title: Foreword Authors: Heber, Bernd; Kóta, József; von Steiger, Rudolf Bibcode: 2013SSRv..176....1H Altcode: 2013SSRv..tmp...69H No abstract at ADS Title: Foreword Authors: Burgess, David; Drake, James; Marsch, Eckart; Velli, Marco; von Steiger, Rudolf; Zurbuchen, Thomas H. Bibcode: 2013mspc.book....1B Altcode: No abstract at ADS Title: Multi-scale Physics in Coronal Heating and Solar Wind Acceleration Authors: Burgess, David; Drake, James; Marsch, Eckart; von Steiger, Rudolf; Velli, Marco; Zurbuchen, Thomas Bibcode: 2013mspc.book.....B Altcode: No abstract at ADS Title: Sources of Solar Wind at Solar Minimum: Constraints from Composition Data Authors: Zurbuchen, Thomas H.; von Steiger, Rudolf; Gruesbeck, Jacob; Landi, Enrico; Lepri, Susan T.; Zhao, Liang; Hansteen, Viggo Bibcode: 2013mspc.book...41Z Altcode: No abstract at ADS Title: Spatially Dependent Heating and Ionization in an ICME Observed by Both ACE and Ulysses Authors: Lepri, Susan T.; Laming, J. Martin; Rakowski, Cara E.; von Steiger, Rudolf Bibcode: 2012ApJ...760..105L Altcode: The 2005 January 21 interplanetary coronal mass ejection (ICME) observed by multiple spacecraft at L1 was also observed from January 21-February 4 at Ulysses (5.3 AU). Previous studies of this ICME have found evidence suggesting that the flanks of a magnetic cloud like structure associated with this ICME were observed at L1 while a more central cut through the associated magnetic cloud was observed at Ulysses. This event allows us to study spatial variation across the ICME and relate it to the eruption at the Sun. In order to examine the spatial dependence of the heating in this ICME, we present an analysis and comparison of the heavy ion composition observed during the passage of the ICME at L1 and at Ulysses. Using SWICS, we compare the heavy ion composition across the two different observation cuts through the ICME and compare it with predictions for heating during the eruption based on models of the time-dependent ionization balance throughout the event. Title: Origin of the most strongly FIP-fractionated solar wind: Ulysses SWICS results Authors: von Steiger, R.; Zurbuchen, T. Bibcode: 2012AGUFMSH52A..03V Altcode: The slow solar wind is one of two quasi-stationary states whose origin - unlike the one of fast wind, which clearly emanates from coronal holes - is much less understood, but must be associated with the coronal streamer belt. The slow wind is also much more variable than its fast counterpart in virtually all parameters, both kinetic and compositional. In order to better pinpoint and characterize its sources and establish observational constraints for the origin of this unusual solar wind plasma we investigate in this paper periods of the most metal-rich solar wind. During such periods ions with a low First Ionization Potential (FIP) such as Fe, Mg, and Si are observed to be enhanced well over the average coronal ratios. We find that these time periods occur in two different heliospheric contexts: within Coronal Mass Ejections (CMEs) and near the Heliospheric Current Sheet (HCS). The CME-associated enhancements have highly elevated Fe charge states (average QFe > 11.5) and also exhibit the well-reported enhancements in alpha particles (α/p > 8 %). Similarly, ionic charge state ratios of C and O are also enhanced, suggesting the presence of intense heating near the Sun. On the other hand, HCS-associated events exhibit some of the coolest Fe charge states observed during the entire mission (QFe < 9.5) and, and exhibit depletions of alpha particles (α/p < 3%). The ionic charge state ratios of C and O do not show any enhancements as compared to the ambient wind that has nominal Mg/O. We put this observational result in the context of theories that predict the origin, heating and acceleration of the slow solar wind. We conclude that highly fractionated CME plasma and the slow wind near the HCS have a common origin in the closed corona and are both intermittently released into the heliosphere. Title: Foreword Authors: Burgess, David; Drake, James; Marsch, Eckart; Velli, Marco; von Steiger, Rudolf; Zurbuchen, Thomas H. Bibcode: 2012SSRv..172....1B Altcode: 2012SSRv..tmp...85B No abstract at ADS Title: Sources of Solar Wind at Solar Minimum: Constraints from Composition Data Authors: Zurbuchen, Thomas H.; von Steiger, Rudolf; Gruesbeck, Jacob; Landi, Enrico; Lepri, Susan T.; Zhao, Liang; Hansteen, Viggo Bibcode: 2012SSRv..172...41Z Altcode: 2012SSRv..tmp...25Z In this discussion of observational constraints on the source regions and acceleration processes of solar wind, we will focus on the ionic composition of the solar wind and the distribution of charge states of heavy elements such as oxygen and iron. We first focus on the now well-known bi-modal nature of solar wind, which dominates the heliosphere at solar minimum: Compositionally cool solar wind from polar coronal holes over-expands, filling a much larger solid angle than the coronal holes on the Sun. We use a series of remote and in-situ characteristics to derive a global geometric expansion factor of ∼5. Slower, streamer-associated wind is located near the heliospheric current sheet with a width of 10-20°, but in a well-defined band with a geometrically small transition width. We then compute charge states under the assumption of thermal electron distributions and temperature, velocity, and density profiles predicted by a recent solar wind model, and conclude that the solar wind originates from a hot source at around 1 million K, characteristic of the closed corona. Title: Composition of the Solar Corona, Solar Wind, and Solar Energetic Particles Authors: Schmelz, J. T.; Reames, D. V.; von Steiger, R.; Basu, S. Bibcode: 2012ApJ...755...33S Altcode: Along with temperature and density, the elemental abundance is a basic parameter required by astronomers to understand and model any physical system. The abundances of the solar corona are known to differ from those of the solar photosphere via a mechanism related to the first ionization potential of the element, but the normalization of these values with respect to hydrogen is challenging. Here, we show that the values used by solar physicists for over a decade and currently referred to as the "coronal abundances" do not agree with the data themselves. As a result, recent analysis and interpretation of solar data involving coronal abundances may need to be revised. We use observations from coronal spectroscopy, the solar wind, and solar energetic particles as well as the latest abundances of the solar photosphere to establish a new set of abundances that reflect our current understanding of the coronal plasma. Title: The Ulysses Legacy Authors: Von Steiger, Rudolf Bibcode: 2012cosp...39.2102V Altcode: 2012cosp.meet.2102V The Ulysses mission was the first space mission to reach genuine high latitudes in the heliosphere, and is the only one to do so to this day. Launched in 1990, it has provided nearly two decades of unprecedented and groundbreaking observations. Thus it has added to our picture of the heliosphere not only the third, out-of-ecliptic, dimension, but also the fourth, time, of almost a full magnetic (Hale) cycle of the Sun. Now that Ulysses has ceased to operate and as we are thinking about future out-of-ecliptic missions it is a good time to pause and review the Ulysses legacy. We will present and review the highlights of what Ulysses has been teaching us about the heliosphere: e.g., the two states of the solar wind, there unexpected structure of the polar magnetic field and what it means for access of cosmic rays, how the magnetic field reverses polarity at solar maximum, and even fortuitous encounters with the tails of distant comets. Finally, we will also review the impact of the lack of imaging instrumentation on Ulysses. Title: Cosmogenic Radionuclides Authors: Beer, Jürg; McCracken, Ken; von Steiger, Rudolf Bibcode: 2012cora.book.....B Altcode: No abstract at ADS Title: Cosmogenic Radionuclides Authors: Beer, Jürg; McCracken, Ken; von Steiger, Rudolf Bibcode: 2012crta.book.....B Altcode: 2012cora.book.....B No abstract at ADS Title: Variability of the solar wind Authors: von Steiger, R.; Zurbuchen, T.; Balogh, A. Bibcode: 2011AGUFMSH11C..03V Altcode: Using data from the entire Ulysses mission (1990-2009) we quantify the variability of the solar wind using distributions of mass, momentum, and total energy measurements in the wind. For this analysis, we separate solar wind measurements according to its two dynamic states - "fast" and "slow" wind. With the advent of composition instrumentation it could be shown that heavy ion charge states are a significantly improved and more physical way for the distinction of these two states. "Fast" wind originates in relatively cool coronal holes, while the source of the "slow" wind is much less clear but must be near or above the streamer belt. Reflecting the properties of their coronal source regions, the "slow" wind is much more variable than its "fast" counterpart. In extreme cases the "slow" wind can have a speed of close to 1000 km/s. We typically find log-normal distributions of these parameters that are about three times wider in the "slow" wind, even for the momentum flux, which was often considered the least variable solar wind parameter. These data should provide important constraints for studies of solar wind turbulence. Title: Polar coronal holes during the past solar cycle: Ulysses observations Authors: von Steiger, Rudolf; Zurbuchen, Thomas H. Bibcode: 2011JGRA..116.1105V Altcode: During its nearly 19-year mission, Ulysses pioneered novel measurements of the three-dimensional heliosphere and particularly in situ observations of high-latitude solar wind from polar coronal holes (PCHs). Winds from PCHs exhibit constant elemental abundances to within the limits of the measurements, indicative of the fact that such winds truly provide a ground state of solar wind composition. However, these solar wind streams show long-term variability in the composition of ionic charge states frozen into the low corona. The C and O freeze-in temperatures measured in high-latitude solar wind have decreased ∼10% as compared to the previous solar minimum and are now around 0.87 and 1.01 MK, respectively. The ionization states of Si and Fe also exhibit a substantial cooling with a reduction of 0.4 and 0.5 charge states, respectively. We show that these observations are indicative of an overall decrease of coronal temperature, forming a trend toward cooler PCH temperature persisting for over 14 years. We support these observations with a detailed and comprehensive description of the data analysis processes relevant for Ulysses SWICS and similar instruments. Title: Oxygen Flux in the Solar Wind: Ulysses Observations Authors: von Steiger, R.; Zurbuchen, T.; McComas, D. J. Bibcode: 2010AGUFMSH33C..01V Altcode: We use the complete set of Ulysses solar wind data to conduct a comprehensive determination of the oxygen flux in relation to the proton flux in the solar wind during a wide range of solar activity levels. The data cover the heliosphere between 1.3 and 5.4 AU and, due to the unique orbit of Ulysses, all of the heliographic latitudes within ±80°. We find log-normal distributions for O and H daily flux values, but with significant differences between slow and fast wind. Coronal hole-associated fast wind has a distribution that is approximately three times narrower than the one of slow wind associated with streamers. Finally, we derive the solar oxygen abundance, finding a value of H/O=1500±300, and discuss this value in comparison with the results of spectroscopic determinations. Title: Oxygen flux in the solar wind: Ulysses observations Authors: von Steiger, Rudolf; Zurbuchen, Thomas H.; McComas, David J. Bibcode: 2010GeoRL..3722101V Altcode: We use the complete set of Ulysses solar wind data to conduct a comprehensive determination of the oxygen flux in relation to the proton flux in the solar wind during a wide range of solar activity levels. The data cover the heliosphere between 1.3 and 5.4 AU and, due to the unique orbit of Ulysses, all of the heliographic latitudes within ±80°. We find log-normal distributions for O and H daily flux values, but with significant differences between slow and fast wind. Coronal hole-associated fast wind has a distribution that is approximately three times narrower than the one of slow wind associated with streamers. Finally, we derive the solar oxygen abundance, finding a value of 8.82 ± 0.08, and discuss this value in comparison with the results of spectroscopic determinations. Title: Turbulence in the Solar Atmosphere and Solar Wind Authors: Petrosyan, A.; Balogh, A.; Goldstein, M. L.; Léorat, J.; Marsch, E.; Petrovay, K.; Roberts, B.; von Steiger, R.; Vial, J. C. Bibcode: 2010SSRv..156..135P Altcode: 2010SSRv..tmp..117P The objective of this review article is to critically analyze turbulence and its role in the solar atmosphere and solar wind, as well as to provide a tutorial overview of topics worth clarification. Although turbulence is a ubiquitous phenomenon in the sun and its heliosphere, many open questions exist concerning the physical mechanisms of turbulence generation in solar environment. Also, the spatial and temporal evolution of the turbulence in the solar atmosphere and solar wind are still poorly understood. We limit the scope of this paper (leaving out the solar interior and convection zone) to the magnetized plasma that reaches from the photosphere and chromosphere upwards to the corona and inner heliosphere, and place particular emphasis on the magnetic field structures and fluctuations and their role in the dynamics and radiation of the coronal plasma. To attract the attention of scientists from both the fluid-dynamics and space-science communities we give in the first two sections a phenomenological overview of turbulence-related processes, in the context of solar and heliospheric physics and with emphasis on the photosphere-corona connection and the coupling between the solar corona and solar wind. We also discuss the basic tools and standard concepts for the empirical analysis and theoretical description of turbulence. The last two sections of this paper give a concise review of selected aspects of oscillations and waves in the solar atmosphere and related fluctuations in the solar wind. We conclude with some recommendations and suggest topics for future research. Title: Solar Wind Properties During the Current Solar Minimum: Ulysses Observations Authors: von Steiger, Rudolf; Zurbuchen, Thomas H. Bibcode: 2010EGUGA..12.5006V Altcode: During its nearly 19 year mission, Ulysses pioneered novel measurements of the three-dimensional heliosphere and particularly first in situ observations of solar wind from polar coronal holes (PCHs). It is thus possible to compare observations in the current, peculiar solar minimum with those obtained in 1994-95. It has been reported earlier that, during the current minimum, there is a ~ 15% reduction of the heliospheric magnetic field (Smith and Balogh, 2008), and ~ 17% and ~ 14% reduction in density and temperature, respectively (McComas et al., 2008), as compared to the previous minimum. But the PCH-associated solar wind streams show long-term variability not only in dynamic, but also in compositional signatures. From 1995 to 2008, the C and O freeze-in temperatures measured in high-latitude solar wind have decreased by ~ 15% and are now around 0.86 MK and 1.0 MK, respectively. Si and Fe ionization states also exhibit a substantial cooling with a reduction of 0.2 and 0.3 charge states, respectively. Thus it appears that the PCH of cycle 23 are cooler overall than those of cycle 22. It is more difficult to assess whether there are significant changes of the elemental composition of the solar wind, as exhibited through the First Ionization Potential fractionation effect, which seems to have remained at f = 1.8 ± 0.3 during both sets of polar passages, i.e., enhanced to the photospheric composition (f = 1). If this can be confirmed the streams from PCH would truly be the 'ground state' of the solar wind. These observations provide a unique test for theories of the solar wind and its composition. We will present results from this data analysis and also provide a discussion of their scientific implications. Title: Division II: Sun and Heliosphere Authors: Melrose, Donald B.; Martinez Pillet, Valentin; Webb, David F.; Bougeret, Jean-Louis; Klimchuk, James A.; Kosovichev, Alexander; van Driel-Gesztelyi, Lidia; von Steiger, Rudolf Bibcode: 2010IAUTB..27..146M Altcode: This report is on activities of the Division at the General Assembly in Rio de Janeiro. Summaries of scientific activities over the past triennium have been published in Transactions A, see Melrose et al. (2008), Klimchuk et al. (2008), Martinez Pillet et al. (2008) and Bougeret et al. (2008). The business meeting of the three Commissions were incorporated into the business meeting of the Division. This report is based in part on minutes of the business meeting, provided by the Secretary of the Division, Lidia van Driel-Gesztelyi, and it also includes reports provided by the Presidents of the Commissions (C10, C12, C49) and of the Working Groups (WGs) in the Division. Title: Solar Wind Properties During the Current Solar Minimum: Ulysses Observations Authors: von Steiger, Rudolf; Zurbuchen, Thomas H. Bibcode: 2010cosp...38.1705V Altcode: 2010cosp.meet.1705V Using Ulysses solar wind composition data it is possible to compare observations in the current, unusual solar minimum with those obtained during the minimum in 1994-95. It has been re-ported earlier that, during the current minimum, there is a ∼ 15% reduction of the heliospheric magnetic field (Smith and Balogh, 2008), and ∼ 17% and ∼ 14% reduction in density and temperature, respectively (McComas et al., 2008), as compared to the previous minimum. But the polar coronal hole (PCH)-associated solar wind streams show long-term variability not only in dynamic, but also in compositional properties. The observed trends provide powerful tools to investigate the properties of the underlying corona during this time. From 1995 to 2008, the C and O freeze-in temperatures measured in high-latitude solar wind have steadily decreased by ∼ 15% and are now around 0.86 MK and 1.0 MK, respectively. Si and Fe ionization states also exhibit a substantial cooling with a reduction of 0.2 and 0.3 charge states, respectively. Thus it appears that all observed PCHs of cycle 23 are cooler overall than those of cycle 22. It is more difficult to assess whether there are significant changes of the elemental composition of the solar wind, as exhibited through the First Ionization Potential fractionation effect, which seems to have remained at f = 1.8 ± 0.3 during all polar passages. These observations provide a unique test for theories of the solar wind and its composition. Furthermore, the comparative analysis of the corona with these data provides important insights about the physical processes that link the Sun and its heliosphere. Title: Polar Coronal Holes during the Past Solar Cycle: Ulysses Observations Authors: von Steiger, R.; Zurbuchen, T. Bibcode: 2009AGUFMSH14A..02V Altcode: During its nearly 19 year mission, Ulysses pioneered novel measurements of the three-dimensional heliosphere and particularly provided the first in situ observations of solar wind from polar coronal holes (PCHs). These PCH-associated solar wind streams show long-term variability in both dynamic and also compositional signatures. Between the polar passages in 1994-95 and in 2007-08, the C and O freeze-in temperatures measured in high-latitude solar wind have decreased by ~15 % and are now around 0.86 MK and 1.0 MK, respectively. Si and Fe ionization states also exhibit a substantial cooling with a reduction of 0.4 and 0.5 charge states on average, respectively. On the other hand, there no significant changes of the elemental composition of the solar wind, as exhibited through the First Ionization Potential fractionation effect, which has remained at f = 1.8±0.3 during both sets of polar passages, i.e., enhanced to the photospheric composition (f = 1). Thus, it appears that the PCH of cycle 23 are cooler overall than those of cycle 22, while their elemental composition has remained unchanged, thus confirming their status as the “ground state” of the solar wind. These observations, together with the observed ~15 % reduction of the heliospheric magnetic field (Smith and Balogh, 2008), and the ~17 % and ~14 % reductions in density and temperature, respectively (McComas et al., 2008), provide a unique test for theories of the solar wind and its composition, in particular for the concept of freezing-in of charge states and of the FIP fractionation effect. We will present results from this analysis of SWICS data and also discuss the scientific implications of these novel results. Title: Turbulence and intermittency in the heliospheric magnetic field in fast and slow solar wind Authors: Yordanova, E.; Balogh, A.; Noullez, A.; von Steiger, R. Bibcode: 2009JGRA..114.8101Y Altcode: 2009JGRA..11408101Y We study the nonuniform solar wind turbulence using high-resolution Ulysses magnetic field data measured at different solar activity level, heliospheric latitudes, and distance. We define several types of solar wind dependent of the coronal region of origin and also of the dynamical behavior of the different streams, namely, “pure” fast wind, fast streams, “pure” slow wind, and slow streams. The turbulent properties of the solar wind types were investigated in terms of their scaling properties and spatial inhomogeneity. A clear trend in the power spectrum of the solar wind magnetic field magnitude is observed: the “pure” fast wind has a slope ∼-1.33 (1/f-like), the fast streams ∼-1.48 (Kraichnan-like), the “pure” slow wind ∼-1.67 (Kolmogorov-like), and the slow streams ∼-1.72. We find that the “pure” fast wind in the polar heliolatitudes is less intermittent than the other types: “pure” slow wind and both slow and fast streams, which is because of the absence of dynamical interactions between streams with different speeds. On the other hand, fast streams are more intermittent than the “pure” fast wind, and slow streams are less intermittent than the “pure” slow winds. A clear radial and latitudinal evolution of the intermittency is observed only for the “pure” fast wind, while in the equatorial plane, the fast streams, the “pure” slow wind, and the slow streams do not show evolution either in heliolatitude or in heliocentric distance. Title: Quiescent current sheets in the solar wind and origins of slow wind Authors: Suess, S. T.; Ko, Y. -K.; von Steiger, R.; Moore, R. L. Bibcode: 2009JGRA..114.4103S Altcode: 2009JGRA..11404103S Solar wind near the heliospheric current sheet is investigated using Ulysses and ACE data in a superposed epoch analysis for several days on either side of the current sheets. Only data near sunspot minima are used, minimizing the influence of transients. New results are shown for composition and ionization state. Existing results showing a ∼2 day wide depletion in He/H (He++/H+) at the current sheet are confirmed, although the depletion is generally more narrow. A recent finding of a broad 5-10 day wide reduction in He/H around the current sheet is also confirmed. An important result is that the narrow depletion is not a real phenomenon but is instead a statistical consequence of the superposition of transient depletions that also create the broad reduction in the averages. These transient depletions last from a few hours up to several days, come from the core of streamers, and are embedded in a quasi-steady flow from streamers' legs. Most depletions contain a current sheet just inside one edge, leading to the apparent narrow depletion at the current sheet in the superposed epoch analysis. These results lead us to a hypothesis for how the He/H depletions form with a current sheet just inside one edge. Fe/O fluctuations associated with the He/H fluctuations further show that mixing of plasma from coronal holes adjacent to streamer brightness boundaries into outflow inside the brightness boundary is not an important process. Title: Division II: Sun and Heliosphere Authors: Melrose, Donald B.; Martínez Pillet, Valentin; Webb, David F.; van Driel-Gesztelyi, Lidia; Bougeret, Jean-Louis; Klimchuk, James A.; Kosovichev, Alexander; von Steiger, Rudolf Bibcode: 2009IAUTA..27...73M Altcode: Division II of the IAU provides a forum for astronomers and astrophysicists studying a wide range of phenomena related to the structure, radiation and activity of the Sun, and its interaction with the Earth and the rest of the solar system. Division II encompasses three Commissions, 10, 12 and 49, and four Working Groups. Title: From the Outer Heliosphere to the Local Bubble Authors: Linsky, J. L.; Izmodenov, V. V.; Möbius, E.; von Steiger, R. Bibcode: 2009fohl.book.....L Altcode: No abstract at ADS Title: Commission 49: Interplanetary Plasma and Heliosphere Authors: Bougeret, Jean-Louis; von Steiger, Rudolf; Webb, David F.; Ananthakrishnan, Subramanian; Cane, Hilary V.; Gopalswamy, Natchimuthuk; Kahler, Stephen W.; Lallement, Rosine; Sanahuja, Blai; Shibata, Kazunari; Vandas, Marek; Verheest, Frank Bibcode: 2009IAUTA..27..124B Altcode: Commission 49 covers research on the solar wind, shocks and particle acceleration, both transient and steady-state, e.g., corotating, structures within the heliosphere, and the termination shock and boundary of the heliosphere. Title: Quiescent Current Sheets in the Solar Wind and Origins of Slow Wind Authors: Suess, S. T.; Ko, Y. -; von Steiger, R.; Moore, R. L. Bibcode: 2008AGUFMSH43B..03S Altcode: Solar wind near the heliospheric current sheet is investigated using Ulysses and ACE data, in a superposed epoch analysis for several days on either side of the current sheets. Only data near sunspot minima are used, minimizing the influence of transients. New results are shown for composition and ionization state. Existing results showing a ~2 day wide depletion in He/H at the current sheet are confirmed, although the depletion is generally more narrow. A recent finding of a broad 5-10 day wide reduction in He/H around the current sheet is also confirmed. An important result is that the narrow depletion is not a real phenomenon, but is instead a statistical consequence of the superposition of transient depletions that also create the broad reduction in the averages. These transient depletions last from a few hours up to several days, come from the core of streamers, and are embedded in a quasi-steady flow from streamers legs. Most depletions contain a current sheet just inside one edge, leading to the apparent narrow depletion at the current sheet in the superposed epoch analysis. These results lead us to a hypothesis for how the He/H depletions form with a current sheet just inside one edge. Fe/O fluctuations associated with the He/H fluctuations further show that mixing of plasma from coronal holes adjacent to streamer brightness boundaries into outflow inside the brightness boundary is not an important process. Title: Solar EUV Spectral Irradiance Throughout The 3-Dimensional Heliosphere Authors: McMullin, D. R.; Auchere, F.; Cook, J. W.; Newmark, J. S.; Quemerais, E.; von Steiger, R.; Witte, M. Bibcode: 2008AGUFMSH13B1522M Altcode: When Ulysses moved from 30 to 80 degrees in solar latitude (July 2001), the Ulysses GAS instrument measured an apparent increase in the neutral He density. This is more naturally interpreted as a latitudinal dependence (decrease) of the loss rate due to solar photoionization rather than a true increase of the neutral He density. This concept has been tested through the development of a 3-Dimensional solar EUV model for the Heliosphere. The model concept has been presented earlier, and we are now presenting results and applications of the new model. Using daily SOHO EIT observations, over successive Carrington rotations, we have developed a three- dimensional model for solar EUV fluxes observed at any heliospheric position, projected to any heliospheric position. The combined effects of solar rotational and latitude-dependent flux variability are explicitly treated in this model. The flux model will be compared with other direct spectral irradiance observations in the ecliptic plane, such as those available from the TIMED SEE instrument as well as broadband measurements available from the SOHO/SEM irradiance time series. These comparisons will be used in part to validate the current results. We then use this flux to compute the photoionization rate of the in-flowing neutral Helium, and compare the modeled change with that observed along the spacecraft trajectory with the direct measurements from the out-of-ecliptic Ulysses GAS observations. The unique GAS comparisons will provide validation of the original hypothesis as to the latitudinal dependence (decrease) of the loss rate due to solar photoionization rather than an increase of the neutral He density. Title: Fe, O, and C Charge States Associated With Quiescent Versus Active Current Sheets in the Solar Wind Authors: Suess, S. T.; Ko, Y.; von Steiger, R. Bibcode: 2008AGUSMSH44A..07S Altcode: Ulysses MAG data were used to locate the heliospheric current sheet in data from 1991 through 2006. The purpose was to characterize typical charge states for Fe, O, and C in the vicinity of the current sheet and provide insight into the physical sources for these charge states in the corona. A study of He/H around the current sheets has led to a clear distinction between quiescent current sheets at times of low solar activity and active current sheets associated with magnetic clouds (and, presumably, ICMEs). It has been shown that high ionization state Fe is produced in the corona in current sheets associated with CMEs through spectroscopic observations of the corona and through in situ detection at Ulysses. Here we show that the ionization state of Fe is typically only enhanced around active current sheets. The ionization states of O and C are commonly enhanced around both quiescent and active current sheets, but the enhancements are much larger around active current sheets. This is consistent with UV coronal spectroscopy, which has shown that reconnection in current sheets behind CMEs leads to high temperatures not typically seen above quiet streamers. Title: Composition of the Solar Wind Authors: von Steiger, Rudolf Bibcode: 2008cosp...37.3366V Altcode: 2008cosp.meet.3366V The motivation for systematic observations of the solar wind composition is twofold: (1) It may be used to deduce the composition of the protosolar nebula from which the entire solar system was made 4.6 gigayears ago, thus representing a sample of the galactic chemical evolution at that time and location. (2) It is a tracer of conditions and processes in the solar atmosphere where the solar wind is accelerated, thus providing information about the structure of the corona. With the launch of a new type of composition sensor on the Ulysses mission in 1990 we have now a database of ten elements in more than 30 charge states during more than a complete solar activity cycle. Together with Ulysses' unique, high-inclination orbit that database reveals much about the three-dimensional structure of not just the solar atmosphere, but also of the heliosphere as a whole. We will review the Ulysses observations of solar wind composition both in its quasi-stationary states, steady fast streams and variable slow wind, as well as in its transient states such as coronal mass ejections, and their significance for the structure of the heliosphere. Title: Mercury Authors: Balogh, André; Ksanfomality, Leonid; von Steiger, Rudolf Bibcode: 2008merc.book.....B Altcode: No abstract at ADS Title: The solar wind throughout the solar cycle Authors: von Steiger, Rudolf Bibcode: 2008hsac.book...41V Altcode: The existence of solar corpuscular radiation (SCR) was conjectured by Biermann (1951) based on the fact that the ion tails of comets always point radially away from the Sun. Earlier it had been thought that this was due to solar radiation pressure, but when the relevant cross-sections were measured it became clear that these were far too small. This is visible in Figure 3.1, where stars can be seen shining through the ion tail of comet Hale-Bopp, one of the more spectacular sights in the sky of the 20th century. Parker (1958) provided the first theoretical description of the SCR in terms of a supersonic magnetized fluid. He coined the term "solar wind" in order to set it apart from other ideas of a (subsonic) solar breeze that were around at the time. The solar wind was ultimately observed in the early 1960s by the Soviets and independently with the American Mariner 2 mission to Venus (Gringauz et al., 1961; Neugebauer and Snyder, 1962). An excellent account of these early developments is given by Parker (2001). Title: Introduction Authors: Balogh, André; Ksanfomality, Leonid; von Steiger, Rudolf Bibcode: 2008merc.book....1B Altcode: No abstract at ADS Title: Calibration of Particle Instruments in Space Physics Authors: Wüest, Martin; Evans, David S.; von Steiger, Rudolf Bibcode: 2007cpis.book.....W Altcode: No abstract at ADS Title: Ulysses Transition into the Polar Coronal Holes Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2007AGUFMSH14A1700V Altcode: The Ulysses spacecraft has now half-completed its third polar orbit around the Sun. Like the first polar orbit, in 1992-1998, it is occurring at declining to minimum solar activity. Yet the two transitions into the hole are remarkably different. The first transition was substantially more regular than the second one is. This may be understood in the context of the current sheet orientation, which was generally flatter during the first transition, but is more strongly warped during the second. We model the global distribution of slow and fast solar wind streams starting from the Wilcox Solar Observatory maps of the solar magnetic field at the source surface. The model assumes slow solar wind to emanate from the vicinity of the current sheet with a speed that increases as a function of angular distance from the CS, i.e., with magnetic latitude, as it has been found on Helios. Fast solar wind of constant speed is assumed to emanate from the coronal holes and to expand superradially so as to fill the entire solid angle above a certain magnetic latitude. Thus we obtain a model solar wind speed at the position of Ulysses, and comparing to the observed solar wind speed there we can optimize the model to finally obtain the angular width of the belt of slow solar wind around the heliospheric current sheet. Title: Introduction Authors: Balogh, André; Ksanfomality, Leonid; von Steiger, Rudolf Bibcode: 2007SSRv..132..183B Altcode: 2007SSRv..tmp..216B No abstract at ADS Title: Encounter of the Ulysses Spacecraft with the Ion Tail of Comet MCNaught Authors: Neugebauer, M.; Gloeckler, G.; Gosling, J. T.; Rees, A.; Skoug, R.; Goldstein, B. E.; Armstrong, T. P.; Combi, M. R.; Mäkinen, T.; McComas, D. J.; von Steiger, R.; Zurbuchen, T. H.; Smith, E. J.; Geiss, J.; Lanzerotti, L. J. Bibcode: 2007ApJ...667.1262N Altcode: Comet McNaught was the brightest comet observed from Earth in the last 40 years. For a period of five days in early 2007 February, four instruments on the Ulysses spacecraft directly measured cometary ions and key properties of the interaction of the comet's ion tail with the high-speed solar wind from the polar regions of the Sun. Because of the record-breaking duration of the encounter, the data are unusually comprehensive. O3+ ions were detected for the first time in a comet tail, coexisting with singly charged molecular ions with masses in the range 28-35 amu. The presence of magnetic turbulence and of ions with energies up to ~200 keV indicate that at a distance of ~1.6 AU from the comet nucleus, the ion tail of comet McNaught had not yet reached equilibrium with the surrounding solar wind. Title: Encounter of Ulysses with Comet McNaught Authors: Gosling, J. T.; Neugebauer, M.; McComas, D. J.; Goldstein, B. E.; Skoug, R. M.; Gloeckler, G.; Zurbuchen, T.; von Steiger, R.; Balogh, A.; Rees, A.; Combi, M. R. Bibcode: 2007AGUSMSH23C..05G Altcode: Comet C/2006 P1 McNaught was the brightest comet observed from Earth in the last 40 years. On February 3, 2007 the comet at a heliocentric distance of ~0.71 AU was nearly radially aligned with the Ulysses spacecraft at a heliocentric distance of ~2.40 AU and at 79 Deg south heliographic latitude. Thus, during a ~4.5-day interval (February 5-9) Ulysses encountered the tail region of this spectacular comet, the region of disturbance in the solar wind produced by the comet being nearly 10 Mkm wide at 2.4 AU. During the encounter the speed of the solar wind dropped from ~750 km/s to a minimum of 360 km/s, the proton density dropped by more than 2 orders of magnitude, and the proton temperature increased from ~1.5x105 to ~4x105 K, while simultaneously very large fluxes of cometary molecular and singly and doubly charged atomic ions were detected. The slowing, depletion and heating of the solar wind proton beam was a result of charge exchange with neutral atoms and molecules in the cometary atmosphere and with the pickup up by the wind of the newly-born cometary ions. Although no shocks were observed during the encounter, the magnetic field strength was slightly enhanced in broad regions at the leading and trailing edges of the tail of the comet and was generally weaker than in the unobstructed solar wind within the heart of the region of interaction. For most of the encounter, the magnetic field direction was nearly radially inward, and thus reversed from its normal outward direction in the southern polar hemisphere at this phase of the present solar cycle. There were, however, shorter periods when the field pointed nearly radially outward, indicating a filamentary structure of the comet tail. One of the intervals of radially outward field coincided with the interval of minimum flow speed and maximum flux of picked up O+ ions. Title: Commission 49: Interplanetary Plasma and Heliosphere Authors: Webb, David F.; Bougeret, Jean-Louis; Cane, Hilary V.; Cramer, Neil F.; Kahler, Stephen W.; Kojima, Masayoshi; Sanahuja, Blai; Vandas, Marek; Verheest, Frank; von Steiger, Rudolf Bibcode: 2007IAUTA..26..103W Altcode: Commission 49 covers research on the solar wind, shocks and particle acceleration, both transient and steady-state, e.g., corotating, structures within the heliosphere, and the termination shock and boundary of the heliosphere. During the last three years there was considerable progress made in studies of solar energetic particles, compositional and other signatures in the heliosphere, solar wind pickup ions, the termination shock, which was finally crossed by a spacecraft, and the boundary between the heliosphere and interstellar medium, and in solar wind modeling and space weather. These topics have been summarized here in five articles, each with extensive references that will guide the reader who wants further details. Observations from the following spacecraft have extensively used during this period: Ulysses, Cassini, Voyager 1 and 2, MESSENGER, ACE, Genesis, SOHO, Wind, and RHESSI. Title: Solar Dynamics and Its Effects on the Heliosphere and Earth Authors: Baker, D. N.; Klecker, B.; Schwartz, S. J.; Schwenn, R.; von Steiger, R. Bibcode: 2007sdeh.book.....B Altcode: No abstract at ADS Title: The Composition of Matter: Symposium honouring Johannes Geiss on the occasion of his 80th Birthday Authors: von Steiger, Rudolf; Gloeckler, George; Mason, Glenn M. Bibcode: 2007coma.book.....V Altcode: No abstract at ADS Title: Coronal Mass Ejections Authors: Kunow, H.; Crooker, N. U.; Linker, J. A.; Schwenn, R.; von Steiger, R. Bibcode: 2007cme..conf.....K Altcode: No abstract at ADS Title: Foreword Authors: von Steiger, R.; Gloeckler, G.; Mason, G. M. Bibcode: 2007coma.book....1V Altcode: No abstract at ADS Title: Large-scale heliospheric structure in 2004-2006 and its solar origin Authors: Rother, O.; Wimmer-Schweingruber, R. F.; von Steiger, R.; Zurbuchen, T. H. Bibcode: 2006AGUFMSH44A..01R Altcode: As solar activity has begun to decline, the large-scale structure of the heliosphere has begun to turn simpler again. Large coronal holes and a more quiet streamer belt are structuring the heliosphere. Ulysses, on its unique orbit, has again begun to measure recurrent high-speed streams originating in coronal holes alternating with slow wind from other regions. Here, we use simple back-mapping techniques to identify the source regions of the solar wind measured by Ulysses. We relate the observed stream interfaces to solar features and give a complete list of stream interfaces for 2004 - 2006. Title: Ulysses Transition into the Newly Formed Southern Fast Stream Observed with Ulysses- SWICS Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2006AGUFMSH52A..07V Altcode: The Ulysses spacecraft currently performs the third revolution on its unique, high-inclination orbit around the Sun. Like on the first orbit the current observations are taken during the declining to minimum phase of the solar activity cycle, albeit with inverted magnetic polarity. However, our observations show rather significant and surprising differences between the configurations of the Heliosphere during the first and the third orbits of Ulysses. In 1992-93 the transition from the slow, variable solar wind into the high-speed stream from the southern polar coronal hole was marked by a regular oscillation from slow to fast solar wind and back once every solar rotation for more than a year, indicating a relatively flat but tilted heliospheric current sheet. The current transition has been much less regular, with slow and variable solar wind pertaining to higher latitudes than back then. The transition proper was much quicker, with duration of only 2-3 solar rotations. Since early 2006 Ulysses is now immersed in the polar fast stream, but this looks also somewhat different than the previous one as it shows some variability and may even contain coronal mass ejections with a composition signature, something that was never observed during more than 2.5 years of polar stream observations in the previous cycle. Title: Planetary Systems and Planets in Systems Authors: Udry, Stéphane; Benz, Willy; von Steiger, Rudolf Bibcode: 2006psps.conf.....U Altcode: No abstract at ADS Title: On the Solar Wind Elemental Composition: Constraints on the Origin of the Solar Wind Authors: Zurbuchen, T. H.; von Steiger, R. Bibcode: 2006ESASP.617E...7Z Altcode: 2006soho...17E...7Z No abstract at ADS Title: Foreword Authors: Baker, D. N.; Klecker, B.; Schwartz, S. J.; Schwenn, R.; von Steiger, R. Bibcode: 2006SSRv..124D...7B Altcode: The topic of Solar Dynamics and its Effects on the Heliosphere and Earth was addressed with a workshop at the International Space Science Institute, under the auspices of the International Living with a Star program, held in April 2005. 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 final section was devoted to common physical processes occuring both at the Sun and in the magnetosphere such as reconnection, shock acceleration, dipolarisation of magnetic field, and others. Title: Kinetic properties of heavy solar wind ions from Ulysses-SWICS Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2006GeoRL..33.9103V Altcode: The kinetic properties of heavy ions in the solar wind reflect the plasma processes governing the solar wind in the heliosphere. We use Ulysses-SWICS data that resolve heavy ions in a wide range of mass-per-charge values, 2 <= m/q <= 9.33, to investigate the heavy ions and their dynamic evolution throughout the heliosphere. While at 1 AU the imprint of Coulomb collisions is known to be present in the slow solar wind, we show that is vanishes by the time the wind has reached 5 AU. All ion species flow with equal bulk and thermal speeds there. This is interpreted as a progressive dominance of wave-particle interactions over Coulomb collisions. Title: Foreword Authors: Kunow, H.; Crooker, N. U.; Linker, J. A.; Schwenn, R.; von Steiger, R. Bibcode: 2006SSRv..123....1K Altcode: 2006SSRv..tmp...62K No abstract at ADS Title: ICMEs in the Outer Heliosphere and at High Latitudes: An Introduction Authors: von Steiger, R.; Richardson, J. D. Bibcode: 2006SSRv..123..111V Altcode: 2006SSRv..tmp...65V Interplanetary coronal mass ejections (ICMEs) are observed at all latitudes and distances from which data are available. We discuss the radial evolution of ICMEs out to large distances and ICME properties at high latitudes. The internal pressure of ICMEs initially exceeds the ambient solar wind pressure and causes the ICMEs to expand in radial width to about 15~AU. Large ICMEs and series of ICMEs compress the leading plasma and form merged interaction regions (MIRs) which dominate the structure of the outer heliosphere at solar maximum. The distribution of high-latitude ICMEs is solar cycle dependent. A few overexpanding ICMEs are observed at high-latitude near solar minimum. Near solar maximum ICMEs are observed at all latitudes, but those above 40° do not have high charge states. Title: Understanding Interplanetary Coronal Mass Ejection Signatures. Report of Working Group B Authors: Wimmer-Schweingruber, R. F.; Crooker, N. U.; Balogh, A.; Bothmer, V.; Forsyth, R. J.; Gazis, P.; Gosling, J. T.; Horbury, T.; Kilchenmann, A.; Richardson, I. G.; Richardson, J. D.; Riley, P.; Rodriguez, L.; von Steiger, R.; Wurz, P.; Zurbuchen, T. H. Bibcode: 2006SSRv..123..177W Altcode: 2006SSRv..tmp...66W While interplanetary coronal mass ejections (ICMEs) are understood to be the heliospheric counterparts of CMEs, with signatures undeniably linked to the CME process, the variability of these signatures and questions about mapping to observed CME features raise issues that remain on the cutting edge of ICME research. These issues are discussed in the context of traditional understanding, and recent results using innovative analysis techniques are reviewed. Title: ICMEs at High Latitudes and in the Outer Heliosphere. Report of Working Group H Authors: Gazis, P. R.; Balogh, A.; Dalla, S.; Decker, R.; Heber, B.; Horbury, T.; Kilchenmann, A.; Kota, J.; Kucharek, H.; Kunow, H.; Lario, D.; Potgieter, M. S.; Richardson, J. D.; Riley, P.; Rodriguez, L.; Siscoe, G.; von Steiger, R. Bibcode: 2006SSRv..123..417G Altcode: 2006SSRv..tmp...70G Interplanetary coronal mass ejections (ICMEs) propagate into the outer heliosphere, where they can have a significant effect on the structure, evolution, and morphology of the solar wind, particularly during times of high solar activity. They are known to play an important role in cosmic ray modulation and the acceleration of energetic particles. ICMEs are also believed to be associated with the large global transient events that swept through the heliosphere during the declining phases of solar cycles 21 and 22. But until recently, little was known about the actual behavior of ICMEs at large heliographic latitudes and large distances from the Sun. Over the past decade, the Ulysses spacecraft has provided in situ observations of ICMEs at moderate heliographic distances over a broad range of heliographic latitudes. More recently, observations of alpha particle enhancements, proton temperature depressions, and magnetic clouds at the Voyager and Pioneer spacecraft have begun to provide comparable information regarding the behavior of ICMEs at extremely large heliocentric distances. At the same time, advances in modeling have provided new insights into the dynamics and evolution of ICMEs and their effects on cosmic rays and energetic particles. Title: Coronal Mass Ejections Authors: Kunow, H.; Crooker, N. U.; Linker, J. A.; Schwenn, R.; von Steiger, R. Bibcode: 2006cme..book.....K Altcode: No abstract at ADS Title: IHY Science and Organization in Europe Authors: Bougeret, J. -L.; Briand, C.; Bonet Navaro, J. A.; Breen, A.; Candidi, M.; Georgevia, K.; Harrison, R.; Marsden, R.; Schmieder, B.; von Steiger, R. Bibcode: 2006cosp...36.3226B Altcode: 2006cosp.meet.3226B We present the scientific and organizational approach to the International Heliophysical Year in Europe A summary is given of the First European General Assembly of the IHY that was held in Paris in January 2006 Initiatives and expected returns are described Title: Dynamical processes in critical regions of the heliosphere Authors: von Steiger, Rudolf; Gedalin, Michael Bibcode: 2006AdSpR..38....1V Altcode: No abstract at ADS Title: ICMEs at High Latitudes and in the Outer Heliosphere Authors: Gazis, P. R.; Balogh, A.; Dalla, S.; Decker, R.; Heber, B.; Horbury, T.; Kilchenmann, A.; Kota, J.; Kucharek, H.; Kunow, H.; Lario, D.; Potgieter, M. S.; Richardson, J. D.; Riley, P.; Rodriguez, L.; Siscoe, G.; von Steiger, R. Bibcode: 2006cme..book..417G Altcode: Interplanetary coronal mass ejections (ICMEs) propagate into the outer heliosphere, where they can have a significant effect on the structure, evolution, and morphology of the solar wind, particularly during times of high solar activity. They are known to play an important role in cosmic ray modulation and the acceleration of energetic particles. ICMEs are also believed to be associated with the large global transient events that swept through the heliosphere during the declining phases of solar cycles 21 and 22. But until recently, little was known about the actual behavior of ICMEs at large heliographic latitudes and large distances from the Sun. Over the past decade, the Ulysses spacecraft has provided in situ observations of ICMEs at moderate heliographic distances over a broad range of heliographic latitudes. More recently, observations of alpha particle enhancements, proton temperature depressions, and magnetic clouds at the Voyager and Pioneer spacecraft have begun to provide comparable information regarding the behavior of ICMEs at extremely large heliocentric distances. At the same time, advances in modeling have provided new insights into the dynamics and evolution of ICMEs and their effects on cosmic rays and energetic particles. Title: In-situ and remote observations of CMEs Authors: Rodriguez, Luciano; Zhukov, A. N.; Woch, J.; Krupp, N.; von Steiger, R.; Forsyth, R. Bibcode: 2006IAUS..233..351R Altcode: We present studies on a series of ICMEs detected by Ulysses and for which the solar sources on the Sun could be identified. EUV and white light data are used in order to correlate characteristics seen during eruption with those measured in-situ. Particularly, an attempt was made to find solar features that show a relationship with the type of ICME seen later (i.e. cloud or non-cloud ICME). For magnetic clouds (MC) the chirality of the magnetic field was then analyzed. Finally, the charge states of oxygen ions contained in ICMEs were used to obtain freezing-in temperatures and then compare these with the presence of flares occurring close (spatially and temporally) to the CME eruption.We have found no solar feature that could be used to predict the presence of a MC in interplanetary space, they occur with the same frequency for cloud and non-cloud ICMEs. The chirality of the clouds seems to follow only weakly the hemisphere rule. The presence of solar flares do not seem to be correlated with the oxygen freezing-in temperatures seen in-situ. Title: Latitude Distribution of Interplanetary Coronal Mass Ejections Authors: von Steiger, R.; Zurbuchen, T. H.; Kilchenmann, A. Bibcode: 2006cosp...36.2327V Altcode: 2006cosp.meet.2327V We present an investigation of the latitude distribution of Coronal Mass Ejections CMEs measured in the heliosphere The Interplanetary CMEs ICMEs are identified and analyzed using combined solar wind plasma parameters and composition data from the Ulysses spacecraft during its solar maximum polar pass We first discuss this combined data set and then analyze the latitude distribution of ICMEs found therein We finally compare these results to coronagraph observations of CMEs and to the results of a simple model of the three-dimensional distribution and propagation of CMEs in the heliosphere at solar maximum Title: Understanding Interplanetary Coronal Mass Ejection Signatures Authors: Wimmer-Schweingruber, R. F.; Crooker, N. U.; Balogh, A.; Bothmer, V.; Forsyth, R. J.; Gazis, P.; Gosling, J. T.; Horbury, T.; Kilchenmann, A.; Richardson, I. G.; Richardson, J. D.; Riley, P.; Rodriguez, L.; von Steiger, R.; Wurz, P.; Zurbuchen, T. H. Bibcode: 2006cme..book..177W Altcode: While interplanetary coronal mass ejections (ICMEs) are understood to be the heliospheric counterparts of CMEs, with signatures undeniably linked to the CME process, the variability of these signatures and questions about mapping to observed CME features raise issues that remain on the cutting edge of ICME research. These issues are discussed in the context of traditional understanding, and recent results using innovative analysis techniques are reviewed. Title: ICMEs in the Outer Heliosphere and at High Latitudes: an Introduction Authors: von Steiger, R.; Richardson, J. D. Bibcode: 2006cme..book..111V Altcode: Interplanetary coronal mass ejections (ICMEs) are observed at all latitudes and distances from which data are available. We discuss the radial evolution of ICMEs out to large distances and ICME properties at high latitudes. The internal pressure of ICMEs initially exceeds the ambient solar wind pressure and causes the ICMEs to expand in radial width to about 15 AU. Large ICMEs and series of ICMEs compress the leading plasma and form merged interaction regions (MIRs) which dominate the structure of the outer heliosphere at solar maximum. The distribution of high-latitude ICMEs is solar cycle dependent. A few overexpanding ICMEs are observed at high-latitude near solar minimum. Near solar maximum ICMEs are observed at all latitudes, but those above 40? do not have high charge states. Title: Thermal Properties of Heavy Ions throughout the Heliosphere: 39 Solar Wind Species from Ulysses-SWICS Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2005AGUFMSH14A..06V Altcode: The kinetic properties of heavy ions in the solar wind reflect the kinetic processes governing the solar wind in the heliosphere. We use Ulysses-SWICS data which resolves heavy ions in a wide range of mass per charge, 2≤ m/q≤9.33. In particular, we look for deviations from the canonical behavior of equal bulk speed and equal thermal speed for all heavies. Such deviations are expected to carry signatures of all important kinetic processes in the solar wind, such as wave-particle interactions, and collisional processes. We also discuss a simple model to assess the relative importance of these effects. The Ulysses-SWICS data set is ideally suited for this task due to its extended m/q range, and also its global coverage of the heliosphere up to 5 AU. Title: Latitude Distribution of Interplanetary Coronal Mass Ejections during Solar Maximum Authors: von Steiger, R.; Zurbuchen, T. H.; Kilchenmann, A. Bibcode: 2005ESASP.592..317V Altcode: 2005ESASP.592E..48V; 2005soho...16E..48V No abstract at ADS Title: A Model for Solar EUV Flux Helium Photoionization Throughout the 3-Dimensional Heliosphere Authors: Auchère, F.; McMullin, D. R.; Cook, J. W.; Newmark, J. S.; von Steiger, R.; Witte, M. Bibcode: 2005ESASP.592..327A Altcode: 2005soho...16E..49A; 2005ESASP.592E..49A No abstract at ADS Title: Freezing-In Temperatures of Oxygen, Carbon and Iron in Magnetic Clouds Authors: Rodriguez, L.; Woch, J.; Krupp, N.; Fränz, M.; von Steiger, R.; Cid, C.; Forsyth, R.; Glaß,eier Bibcode: 2005ESASP.592..759R Altcode: 2005soho...16E.155R; 2005ESASP.592E.155R No abstract at ADS Title: Solar Wind from the Coronal Hole Boundaries Authors: Schwadron, N. A.; McComas, D. J.; Elliott, H. A.; Gloeckler, G.; Geiss, J.; von Steiger, R. Bibcode: 2005ESASP.592..645S Altcode: 2005soho...16E.127S; 2005ESASP.592E.127S No abstract at ADS Title: The Heliospheric He II 30.4 nm Solar Flux During Cycle 23 Authors: Auchère, F.; Cook, J. W.; Newmark, J. S.; McMullin, D. R.; von Steiger, R.; Witte, M. Bibcode: 2005ApJ...625.1036A Altcode: Because of the orbit characteristics of the vast majority of spacecraft, the solar flux has predominantly been measured at Earth or at least in the plane of the ecliptic. Therefore, the existing data do not directly demonstrate the fact that the latitudinal distribution of the extreme-ultraviolet (EUV) solar flux is largely anisotropic. Indeed, in the EUV the nonuniform distribution of very contrasted bright features (i.e., active regions) and dark features (i.e., coronal holes) at the surface of the Sun produces both the obvious rotational (or longitudinal) modulation of the flux and also a strong latitudinal anisotropy. Although largely ignored up to now, the latitudinal anisotropy affects the physical conditions in the corona and heliosphere and should therefore be taken into account in several solar and heliospheric physics applications. We describe in this paper a technique for computing the He II 30.4 nm flux at an arbitrary position in the heliosphere from Solar and Heliospheric Observatory (SOHO) EUV Imaging Telescope (EIT) images. This procedure was used to produce daily all-sky maps of the 30.4 nm flux from 1996 January to 2003 August, covering the first 8 yr of solar cycle 23. As could be expected from the examination of the EIT images, the 30.4 nm flux was found to be strongly anisotropic. The anisotropy Ipol/Ieq between the fluxes computed for viewpoints located above the solar poles and within the solar equatorial plane ranges from 0.9 at solar minimum to 0.6 at solar maximum. A 20% difference was also discovered between the north and south polar fluxes. The generalization of this technique to other lines of the EUV and far-ultraviolet (FUV) spectrum is discussed. Title: Solar wind from the coronal hole boundaries Authors: Schwadron, N. A.; McComas, D. J.; Elliott, H. A.; Gloeckler, G.; Geiss, J.; von Steiger, R. Bibcode: 2005JGRA..110.4104S Altcode: 2005JGRA..11004104S Recent studies using in situ observations established that the interface between fast and slow wind in interplanetary space has two distinct parts: a smoothly varying boundary layer flow that flanks fast wind from coronal holes and a sharper plasma discontinuity between intermediate and slow solar wind. Other studies using in situ observations and modeling have demonstrated the existence of the sub-Parker spiral structure of the heliospheric magnetic field in which the magnetic connection between fast and slow wind created by foot point motion at the Sun deforms field lines, making them significantly less transverse than the Parker spiral. Here we model the formation of corotating interaction regions, and by including a coronal hole boundary layer (CHBL) and magnetic foot point motion across the coronal hole boundary back at the Sun we explain the detailed, characteristic variations in composition and magnetic field orientation observed in interplanetary space. Our model accomplishes this using only two free parameters, with all other quantities derived directly from solar wind observations. Through the model we trace the observed interplanetary variations back to an intrinsic two-part structure in the source of solar wind at the Sun. These parts are (1) a CHBL that encircles the coronal hole and has a smooth transition in the source properties that produce the fast through intermediate speed (∼600 km s-1) solar wind and (2) a sharp coronal hole discontinuity separating the distinct sources of solar wind with intermediate speeds and temperatures from slow solar wind. This study establishes the connection between the characteristic variations of the solar wind speed, charge state composition, and magnetic field orientation observed in situ near 5 AU with their sources in the two-part structure of coronal hole boundaries back at the Sun. Title: Bidirectional Proton Flows and Comparison of Freezing-in Temperatures in ICMEs and Magnetic Clouds Authors: Rodriguez, L.; Woch, J.; Krupp, N.; Fränz, M.; von Steiger, R.; Cid, C.; Forsyth, R.; Glaßmeier, K. -H. Bibcode: 2005IAUS..226..420R Altcode: From all the transient events identified in interplanetary space by in-situ measurements, Magnetic Clouds (MCs) are among the most intriguing ones. They are a special kind of Interplanetary Coronal Mass Ejections (ICMEs), characterized by a well-defined magnetic field configuration. We use a list of 40 MCs detected by Ulysses to study bidirectional flows of protons in the ∼0.5 MeV energy range. Solar wind ions are also analysed in order to compare cloud to non-cloud ICMEs.</p>The enhancement in freezing-in temperatures inside the clouds, obtained with data from the SWICS instrument, provides insights into processes occurring early during the ejection of the material and represents a complementary tool to differentiate cloud from non-cloud ICMEs. At higher energies, directional information for protons obtained with the EPAC instrument allows a comparison with previous results concerning bidirectional suprathermal electrons. The findings are qualitatively comparable. Apparently, the portion of bidirectional flows inside magnetic clouds is neither heavily dependent on distance from the Sun nor on parameters obtained from a flux rope model. Title: The Sun, from Core to Corona and Solar Wind Authors: von Steiger, R.; Fröhlich, C. Bibcode: 2005ISSIR...3...99V Altcode: 2005ssb..book...99V; 2005ESASR...3...99V No abstract at ADS Title: Model of the all-sky He II 30.4 nm solar flux Authors: Auchère, F.; Cook, J. W.; Newmark, J. S.; McMullin, D. R.; von Steiger, R.; Witte, M. Bibcode: 2005AdSpR..35..388A Altcode: Because of the orbit characteristics of the vast majority of spacecraft, the solar flux has been generally measured at Earth or in the plane of the ecliptic. So far, most published studies did not consider the fact that the extreme ultraviolet (EUV) solar flux is largely anisotropic. Indeed, in the EUV, the distribution of very contrasted bright and dark features at the surface of the Sun produces both the obvious rotational (longitudinal) modulation of the flux, but also a strong latitudinal anisotropy. Although largely ignored up to now, the latitudinal anisotropy affects the physical conditions in the corona and heliosphere. We describe an empirical model of the all-sky He II 30.4 nm flux based on EIT/ SOHO data. The 30.4 nm flux was found to be strongly anisotropic. The anisotropy Ipol/ Ieq between the fluxes computed for viewpoints located above the solar poles and within the solar equatorial plane ranges from 0.9 at solar minimum to 0.6 at solar maximum. A 20% asymmetry was also discovered between the north and south polar fluxes. Title: A Model For EUV Flux Throughout The 3-Dimensional Heliosphere Authors: McMullin, D. R.; Auchere, F.; Cook, J.; Newmark, J. S.; Quemerais, E.; von Steiger, R.; Witte, M. Bibcode: 2004AGUFMSH21B0423M Altcode: After July 2001, when Ulysses moved from 30 to 80 degrees in solar latitude, the Ulysses GAS instrument measured an apparent increase in the neutral He density. This is more naturally interpreted as a latitudinal dependence (decrease) of the loss rate due to solar photoionization rather than a true increase of the neutral He density. We have developed a three-dimensional model for solar EUV fluxes observed at any heliospheric position, using daily SOHO EIT observations, over successive Carrington rotations, projected to any heliospheric position. The combined effects of solar rotational and latitude-dependent flux variability are explicitly treated in this model. The flux model has been directly compared with other direct irradiance observations in the ecliptic plane with the SOHO/SEM irradiance time series for validation. We then use this flux to compute the photoionization rate of the in-flowing neutral He, and compare the modeled change with time along the spacecraft trajectory with the direct measurements from the out -of -ecliptic Ulysses GAS observations. The 3-D model developed will be directly applicable to STEREO EUV images from the SECCHI instrument suite. As the two spacecraft separate, the amount of the solar surface observed will increase through the mission, providing more accurate solar inputs. Title: Inferences for Isotopic Fractionation Processes in the Solar Wind Using the Full Solar Cycle Record of Abundances from Ulysses: Anticipating Results from the Genesis Mission Authors: Bochsler, P.; von Steiger, R. Bibcode: 2004ESASP.575..372B Altcode: 2004soho...15..372B No abstract at ADS Title: Composition of Interplanetary Coronal Mass Ejections at Very High Latitudes Authors: von Steiger, R.; Zurbuchen, T. H.; Kilchenmann, A. Bibcode: 2004AGUFMSH33B..02V Altcode: Composition signatures such as a high average iron charge state, a high O7+/O6+ ratio, or a high alpha to proton ratio are established tools for the identification of interplanetary coronal mass ejections (ICMEs). However, their relation to the classical signatures such as conterstreaming electrons, low plasma beta, or magnetic field rotation, is far from being one-to-one, and therefore deserves some attention. When Ulysses was traveling to high latitudes it encountered ICMEs both during the first set of polar passes at solar minimum and during the second set, which occurred around the maximum of solar cycle 23. Six high-latitude ICMEs had been observed in the large fast streams from the polar coronal holes at solar minimum, defining a new class of overexpanding ICMEs, but none had a compositional signature whatsoever. In this paper we analyze five ICME events that were also embedded in a polar fast stream, but occurred not far from solar maximum, in October to December 2001 at a heliolatitude of >70o north. These five events show a surprising variety of compositional signatures, from hardly any to strong. They are ideally suited for the study of these signatures since the background fast solar wind is compositionally uniform, making the boundaries appear very sharp. This enables us to compare the two sets of signatures to a high degree of accuracy. Title: Observations of the helium focusing cone with pickup ions Authors: Gloeckler, G.; Möbius, E.; Geiss, J.; Bzowski, M.; Chalov, S.; Fahr, H.; McMullin, D. R.; Noda, H.; Oka, M.; Ruciński, D.; Skoug, R.; Terasawa, T.; von Steiger, R.; Yamazaki, A.; Zurbuchen, T. Bibcode: 2004A&A...426..845G Altcode: The helium gravitational focusing cone has been observed using pickup He+, first during the solar minimum in 1984-1985 with the AMPTE/IRM spacecraft, and again in more detail from 1998 to 2002 with ACE and in 2000 with Nozomi. Five traversals of the cone allow us to obtain an accurate determination of the ecliptic longitude of the interstellar wind flow direction, λ = 74.43 ° ± 0.33 ° , while observations of pickup He++ with Ulysses give us an estimate, relatively free of instrumental systematic uncertainties, of the neutral He density, nHe = 0.0151 ± 0.0015 cm-3, in the Local Interstellar Cloud. From best fits to the measured velocity distributions of pickup He+ using time-stationary models we deduce the radial dependence and magnitude of electron-impact ionization rates that cannot presently be measured, and find this to be an important ionization process in the inner (⪉0.5 AU) heliosphere. We obtain excellent model fits to the 1998 cone profile using measured or deduced rates and known interstellar He parameters, and from this conclude that cross-field diffusion of pickup He+ is small. Furthermore, we find no evidence for extra sources of He in or near the cone region. Best fits to the velocity distributions of He+ are obtained assuming isotropic solar-wind-frame distributions, and we conclude from this that the scattering mean free path for pickup He+ in the turbulent slow solar wind is small, probably less than 0.1 AU. We argue that application of 3D, time-dependent models for computation of the spatial distribution of interstellar neutral helium in the inner heliosphere may lead to excellent fits of short-term averaged pickup He+ data without assuming loss rates that are significantly different from production rates. Title: Heliospheric conditions that affect the interstellar gas inside the heliosphere Authors: McMullin, D. R.; Bzowski, M.; Möbius, E.; Pauluhn, A.; Skoug, R.; Thompson, W. T.; Witte, M.; von Steiger, R.; Rucinski, D.; Judge, D.; Banaszkiewicz, M.; Lallement, R. Bibcode: 2004A&A...426..885M Altcode: The interstellar gas that flows through the heliosphere is strongly affected by ionization close to the Sun, in particular solar photoionization, electron impact, and charge exchange. Therefore, the interpretation of any observation of interstellar gas in the inner heliosphere hinges upon the accurate knowledge of these effects and their variations. In addition, the irradiance and line profile of the relevant solar spectral line are needed to properly interpret resonant backscattering observations of the interstellar neutral gas. With instrumentation on ACE, SOHO and Wind, continuous monitoring of these important environmental conditions simultaneously with a multitude of interstellar gas observations has become possible for the first time. In this paper we present a compilation of the processes and parameters that affect the distribution of interstellar helium inside the heliosphere and their observation, including the irradiance and line profile of the He 58.4 nm line. We also make the connection to proxies for these parameters and evaluate their accuracy in order to expand the time period of coverage wherever possible. Title: Synopsis of the interstellar He parameters from combined neutral gas, pickup ion and UV scattering observations and related consequences Authors: Möbius, E.; Bzowski, M.; Chalov, S.; Fahr, H. -J.; Gloeckler, G.; Izmodenov, V.; Kallenbach, R.; Lallement, R.; McMullin, D.; Noda, H.; Oka, M.; Pauluhn, A.; Raymond, J.; Ruciński, D.; Skoug, R.; Terasawa, T.; Thompson, W.; Vallerga, J.; von Steiger, R.; Witte, M. Bibcode: 2004A&A...426..897M Altcode: A coordinated effort to combine all three methods that are used to determine the physical parameters of interstellar gas in the heliosphere has been undertaken. In order to arrive at a consistent parameter set that agrees with the observations of neutral gas, pickup ions and UV backscattering we have combined data sets from coordinated observation campaigns over three years from 1998 through 2000. The key observations include pickup ions with ACE and Ulysses SWICS, neutral atoms with Ulysses GAS, as well as UV backscattering at the He focusing cone close to the Sun with SOHO UVCS and at 1 AU with EUVE. For the first time also the solar EUV irradiance that is responsible for photo ionization was monitored with SOHO CELIAS SEM, and the He I 58.4 nm line that illuminates He was observed simultaneously with SOHO SUMER. The solar wind conditions were monitored with SOHO, ACE, and WIND. Based on these data the modeling of the interstellar gas and its secondary products in the heliosphere has resulted in a consistent set of interstellar He parameters with much reduced uncertainties, which satisfy all observations, even extended to earlier data sets. It was also established that a substantial ionization in addition to photo ionization, most likely electron impact, is required, with increasing relative importance closer to the Sun. Furthermore, the total combined ionization rate varies significantly with solar latitude, requiring a fully three dimensional and time dependent treatment of the problem. Title: Heliospheric Magnetic Field Configuration at Solar Maximum Conditions: Consequences for Galactic Cosmic Rays Authors: Zurbuchen, T. H.; von Steiger, R.; Manchester, W. B.; Fisk, L. A. Bibcode: 2004AIPC..719...70Z Altcode: During solar maximum conditions, the heliosphere is highly structured on all spatial scales. It is the purpose of this paper to summarize our current understanding of these structures from global scales to mesoscale, a fraction of 1 AU. We use theoretical considerations, in situ observations near Earth and the Ulysses spacecraft, and global heliosphere calculations to discuss the effects on both global and mesoscales on the three-dimensional structure of the heliospheric magnetic field and their effects on galactic cosmic rays. These conclusions are in contrast to near-solar-minimum-like heliospheric conditions that are currently assumed in modulation and transport calculations even during solar maximum. The expected complex heliospheric properties should be of major importance for the interpretation of the heliospheric boundary events observed by Voyager 1 since 2002. A companion paper by L. A. Fisk will explore the effects of the mesoscale structures on particle acceleration in the heliospheric boundary region. Title: Cometary Ions Trapped in a Coronal Mass Ejection Authors: Gloeckler, G.; Allegrini, F.; Elliott, H. A.; McComas, D. J.; Schwadron, N. A.; Geiss, J.; von Steiger, R.; Jones, G. H. Bibcode: 2004ApJ...604L.121G Altcode: Ion tails of comets are known to extend radially away from the Sun over very large distances. Crossing these tails by spacecraft not specifically targeted to intercept them was believed to be extremely improbable, since that requires precise angular alignment of the spacecraft with a comet. We report here the fortuitous detection of cometary ions at large angular separation far from the comet. To explain this unexpected discovery, we conclude that these ions were ducted laterally along magnetic fields that were randomly distorted by a coronal mass ejection and that such transport increases the probability of an unplanned detection of comets. Title: A statistical study of oxygen freezing-in temperature and energetic particles inside magnetic clouds observed by Ulysses Authors: Rodriguez, L.; Woch, J.; Krupp, N.; FräNz, M.; von Steiger, R.; Forsyth, R. J.; Reisenfeld, D. B.; GlaßMeier, K. -H. Bibcode: 2004JGRA..109.1108R Altcode: Interplanetary Coronal Mass Ejections (ICMEs) have proven to be very complex phenomena, not easy to unveil using a single set of observations. We combine Ulysses observations of medium energy particles, solar wind plasma parameters, magnetic field, and charge state distributions of heavy ions in order to identify and characterize CME ejecta in the heliosphere. We focused on a special class of ICMEs, so-called magnetic clouds (MC). The large number of MCs detected by Ulysses allowed us to perform a statistical analysis of the freezing-in temperature and energetic particle population within MCs. Based on a larger statistical set of events covering a full solar cycle and all heliolatitudes, we can confirm previous findings of a significant temperature increase within MCs. Furthermore, we found that this increase occurs at all latitudes and phases of the solar cycle. Intensities of medium-energy particles are generally depleted or not changed inside the MCs. This behavior is, again, found at all latitudes and solar cycle phases. Title: Preface to: COSPAR 2002 D2.2-E3.3 Authors: Esser, R.; von Steiger, R. Bibcode: 2004AdSpR..33..667E Altcode: No abstract at ADS Title: Charge States and Abundances of Heavy Ions as Signatures of Interplanetary Coronal Mass Ejections Authors: von Steiger, R.; Kilchenmann, A.; Zurbuchen, T. H. Bibcode: 2004cosp...35.1574V Altcode: 2004cosp.meet.1574V Compositional signatures are by now a well-established tool for the identification of Interplanetary Coronal Mass Ejections. An alpha-to-proton ratio of >8 % is a sufficient criterion for the presence of an ICME, as is an average charge state of iron ions of < Q_Fe > ≥ 12; both of these signatures are not necessary ones, though. An increased C and O freezing-in temperature is also likely to be a robust ICME signature. Compositional signatures are particulary attractive because, unlike kinetic and magnetic ones, they remain essentially unchanged throughout the entire heliosphere. Using data obtained with Ulysses-SWICS we evaluate the occurrence rate of composition signatures in ICMEs as identified both by their classical (kinetic and magnetic) as well as by their compositional signatures. We then attempt to identify and define different classes of ICMEs based on the presence of particular, characteristic combinations of such signatures. Finally, the distribution of ICMEs with and without a compositional signature as a function of heliographic latitude will be evaluated. Title: Internal Structure of Magnetic Clouds seen by Ulysses Authors: Rodriguez-Romboli, L.; Woch, J.; Krupp, N.; Fränz, M.; von Steiger, R.; Cid, C.; Forsyth, R.; Glaßmeier, K. -H. Bibcode: 2004cosp...35.2285R Altcode: 2004cosp.meet.2285R Magnetic clouds represent nearly one third of all the coronal mass ejections seen by Ulysses. Among the many open questions regarding their origin and evolution, one of the most challenging scientific problems is to gain insights into their internal structure. On a first approximation, the question is whether the intrinsic structure of CMEs seen at the Sun still prevails in interplanetary space. We use data from the SWICS and EPAC instruments onboard Ulysses to analyse intensities, composition, anisotropies and spectra of ions from the plasma to the 1MeV/nuc energy range. These data are used in conjunction with a flux rope model for the magnetic field, to order the obtained results in a topological frame of reference. Title: The ICME Superevent 2003: A view from Ulysses Authors: Kilchenmann, A.; von Steiger, R.; Zurbuchen, T. H. Bibcode: 2004cosp...35.1332K Altcode: 2004cosp.meet.1332K In October-November 2003 a series of exceptionally large events took place on the Sun. They led to a series of CMEs, which propagated through interplanetary space and reached Ulysses, where they created a very unusually strong ICME event. We will present the observations from Ulysses, which was located at 5 AU close to the west limb of the Sun. The speed resulting from this event, vα∼ 999.2 km/s, was the highest 3-hour average ever observed at Ulysses during its entire mission since late 1990. During almost a week, events were arriving at Ulysses, which all had the same source region at the Sun. We describe the superevent from Ulysses-SWICS data with consideration of compositional signatures, such as Fe charge state, O7+/O6+ ratio and the α/p ratio. Then we map the in situ observations back to the Sun and identify them with events observed from SOHO. We will discuss the detailed association of SOHO CMEs and Ulysses in situ observations. Title: The October/November 2003 Events: ACE and Ulysses Results Authors: Zurbuchen, T. H.; von Steiger, R. Bibcode: 2004cosp...35.1658Z Altcode: 2004cosp.meet.1658Z The solar activity during a period of approximately 10 days starting in late October 2003 is being discussed based on ACE and Ulysses data. The solar events of interest were associated with a very large cluster of highly complex active regions. These resulted in coronal mass ejections that led to a number of the most spectacular events ever observed in situ. It is the purpose of this talk to, first, summarize observations from ACE. We will focus on measurements of solar wind dynamics, speeds in excess of 1900 km/s, and plasma heating to levels not previously observed. We will then discuss the compositional signatures of these events. The ionic charge states of Fe were observed to reach record levels, O and C were almost fully ionized, and there were unusual elemental fractionation patterns observed during the most extreme event. Finally, we will address the heliospheric consequences of these events, by comparing ACE and Ulysses data. This time of very unusual solar activity also led to record-breaking events in the outer heliosphere, far off the Sun-Earth line. We will discuss the global consequences of these events. Title: Charge states and abundances of heavy ions as signatures of interplanetary coronal mass ejections Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2003AGUFMSH11A..04V Altcode: Interplanetary Coronal Mass Ejections (ICMEs) are not easy to recognise. Several signatures are used to identify such events: Counterstreaming electrons, magnetic field rotation and fluctuation, low kinetic temperature, etc. However, an individual ICME rarely shows them all, so identification remains a somewhat subjective art form. Composition signatures were long known to provide a useful identifier: An alpha-to-proton ratio of >8% is a sufficient criterion for the presence of an ICME. More recently, a high average Fe charge state was established as another sufficient (but not necessary) signature, as is probably the case for an increased C and O freezing-in temperature. Such signatures are particulary attractive because, unlike kinetic and magnetic ones, they remain largely unchanged throughout the entire heliosphere. Using data obtained with Ulysses-SWICS we evaluate the occurrence rate of composition signatures in ICMEs as identified by their classical signatures. The definition of the appropriate threshold values of these signatures will receive particular attention. Finally, the distribution of ICMEs with and without a compositional signature as a function of heliographic latitude will be evaluated. Title: Solar wind composition measurements during one entire solar cycle Authors: Zurbuchen, T. H.; von Steiger, R. Bibcode: 2003AGUFMSH11A..03Z Altcode: The Solar Wind Ion Composition Sensors on Ulysses and ACE have provided the most comprehensive set of solar wind elemental composition data to date. Solar wind elemental compositional variations have been observed by these instruments since 1990 and 1997 respectively. All solar wind is observed to be fractionated throughout the entire solar cycle. However, the degree of fractionation varies as a function and time and location throughout the solar cycle. We will review these observations and discuss a theoretical model used to explain these fractionation patterns. We will also discuss the implications of these models on long-term averaged isotopic composition measurements, such as to be provided by Genesis. Title: Earth Gravity Field from Space - from Sensors to Earth Sciences Authors: Beutler, G.; Drinkwater, M. R.; Rummel, R.; von Steiger, R. Bibcode: 2003egfs.conf.....B Altcode: The ESA explorer core mission GOCE, to be launched in 2006, will enhance our knowledge of the global static gravity field and of the geoid by orders of magnitude. The U.S. satellite gravity mission GRACE (2002-2006) is currently measuring, in addition, the temporal variations of the gravity field. With these new data a whole range of fascinating new possibilities will be opened for solid Earth physics, oceanography, geodesy and sea-level research. The new generation of gravity missions employs sensor concepts for gravity field measurement, orbit and attitude control and orbit determination that show interesting similarities with space experiments planned in the field of fundamental physics. This volume is the result of a workshop that brought together some 50 acknowledged experts in their field to discuss (1) strategies for ultra precision orbit determination and gravity field modelling with the data of the upcoming gravity field missions, (2) the use of accurate and high resolution gravity models in Earth sciences whereby, in particular, synergy is expected between the various science fields in their use of this type of new information, and (3) gravity field requirements and possible sensor and mission concepts for the time after GRACE and GOCE.

Link: http://www.wkap.nl/prod/b/1-4020-1408-2 Title: Composition signatures of interplanetary coronal mass ejections Authors: von Steiger, Rudolf; Zurbuchen, Thomas H. Bibcode: 2003ESASP.535..835V Altcode: 2003iscs.symp..835V The interplanetary counterparts of coronal mass ejections (ICMEs) are complex phenomena that are not recognised or characterised easily. Many signatures have been defined and used to identify them: kinetic, magnetic, thermal, energetic particles, etc., but hardly any ICME event shows a signal in all of them simultaneously. Another classical ICME identifier is the abundance of alpha particles. It was shown that an alpha-to-proton ratio of >8% is a sufficient criterion for ICME detection, albeit not a necessary one. In recent years more composition signatures for ICMEs were defined using the time-of-flight instruments on Ulysses and ACE, and it could be shown that a high average iron charge state is also a sufficient but no necessary ICME signature. The same is probably true for an increased oxygen or carbon freezing in temperature above a certain threshold value. Composition signatures are particularly attractive since they are unlikely to change once the SME has left the Sun, making them a robust tool for ICME identification throughout the entire heliosphere. Using the data obtained with Ulysses SWICS we assess which of the composition signatures are observed in ICMEs defined by the classical signatures. Conversely, we search for occurrences of composition signatures and assess whether or not an ICME is associated with it. As a result we obtain a quality measure for each composition signature. Title: Temperature Anisotropies of Heavy Solar Wind Ions from Ulysses-SWICS Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2003AIPC..679..526V Altcode: We report the first in-situ measurements of temperature anisotropies of heavy ions in the solar wind, obtained with the Solar Wind Ion Composition Spectrometer (SWICS) on the Ulysses spacecraft. Since SWICS measures only 1-dimensional cuts through the full, 3-d velocity distribution functions we resort to a statistical approach, separating the particle data according to the instantaneous magnetic field angle. We apply this analysis to the ions of He++ and O6+ during extended time periods in the fast streams from both the south and the north polar coronal holes that Ulysses traversed in 1993-96. In both cases we find anisotropies of the order of T⊥/T∥ = 0.8. The results of this study are discussed in relation to the observations made on Helios for He++ in the 1970s, and to recent observations made on SOHO-UVCS, which show extreme temperature anisotropies of O VI, or O5+, at a few solar radii. Title: The Composition of Interplanetary Coronal Mass Ejections Authors: Zurbuchen, Thomas H.; Fisk, L. A.; Lepri, S. T.; von Steiger, R. Bibcode: 2003AIPC..679..604Z Altcode: Interplanetary coronal mass ejection (ICME) associated plasma can exhibit signatures in elemental, ionic and isotopic composition. These signatures occur in less than 50% of all ICMEs, but are very indicative of ICME plasma. We review these compositional anomalies and briefly discuss a physical scenario that could be responsible for these anomalies. Title: Foreword Authors: Beutler, G.; Drinkwater, M. R.; Rummel, R.; von Steiger, R. Bibcode: 2003SSRv..108D...9B Altcode: No abstract at ADS Title: Interplanetary and solar surface properties of coronal holes observed during solar maximum Authors: Zhang, J.; Woch, J.; Solanki, S. K.; von Steiger, R.; Forsyth, R. Bibcode: 2003JGRA..108.1144Z Altcode: Data from the Solar Wind Ion Composition Spectrometer (SWICS) on board the Ulysses spacecraft and synoptic maps from Kitt Peak are used to analyze the relatively short-lived coronal holes which exist during the maximum phase of the solar activity cycle 23. They are compared with the persistent polar coronal holes which prevail around solar minimum. A solar wind velocity increase coinciding with a shift of the ionic charge composition toward lower charge states serves as a robust criterion for identifying solar wind streams emanating from solar maximum holes. This allows an unambiguous association of every stream identified in interplanetary space with a coronal hole on the solar surface with consistent magnetic polarity. Solar wind streams emanating from the solar maximum holes generally show lower velocities of 400 to 600 km/s compared to the polar hole stream velocities of 700 to 800 km/s. However, the SWICS O7+/O6+ charge-state ratios, which are a proxy for coronal temperatures, do not reveal a consistent difference. Though a number of solar maximum holes have a significantly, up to three times, higher temperature compared to the polar coronal holes, the majority of the investigated holes and specifically those with new cycle polarity have a coronal temperature within the range of polar hole temperatures. Likewise, the magnetic flux density in the solar maximum holes and in the polar coronal holes, as derived from the synoptic maps, is not strikingly different. Therefore any intrinsic difference between solar maximum holes and polar coronal holes is small. The striking discrepancy in their kinetic properties, namely the slower velocity of the solar wind streams emanating from solar maximum holes, may partly be attributed to deceleration of the solar wind during propagation to the spacecraft. The discrepancy may also be influenced by active regions in close proximity to the coronal holes, which presumably is more likely for smaller holes. There may, however, be a tendency for the faster wind streams to emanate from cooler holes. Title: Latitude Dependence of Element Abundances in the Slow Solar Wind Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2002AGUFMSH21A0515V Altcode: Since 1992 the Ulysses spacecraft orbits the Sun on a high-inclination orbit with an inclination of 80 degrees to the heliographic equator. The first orbit, in 1992--98, took place around solar minimum and revealed a highly ordered state of the heliosphere with large high-speed streams poleward of about 30 degrees heliolatitude, emanating from the relatively cool polar coronal holes, separated by a band of slow solar wind at low latitudes. In the slow wind the abundances of elements with a low first ionisation potential (FIP) such as Fe, Mg, and Si, are found to be enhanced over the solar values relative to the high-FIP elements by a significant factor of 2--5. On the other hand, this FIP enrichment factor was found to be less than a factor of two, but still significantly larger than one, in the polar high speed streams. On the second orbit, which is now taking place around the maximum of solar cycle 23, slow solar wind is found at all heliolatitudes, interspersed with fast streams from fragmented coronal holes and from coronal mass ejections, also at all latitudes. Using data from the SWICS sensor on Ulysses, we have found that the strength of the FIP fractionation factor appears to depend on the heliographic latitude, even if we restrict ourselves to unequivocal slow solar wind. The strongest FIP enrichments are found at low latitudes, which can also be observed from the ecliptic plane, but they are becoming increasingly weaker at higher latitudes. This was particularly evident during the second fast latitude scan in 2000/01. We will present the observational data and discuss their possible implications for the underlying coronal structure, specifically in the framework of the Fisk model. In this model the slow solar wind is pictured as made up from a sequence of prevoiusly closed magnetic loops that are emptied onto open, migrating field lines. The strength of the FIP fractionation of the loop material may expected to be a function of loop parameters such as length, temperature, or age, so therefore a systematic variation of the FIP fractonation factor may reveal a dependence of these parameters on heliographic latitude. Title: Matter in the Universe Authors: Jetzer, Ph.; Pretzl, K.; von Steiger, R. Bibcode: 2002maun.conf.....J Altcode: The knowledge of the amount and nature of matter present in the Universe is undoubtedly 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 recent 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, the present volume presents a very useful synopsis on all constituents of matter in the Universe. Link: http://www.wkap.nl/prod/b/1-4020-0666-7 Title: Kinetic properties of heavy solar wind ions from Ulysses-SWICS Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2002AdSpR..30...73V Altcode: The kinetic properties of heavy ions in the solar wind reflect the microphysical processes governing the solar wind in the heliosphere. We use the unique data set of Ulysses-SWICS which provides data in a wide rage of mass per charge, 2 ≤ m/q ≤ 9.33. In particular, we look for slight deviations from the canonical behaviour of equal bulk speed and equal thermal speed of all heavy ion species. Such deviations are expected to carry signatures of the wave-particle interaction processes in the solar wind, and to a lesser extent, to collisions which tend to bring the particles closer to thermal equilibrium. The data set of Ulysses-SWICS is ideal for this task because it spans not only a large range in m/q, but also in time, solar wind speed (covering extended time periods in slow and in fast wind), heliographic latitude, and heliocentric distance. Title: The radiometric calibration and intercalibration of SOHO Authors: Huber, M. C. E.; Pauluhn, A.; von Steiger, R. Bibcode: 2002ESASP.508..213H Altcode: 2002soho...11..213H The radiometric calibration of spectrometric telescopes assures that the observed spectral radiance (or irradiance) is measured on a scale that is defined by the radiometric standards realised and used in terrestrial laboratories. All SOHO instruments therefore have been calibrated by use of source and detector standards that are traceable to the primary radiometric standards. As any calibration, the laboratory calibration has uncertainties. Moreover, environmental influences, namely molecular and particulate contamination on the ground and effects by photon and particle radiaton in space, do change the responsivity of the instruments. In two workshops held at the International Space Science Institute in Bern the individual instrument calibrations were discussed and reconciled. The outcome of the workshops, to which all instrument groups contributed, is summarised in a book that is presented here before it goes to press. Title: Adaptive Systems for Detection and Forecasting of Coronal Mass Ejections From Solar Mean Magnetic Field Authors: Ganguli, S. B.; Gavrichtchaka, V. V.; Von Steiger, R. Bibcode: 2002AGUSMSH52A..01G Altcode: Coronal mass ejections (CME) are important sources of dynamical phenomena that collectively influence geo-space weather. For example, large, nonrecurrent geomagnetic storms are caused by interplanetary disturbances driven by fast CMEs. Therefore efficient techniques for detection and forecasting of CME events can significantly increase the performance of any realistic space weather forecasting system. Recently it has been shown that wavelet analysis of the high-resolution solar mean magnetic field (SMMF) data can provide valuable information for CME detection. However not all CME events produce easy detectable signatures in the wavelet transformed SMMF time series. Moreover CME forecasting would require extracting information from the data prior to CME onset where these signatures are even less obvious. Therefore to achieve acceptable accuracy in CME detection/forecasting, multiple features from the wavelet spectrum or raw SMMF data should be processed with a powerful classifier based on statistical or machine learning techniques. We applied neural network and support vector machine for this purpose. Performance of the obtained systems will be discussed. Title: Solar wind from high-latitude coronal holes at solar maximum Authors: McComas, D. J.; Elliott, H. A.; von Steiger, R. Bibcode: 2002GeoRL..29.1314M Altcode: 2002GeoRL..29i..28M In this study we combine Ulysses' observations from the solar wind plasma (SWOOPS) and ion composition (SWICS) instruments to study high-latitude coronal holes near solar maximum for the first time. While chromospheric and coronal composition signatures indicate that there is a unique type of solar wind, which flows from coronal holes, variations in the acceleration process produce a wide range of solar wind speeds from these holes. High-speed wind (>700 km s-1) can be produced in small as well as large holes, although the very highest speed non-transient winds do come from the centers of the largest holes. Along the edges of coronal holes, the acceleration decreases and freezing-in temperatures increase relatively smoothly into the surrounding solar wind, indicating a transition layer around the edges of coronal holes. Title: The solar wind composition throughout the solar cycle: A continuum of dynamic states Authors: Zurbuchen, T. H.; Fisk, L. A.; Gloeckler, G.; von Steiger, R. Bibcode: 2002GeoRL..29.1352Z Altcode: 2002GeoRL..29i..66Z Variations in the speed and elemental and ionic charge composition of the solar wind are reported throughout the solar cycle, as observed by the SWICS instrument on Ulysses. The apparent bimodal nature of the solar wind during the solar minimum does not persist throughout the solar cycle. Rather, with increasing solar activity, a continuum of solar wind speeds and charge states is observed. The exception is the elemental composition which is noticeably less enhanced in elements with low first ionization potential (FIP) in material from coronal holes throughout the solar cycle. These observations are consistent with theories in which the solar wind originates from coronal loops that reconnect with open magnetic field lines. Title: The Sun at solar minimum: North - south asymmetry of the polar coronal holes Authors: Zhang, J.; Woch, J.; Solanki, S. K.; von Steiger, R. Bibcode: 2002GeoRL..29.1236Z Altcode: 2002GeoRL..29h..77Z Data from the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses and synoptic charts derived from Kitt Peak magnetograms are used to compare the south and north polar coronal holes which existed during the declining/minimum phase of the solar activity cycle from 1992 to 1997. The kinetic properties of the solar wind emanating from the two polar coronal holes, as represented by solar wind speed, do not differ significantly. However, the electron temperature in the two coronal holes inferred from ionic charge composition data, namely the O7+/O6+ ratio, show consistent differences, with the south polar hole being 10 to 15% hotter. The ground-based magnetograms show that the north polar coronal hole covers a larger part of the solar surface than the southern one. The total magnetic flux and, specifically, the flux density of the north polar coronal hole is considerably lower for the whole interval of time between 1992 and 1997. This strongly indicates that the difference in coronal hole temperature between the southern and northern coronal hole is intrinsic and is not due to the fact that the Ulysses observations in the south and north coronal hole streams were made at different phases of the solar cycle. Thus the differences found represent a real north-south asymmetry during this time period. Title: The Astrophysics of Galactic Cosmic Rays Authors: Diehl, Roland; Parizot, Etienne; Kallenbach, Reinald; von Steiger, Rudolf Bibcode: 2002agcr.conf.....D Altcode: This volume together with the ones 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 CRs. 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. Other themes are the extent to which galactic-scale processes can be illuminated by studies or analogous heliospheric processes, and the identification of key questions for future investigations. The workshop assembled physicists working in the fields of cosmic rays origin and propagation, structure evolution and composition of the Galaxy and the interstellar medium. In addition, researchers working in relevant areas of radio, optical, X-ray and gamma-ray astronomy, attended the workshops. This has strengthened the interdisciplinary links between these scientific communities. Link: http://www.wkap.nl/prod/b/1-4020-0107-X Title: Foreword Authors: Pauluhn, A.; Huber, M. C. E.; von Steiger, R. Bibcode: 2002ISSIR...2D...7P Altcode: 2002ESASR...2D...7P; 2002rcs..confD...7P No abstract at ADS Title: The solar wind Authors: Neugebauer, M.; von Steiger, R. Bibcode: 2002css1.book.1115N Altcode: No abstract at ADS Title: The Radiometric Calibration of SOHO Authors: Pauluhn, A.; Huber, M. C. E.; von Steiger, R. Bibcode: 2002ISSIR...2.....P Altcode: 2002ESASR...2.....P; 2002rcs..conf.....P No abstract at ADS Title: Foreword Authors: Pauluhn, A.; Huber, M. C. E.; von Steiger, R. Bibcode: 2002ISSIR...2D...5P Altcode: 2002ESASR...2D...5P; 2002rcs..confD...5P No abstract at ADS Title: The Sun At Solar Minimum: North - South Asymmetry of The Polar Coronal Holes Authors: Woch, J.; Zhang, J.; Solanki, S. K.; von Steiger, R. Bibcode: 2002EGSGA..27.4007W Altcode: Data from the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses and synoptic charts derived from Kitt Peak magnetograms are used to compare the south and north polar coronal holes which existed during the declining/minimum phase of the solar activity cycle from 1992 to 1997. The kinetic properties of the solar wind emanating from the two polar coronal holes, as represented by solar wind speed, do not differ significantly. However, the electron temperature in the two coronal holes inferred from ionic charge composition data, namely the O7+/O6+ ratio, show consis- tent differences, with the south polar hole being 10 to 15% hotter. The ground-based magnetograms show that the north polar coronal hole covers a larger part of the so- lar surface than the southern one. The total magnetic flux and, specifically, the flux density of the north polar coronal hole is considerably lower for the whole interval of time between 1992 and 1997. This strongly indicates that the difference in coronal hole temperature between the southern and northern coronal hole is intrinsic and is not due to the fact that the Ulysses observations in the south and north coronal hole streams were made at different phases of the solar cycle Thus the differences found represents a real north-south asymmetry. Title: Interplanetary and solar surface properties of coronal holes Authors: Woch, J.; Zhang, J.; Solanki, S.; von Steiger, R. Bibcode: 2002cosp...34E.967W Altcode: 2002cosp.meetE.967W Data from the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses and synoptic maps from Kitt Peak are used to analyse coronal holes throughout the solar activity cycle. The large polar coronal holes existing during the declining/minimum phase of solar cycle 22 show a persistent north-south asymmetry. The coronal temperature, inferred from ionic charge-state distributions, and the magnetic flux density are significantly lower in the north polar coronal hole. The temperature of the emerging north polar hole of solar cycle 23 is remarkably similar to that of solar cycle 22, confirming that the coronal temperatures of the polar coronal holes do not evolve in the course of the activity cycle. Solar wind streams emanating from the small-scale coronal holes observed around solar maximum generally show lower velocities compared to the polar coronal hole streams. However, the coronal temperatures do not reveal a consistent difference. Though a large number of solar maximum holes have a significantly higher temperature compared to the polar coronal holes the majority has a coronal temperature within the range of polar hole temperatures. Above all, the latter holds for solar maximum coronal holes having a magnetic polarity consistent with the polarity of the new solar cycle. Likewise, the magnetic flux density in the solar maximum holes and in the polar coronal holes, as derived from the synoptic maps, is not strikingly different. Therefore, it can be concluded that there is no indication for an intrinsic difference of solar maximum and polar coronal holes. Title: Latitude dependence of element abundances in the slow solar wind Authors: von Steiger, R.; Zurbuchen, T.; Schwadron, N.; Gloeckler, G.; Geiss, J.; Fisk, L. Bibcode: 2002cosp...34E1205V Altcode: 2002cosp.meetE1205V Since 1992 the Ulysses spacecraft orbits the Sun on a high-inclination orbit with an inclination of 80 degrees to the heliographic equator. The first orbit, in 1992-1998, took place around solar minimum and revealed a highly ordered state of the heliosphere with large high-speed streams poleward of30 heliolatitude, emanating from the relatively cool polar coronal holes, separated by a band of slow solar wind at low latitudes. In the slow wind the abundances of elements with a low first ionisation potential (FIP) such as Fe, Mg, and Si, are found to be enhanced over the solar values relative to the high-FIP elements by a significant factor of 2-5. On the other hand, this FIP enrichment factor was found to be less than a factor of two, but still significantly >1, in the polar high speed streams. On the second orbit, which is now taking place around the maximum of solar cycle 23, slow solar wind is found at all heliolatitudes, interspersed with fast streams from fragmented coronal holes and from coronal mass ejections, also at all latitudes. Using data from the SWICS sensor on Ulysses, we have found that the strength of the FIP fractionation factor appears to depend on the heliographic latitude, even if we restrict ourselves to unequivocal slow solar wind. The strongest FIP enrichments are found at low latitudes, which can also be observed from the ecliptic plane, but they are becoming increasingly weaker at higher latitudes. This was particularly evident during the second fast latitude scan in 2000/01. We will present the observational data and discuss their possible implications for the underlying coronal structure, specifically in the framework of the Fisk model. In this model the slow solar wind is pictured as made up from a sequence of prevoiusly closed magnetic loops that are emptied onto open, migrating field lines. The strength of the FIP fractionation of the loop material may expected to be a function of loop parameters such as length, temperature, or age, so therefore a systematic variation of the FIP fractonation factor may reveal a dependence of these parameters on heliographic latitude. Title: Solar wind at solar maximum Authors: von Steiger, R. Bibcode: 2002cosp...34E1201V Altcode: 2002cosp.meetE1201V During the last solar minimum in 1996 Ulysses, on its first polar orbit, found a heliosphere that was relatively simply structured. Large fast streams emanating from the polar coronal holes dominated the heliosphere poleward of30 , separated by a zone of generally slow and very variable solar wind within20 from the solar equator. Composition data were essential in defining these two quasi-stationary stream types and in particular the boundary between them, which appears to be remarkably sharp and well-defined from down in the chromosphere out to Ulysses at 5 AU. Now, around the time of solar maximum activity of cycle 23, Ulysses is on its second polar orbit, and the picture of the heliosphere that we obtain this time around is radically different. Superficially it looks as if the fast streams had almost completely vanished and the slow, variable solar wind subtended the full solid angle. Yet composition data of both Ulysses- and ACE-SWICS reveal that the fast streams are, and have been, present all along. As the solar magnetic field reverses around maximum activity, the large polar coronal holes fragment and are replaced by a number of smaller coronal holes at low latitudes (possibly of about equal integrated area). The fast streams emanating from these equatorial coronal holes are affected by stream-stream interaction due to the solar rotation and their kinetic signature may be altered thereby. But compositional signatures such as a low O7+ /O6+ charge state ratio are unaffected by such interactions and clearly indicate their coronal hole origin. Moreover, the solar wind around solar maximum is interspersed with interplanetary coronal mass ejections of any speed, and again compositional signatures such as a high average Fe charge state can be used to identify many of these. Title: Coronal Holes During Solar Maximum: Swics/ulysses and Kitt Peak Observations Authors: Zhang, J.; Woch, J.; Solanki, S. K.; von Steiger, R. Bibcode: 2002EGSGA..27.4034Z Altcode: Synoptic maps of the solar coronal magnetic field from Kitt Peak show the existence of small-scale coronal holes at low and mid latitudes during the maximum phase of the present solar cycle. The solar wind originating from the most prominent holes can be unambiguously identified in interplanetary space at distances of 2 to 4 AU with the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses. The coronal hole plasma is characterized by an enhanced velocity and a decreased O7+/O6+ ratio com- pared to the ambient solar wind. The decreased ratio is indicative for a lower coronal temperature in the source region on the Sun. Though clearly distinguishable from the ambient solar wind plasma, the solar wind originating from small scale coronal holes has a lower velocity and less reduced O7+/O6+ ratio than the solar wind emanating from the large-scale polar coronal holes during solar minimum. This difference is re- flected in synoptic coronal hole maps and magnetograms. The magnetic flux density of the small scale coronal holes is considerably lower compared to the flux density of the polar coronal holes. We suggest that the two types of coronal holes are intrinsically different. Title: Temperatures and Temperature Anisotropies of Heavy Solar Wind Ions From Ulysses-SWICS Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2001AGUFMSH21A0732V Altcode: The kinetic properties of heavy ions in the solar wind are indicative of processes affecting their distribution functions in interplanetary space. Observations at 1 AU reported earlier have established that all heavy ion species flow approximately at the same bulk speed and have approximately equal thermal speeds (i.e., mass-proportional temperatures), with exceptions at times when the solar wind density was unusually high. At 5 AU such exceptions no longer occur and the basic picture (of equal bulk speeds and thermal speeds) applies with very high accuracy. This was interpreted as evidence for the growing dominance of wave-particle interactions over Coulomb collisions with increasing heliocentric distance. Moreover, ubiquitous supra-thermal tails on the distribution functions of heavy ions (without any association to shocks) were interpreted as evidence for wave-particle interactions referentially heating and accelerating heavy ions from thermal energies to energies where they become amenable to shock acceleration, at about 2--3 v SW. In this work we examine yet another property of heavy ion distribution functions: their thermal anisotropy. This is not a straightforward matter since with SWICS only 1-dimensional cuts through the full, 3-d velocity distribution functions are measured. We therefore have to resort to a statistical approach, separating the particle data according to the instantaneous magnetic field pitch angle (and restricting ourselves to periods when this angle remains sufficiently constant over an instrument cycle of 13 minutes). We apply this analysis to the ions of He++ and O6+ during extended time periods in both the fast streams from the south and the north polar coronal holes observed by Ulysses in 1993--96. The results of this study are interpreted in relation to the observations made on Helios for He2+ in the 1970s, and to recent observations made on SOHO-UVCS, which show extreme temperature anisotropies of O vi, or O5+, at a few solar radii. Title: Measuring Solar Abundances Authors: von Steiger, R.; Vial, J. -C.; Bochsler, P.; Chaussidon, M.; Cohen, C. M. S.; Fleck, B.; Heber, V. S.; Holweger, H.; Issautier, K.; Lazarus, A. J.; Ogilvie, K. W.; Paquette, J. A.; Reisenfeld, D. B.; Teriaca, L.; Wilhelm, K.; Yusainee, S.; Laming, J. M.; Wiens, R. C. Bibcode: 2001AIPC..598...13V Altcode: 2001sgc..conf...13V This is the rapporteur paper of Working Group 2 on Measuring Solar Abundances. The working group presented and discussed the different observations and methods for obtaining the elemental and isotopic composition of the Sun, and critically reviewed their results and the accuracies thereof. Furthermore, a few important yet unanswered questions were identified, and the potential of future missions to provide answers was assessed. . Title: The Astrophysics of Galactic Cosmic Rays Authors: Diehl, R.; Kallenbach, R.; Parizot, E.; Von Steiger, R. Bibcode: 2001SSRv...99....3D Altcode: Observations of cosmic rays and their related radio to gamma-ray signatures are surveyed and discussed critically, and compared to theoretical models of the cosmic-ray origin and propagation. The analogous heliospheric processes are included as a well-studied case of the principal physical processes of energetic particle acceleration and propagation. Reinforcements, or conflicts, in the interpretations of cosmic-ray spectral and compositional characteristics arise when cosmic-ray source and propagation models are confronted with astronomical information about the Galaxy as a whole and from potential source sites, i.e., supernova remnants or regions with high massive-star density. This volume represents the outcome of two workshops held at ISSI. In this chapter we summarize the introductory papers presented below, and include insights from the workshop discussions. Title: An ICME observed by Voyager 2 at 58 AU and by Ulysses at 5 AU Authors: Paularena, K. I.; Wang, C.; von Steiger, R.; Heber, B. Bibcode: 2001GeoRL..28.2755P Altcode: Between days 175 and 180 (June 24 through 29) of 1999, the PLS instrument on Voyager 2 observed alpha particle enhancements with fractional percentages of alpha to proton number densities exceeding 10%. Ulysses (located at 5.3 AU) observed at least two candidate source features for these enhancements. To identify the correct source structure, a 1D MHD model was used to propagate the Ulysses plasma data to the Voyager radial position (58.2 AU). An ICME-related alpha enhancement observed by Ulysses beginning on day 331 (November 27), 1998 appears to be the correct feature. While a speed jump and cosmic ray decreases were observed by Ulysses in conjunction with this alpha enhancement, the timing of these features differed markedly at Voyager 2. The speed jump arrival-time difference is due to the faster propagation of the shock relative to the rest of the ejecta. It is unclear what mechanism is responsible for the delay in the cosmic ray decrease. Nevertheless, we have demonstrated that alpha enhancement signatures of ICMEs can be used to track these features to heliospheric distances >50 AU. Title: Ionization state and magnetic topology of coronal mass ejections Authors: Henke, T.; Woch, J.; Schwenn, R.; Mall, U.; Gloeckler, G.; von Steiger, R.; Forsyth, R. J.; Balogh, A. Bibcode: 2001JGR...10610597H Altcode: Charge state distributions of heavy solar wind ions measured in interplanetary space can be used to probe the physical conditions in the solar corona. This paper presents a study of the charge state distributions and the magnetic topology of 56 coronal mass ejections (CMEs) observed in interplanetary space by the Ulysses spacecraft. The analysis of the data from the Solar Wind Ion Composition Spectrometer (SWICS) instrument and the Vector Helium Magnetometer (VHM) experiment onboard Ulysses shows a clear correlation between the charge state distributions and the magnetic topology of CMEs. Almost all CMEs whose charge state distributions are shifted to higher charge states with respect to the ambient solar wind have the structure of magnetic clouds, whereas CMEs with the same charge state distributions as the surrounding solar wind do not show magnetic cloud structure. This correlation is found for CMEs observed at low, mid, and high solar latitudes. On the basis of the numerical solution of the ionization/recombination equations for oxygen and silicon, it is investigated which changes of the electron temperature, electron density, and the speed of the ions in the source region of the CMEs can reproduce the observations. It is shown that the main reason for the observed enhancement of higher charge states in the cloud CMEs is an increased electron temperature. However, the evolution of the density and velocity of the CMEs before the charge states freeze in cannot be neglected. Title: Solar Wind Source Diversity as Revealed by its Composition Authors: von Steiger, R.; Zurbuchen, T. H. Bibcode: 2001AGUSM..SH61B01V Altcode: The solar wind is a bimodal stream that is either called fast if it originates from coronal holes, or slow if it originates above the streamer belt. The two quasi-stationary modes are interspersed with transient streams with a duration of several hours to days that may differ radically in their properties: the coronal mass ejections. The stream types are traditionally defined by their kinetic and magnetic properties, perhaps supplemented (in the case of CMEs) by particle signatures. But over the last decade new instrumentation has added heavy ion composition as a diagnostic tool to describing the solar wind. We present the compositional signatures that are associated with the different stream types and the boundaries between them, and we show that in many cases they do more than just adding evidence to an otherwise clear-cut case. Compositional signatures identify stream interfaces, CMEs, or fast streams even in cases where the kinetic signatures are unclear. Moreover, they are a powerful tool for decoding the solar wind origin and acceleration: The charge states of heavy elements are indicative of the coronal temperature and its profile, whereas the elemental abundances probe the conditions and the processes in the chromosphere and lower transition region. Title: The 3-D Heliosphere from the Ulysses and ACE Solar Wind Ion Composition Experiments Authors: von Steiger, R.; Zurbuchen, T. H.; Geiss, J.; Gloeckler, G.; Fisk, L. A.; Schwadron, N. A. Bibcode: 2001SSRv...97..123V Altcode: The source region of solar wind plasma is observed to be directly reflected in the compositional pattern of both elemental and charge state compositions. Slow solar wind associated with streamers shows higher freeze-in temperatures and larger FIP enhancements than coronal hole associated wind. Also, the variability of virtually all compositional parameters is much higher for slow solar wind compared to coronal hole associated wind. We show that these compositional patterns persist even though stream-stream interactions complicate the identification based on in situ plasma parameters. Title: Coronal hole boundaries from the Sun to the Heliosphere: Constraints on the sources and structure of the solar wind Authors: Zurbuchen, T. H.; Von Steiger, R.; Riley, P.; Raymond, J.; Geiss, J.; Antonucci, E.; Abbo, L. Bibcode: 2001AGUSM..SH21B06Z Altcode: Coronal holes are known to be a source of fast, relatively homogenous solar wind. A more variable slow solar wind emerges from the corona adjacent to these fast streams and dominates the low latitude heliosphere. The relation between these two qualitatively different solar wind types is best studied by investigating in detail the structure and evolution of the coronal hole boundaries from the low atmosphere of the Sun, through the corona and into the deep heliosphere. We present a comprehensive data-study combining data from He I 10830A, EIT, UVCS and in situ plasma and composition measurements from SWICS on Ulysses and ACE. First, the location and structure of the coronal hole boundary is determined in each of the remote data-sets. We then project the in situ plasma and composition measurements to 30 Rs using a sophisticated 2D MHD tracing technique. This technique then allows a direct comparison of solar and in situ coronal hole boundaries. We particularly concentrate on UVCS and SWICS data of heavy ions in the solar wind that allow the most rigorous comparisons of solar and in situ data, using the same measurement in the corona as in the solar wind. We will then discuss these data in the context of models and theories of the structure of the three-dimensional structure of the corona and the solar wind. We will also compare the observations with an 3D MHD calculation that predicts super-radial expansion of the fast solar wind associated with coronal holes. This paper is a report of an ISSI International Team on coronal hole boundaries. Title: An ICME Observed by Voyager~2 at 58~AU and by Ulysses at 5~AU Authors: Paularena, K. I.; Wang, C.; von Steiger, R.; Heber, B. Bibcode: 2001AGUSM..SH62A04P Altcode: Between days 175 and 180 of 1999, the PLS instrument on Voyager~2 observed alpha particle enhancements with fractional percentages of alpha to proton number densities exceeding 10%. Ulysses (located at 5.3~AU) observed at least two candidate source features for these enhancements. To identify the correct source structure, a 1D MHD model was used to propagate the Ulysses plasma data to the Voyager radial position (58.2~AU). An ICME-related alpha enhancement observed by Ulysses beginning on day 331, 1998 appears to be the correct feature. While a speed jump and cosmic ray decreases were observed by Ulysses in conjunction with this alpha enhancement, the timing of these features differed markedly at Voyager~2. The speed jump arrival-time difference is due to the faster propagation of the shock relative to the rest of the ejecta. It is unclear what mechanism is responsible for the delay in the cosmic ray decrease. Nevertheless, we have demonstrated that alpha enhancement signatures of ICMEs can be used to track these features to heliospheric distances of over 50~AU. Title: The Astrophysics of Galactic Cosmic Rays Authors: Diehl, R.; Kallenbach, R.; Parizot, E.; Von Steiger, R. Bibcode: 2001agcr.book....3D Altcode: No abstract at ADS Title: The Astrophysics of Galactic Cosmic Rays Authors: Diehl, Roland; Parizot, Etienne; Kallenbach, Reinald; Von Steiger, Rudolf Bibcode: 2001agcr.book.....D Altcode: No abstract at ADS Title: Composition of quasi-stationary solar wind flows from Ulysses/Solar Wind Ion Composition Spectrometer Authors: von Steiger, R.; Schwadron, N. A.; Fisk, L. A.; Geiss, J.; Gloeckler, G.; Hefti, S.; Wilken, B.; Wimmer-Schweingruber, R. F.; Zurbuchen, T. H. Bibcode: 2000JGR...10527217V Altcode: Using improved, self-consistent analysis techniques, we determine the average solar wind charge state and elemental composition of nearly 40 ion species of He, C, N, O, Ne, Mg, Si, S, and Fe observed with the Solar Wind Ion Composition Spectrometer on Ulysses. We compare results obtained during selected time periods, including both slow solar wind and fast streams, concentrating on the quasi-stationary flows away from recurrent or intermittent disturbances such as corotating interaction regions or coronal mass ejections. In the fast streams the charge state distributions are consistent with a single freezing-in temperature for each element, whereas in the slow wind these distributions appear to be composed of contributions from a range of temperatures. The elemental composition shows the well-known first ionization potential (FIP) bias of the solar wind composition with respect to the photosphere. However, it appears that our average enrichment factor of low-FIP elements in the slow wind, not quite a factor of 3, is smaller than that in previous compilations. In fast streams the FIP bias is found to be yet smaller but still significantly above 1, clearly indicating that the FIP fractionation effect is also active beneath coronal holes from where the fast wind originates. This imposes basic requirements upon FIP fractionation models, which should reproduce the stronger and more variable low-FIP bias in the slow wind and a weaker (and perhaps conceptually different) low-FIP bias in fast streams. Taken together, these results firmly establish the fundamental difference between the two quasi-stationary solar wind types. Title: Transition Region: First Ionization Potential Effect Authors: von Steiger, R. Bibcode: 2000eaa..bookE2265V Altcode: The first ionization potential (FIP) effect causes a fractionation, i.e. a change of the relative abundances, of elements with a low FIP in the corona and solar wind as compared with the SOLAR PHOTOSPHERE. These elements (specifically Mg, Si and Fe) are becoming enriched somewhere in the solar atmosphere by an average factor of 2-5 relative to the high-FIP elements (specifically oxygen). The proc... Title: Pick-up Ion Measurements in the Heliosphere - A Review Authors: Kallenbach, R.; Geiss, J.; Gloeckler, G.; von Steiger, R. Bibcode: 2000Ap&SS.274...97K Altcode: Measurements of the composition and spatial distribution of pick-up ions inside the heliosphere are reviewed. The first interstellar ^4He^+ pick-up ions were detected with the SULEICA instrument on the AMPTE spacecraft near Earth's orbit. Most data on pick-up ions were taken in the solar-wind and suprathermal energy range of SWICS on Ulysses while the spacecraft cruised from 1.4 to 5.4 AU and explored the high-latitude heliosphere and solar wind from the ecliptic to +/- 80^° heliolatitude. This includes the discovery of H^+, ^4He^++, ^3He^+, N^+, O^+, and Ne^+ pick-up ions that originate from the interstellar neutral gas penetrating the heliosphere. From their fluxes properties of the interaction region between the heliosphere and the Local Interstellar Cloud such as the limits on filtration and the strength of the interstellar magnetic field have been revealed. Detailed analysis of the velocity distributions of pick-up ions led to 1) the discovery of a new distinct source, the so-called Inner Source, consisting of atoms released from interstellar and interplanetary dust inside the heliosphere, 2) the determination of pick-up ion transport parameters such as the long mean free path for pitch-angle scattering of order 1 AU, and 3) detailed knowledge on the very preferential injection and acceleration of pick-up ions during interplanetary energetic particle events such as Co-rotating Interaction Regions and Coronal Mass Ejections. SWICS measurements have fully confirmed the theory of Fisk, Koslovsky, and Ramaty that pick-up ions derived from the interstellar gas are the dominant source of the Anomalous Cosmic Rays; they are pre-accelerated inside the heliosphere and re-accelerated at the solar-wind Termination Shock according to Pesses, Eichler, and Jokipii. The data indicate that the Inner Source of pick-up ions is largely responsible for the occurence of C^+ in the Anomalous Cosmic Rays. The abundances of recently discovered Inner-Source Mg^+ and Si^+ are solar-wind like and consistent with their abundances in the energetic particles associated with Co-rotating Interaction Regions. Knowledge on the injection and acceleration processes in Co-rotating Interaction Regions is applied to discuss the current observational evidence for the Interplanetary Focusing Cone of the interstellar neutral gas due to the Sun's gravitational force. The 25-150 keV/amu suprathermal ^4He^+ pick-up ion fluxes measured by CELIAS/STOF on board SOHO over 360^° of ecliptic longitude represent a `local' ionization and acceleration of interstellar atoms at 1 AU or smaller heliocentric distances. Completing the first limited data set of SULEICA/AMPTE on ^4He^+ pick-up ions they indicate a density enhancement in the Interplanetary Focusing Cone which is confirmed by recent SWICS/ACE data. Clear evidence for signatures in ecliptic longitude are found in the data on energetic neutral H fluxes observed with the CELIAS/HSTOF sensor on board SOHO. These fluxes are enhanced in the upstream and downstream directions of the interstellar wind. Detection of energetic H atoms, which propagate unaffected by the Heliospheric Magnetic Field, provided for the first time a diagnostic tool for observations near Earth to analyze the structure in ecliptic longitude of the interface region between the heliosphere and the Local Interstellar Cloud. Title: Inner source distributions: Theoretical interpretation, implications, and evidence for inner source protons Authors: Schwadron, N. A.; Geiss, J.; Fisk, L. A.; Gloeckler, G.; Zurbuchen, T. H.; von Steiger, R. Bibcode: 2000JGR...105.7465S Altcode: A new and important source of pickup ions has been recently observed for the first time, the so-called inner source. We examine properties of inner source ions at high heliographic latitudes through analysis of data from the Solar Wind Ion Composition Spectrometer on the Ulysses satellite for a period extending through the year of 1994 while Ulysses achieved its southernmost latitudes. As demonstrated by Gloeckler et al. [this issue], the relative abundances of inner source ions resemble those of the solar wind, which implies that the dominant production mechanism for the inner source ions involves the absorption and reemission of solar wind ions from interplanetary dust grains. A simple transport model is devised that compares favorably to observed distribution functions and provides an important consistency check for the previously mentioned production mechanism. The model comparison also allows for constraints to be placed on the total dust geometric cross section. The observed distribution function of protons reveals a significant contribution from the inner source, but the abundance of inner source protons relative to oxygen falls significantly below the universal abundance. We postulate causes of this low relative abundance. We also find that inner source protons have a sizable pressure and may constitute an important energetic population in the solar wind, particularly near the their source. Title: Interception of comet Hyakutake's ion tail at a distance of 500 million kilometres Authors: Gloeckler, G.; Geiss, J.; Schwadron, N. A.; Fisk, L. A.; Zurbuchen, T. H.; Ipavich, F. M.; von Steiger, R.; Balsiger, H.; Wilken, B. Bibcode: 2000Natur.404..576G Altcode: Remote sensing observations and the direct sampling of material from a few comets have established the characteristic composition of cometary gas. This gas is ionized by solar ultraviolet radiation and the solar wind to form `pick-up' ions, ions in a low ionization state that retain the same compositional signatures as the original gas. The pick-up ions are carried outward by the solar wind, and they could in principle be detected far from the coma. (Sampling of pick-up ions has also been used to study interplanetary dust, Venus' tail and the interstellar medium.) Here we report the serendipitous detection of cometary pick-up ions, most probably associated with the tail of comet Hyakutake, at a distance of 3.4 AU from the nucleus. Previous observations have provided a wealth of physical and chemical information about a small sample of comets, but this detection suggests that remote sampling of comet compositions, and the discovery of otherwise invisible comets, may be possible. Title: The relation of temporal variations of soft X-ray emission from comet Hyakutake to variations of ion fluxes in the solar wind Authors: Neugebauer, M.; Cravens, T. E.; Lisse, C. M.; Ipavich, F. M.; Christian, D.; von Steiger, R.; Bochsler, P.; Shah, P. D.; Armstrong, T. P. Bibcode: 2000JGR...10520949N Altcode: Both the Röntgen X-Ray Satellite (ROSAT) and the Extreme Ultraviolet Explorer (EUVE) have detected soft X-ray emission from comet C/Hyakutake 1996 B2. This emission varied by a factor of about 2 over a few hours and by a factor of 4 from day to day. One explanation for the excitation of cometary X rays is the charge transfer mechanism suggested by Cravens. This process involves charge exchange collisions between highly charged heavy ions in the solar wind and neutral gas in the cometary coma. Oxygen ion fluxes observed by the Charge, Element, and Isotope Analysis System (CELIAS) Mass Time-of-Flight (MTOF) instrument on the SOHO spacecraft and proton fluxes measured by near-Earth spacecraft are mapped to the location of the comet to demonstrate that the comet X-ray variability can be explained on the basis of variability in the solar wind. There is a good correlation between cometary X-ray emission and oxygen ion fluxes and a poorer correlation with proton flux. The correlation between the solar wind oxygen flux and cometary X rays degrades with increasing latitudinal separation of SOHO from the comet. Cometary X-ray emission is not sensitive to variations in solar X-ray fluxes and is unlikely to be caused by crossing of the heliospheric current sheet. The charge transfer mechanism appears to be supported by all the data examined to date. Cometary X rays have some shortcomings as remote sensors of the solar wind, however, because of variations in cometary gas production rates and in the charge states and abundances of heavy solar wind ions. Title: Solar Variability and Climate Authors: Friis-Christensen, E.; Fröhlich, C.; Haigh, J. D.; Schüssler, M.; Von Steiger, R. Bibcode: 2000svc..book.....F Altcode: No abstract at ADS Title: Solar Wind Composition Authors: von Steiger, R.; Schwadron, N. A. Bibcode: 2000ASPC..206...54V Altcode: 2000hesp.conf...54V No abstract at ADS Title: Origin, Injection, and Acceleration of CIR Particles: Observations Report of Working Group 6 Authors: Mason, G. M.; von Steiger, R.; Decker, R. B.; Desai, M. I.; Dwyer, J. R.; Fisk, L. A.; Gloeckler, G.; Gosling, J. T.; Hilchenbach, M.; Kallenbach, R.; Keppler, E.; Klecker, B.; Kunow, H.; Mann, G.; Richardson, I. G.; Sanderson, T. R.; Simnett, G. M.; Wang, Y. -M.; Wimmer-Schweingruber, R. F.; Fränz, M.; Mazur, J. E. Bibcode: 1999SSRv...89..327M Altcode: This report emphasizes new observational aspects of CIR ions revealed by advanced instruments launched on the Ulysses, WIND, SOHO, and ACE spacecraft, and by the unique vantage point of Ulysses which carried out the first survey of Corotating Interaction Region (CIR) properties over a very wide range of heliolatitudes. With this more complete observational picture established, this review is the basis to consider the status of theoretical models on origin, injection, and acceleration of CIR particles reported by Scholer, Mann et al. (1999) in this volume. Title: Corotating Interaction Regions at High Latitudes Authors: Kunow, H.; Lee, M. A.; Fisk, L. A.; Forsyth, R. J.; Heber, B.; Horbury, T. S.; Keppler, E.; Kóta, J.; Lou, Y. -Q.; McKibben, R. B.; Paizis, C.; Potgieter, M. S.; Roelof, E. C.; Sanderson, T. R.; Simnett, G. M.; von Steiger, R.; Tsurutani, B. T.; Wimmer-Schweingruber, R. F.; Jokipii, J. R. Bibcode: 1999SSRv...89..221K Altcode: Ulysses observed a stable strong CIR from early 1992 through 1994 during its first journey into the southern hemisphere. After the rapid latitude scan in early 1995, Ulysses observed a weaker CIR from early 1996 to mid-1997 in the northern hemisphere as it traveled back to the ecliptic at the orbit of Jupiter. These two CIRs are the observational basis of the investigation into the latitudinal structure of CIRs. The first CIR was caused by an extension of the northern coronal hole into the southern hemisphere during declining solar activity, whereas the second CIR near solar minimum activity was caused by small warps in the streamer belt. The latitudinal structure is described through the presentation of three 26-day periods during the southern CIR. The first at ∼24°S shows the full plasma interaction region including fast and slow wind streams, the compressed shocked flows with embedded stream interface and heliospheric current sheet (HCS), and the forward and reverse shocks with associated accelerated ions and electrons. The second at 40°S exhibits only the reverse shock, accelerated particles, and the 26-day modulation of cosmic rays. The third at 60°S shows only the accelerated particles and modulated cosmic rays. The possible mechanisms for the access of the accelerated particles and the CIR-modulated cosmic rays to high latitudes above the plasma interaction region are presented. They include direct magnetic field connection across latitude due to stochastic field line weaving or to systematic weaving caused by solar differential rotation combined with non-radial expansion of the fast wind. Another possible mechanism is particle diffusion across the average magnetic field, which includes stochastic field line weaving. A constraint on connection to a distant portion of the CIR is energy loss in the solar wind, which is substantial for the relatively slow-moving accelerated ions. Finally, the weaker northern CIR is compared with the southern CIR. It is weak because the inclination of the streamer belt and HCS decreased as Ulysses traveled to lower latitudes so that the spacecraft remained at about the maximum latitudinal extent of the HCS. Title: Composition variations in fast solar wind streams Authors: von Steiger, R.; Fisk, L. A.; Gloeckler, G.; Schwadron, N. A.; Zurbuchen, T. H. Bibcode: 1999AIPC..471..143V Altcode: 1999sowi.conf..143V The Ulysses spacecraft has now completed its first revolution around the Sun on its nearly-polar orbit. Thereby it has traversed the extended high speed streams from the polar coronal holes (south in 1993/94, north in 1995/96) which were well-developed during that time of close to minimal solar activity. It is evident that the fluctuations of both the kinetic and the compositional parameters are much weaker in the high-speed streams than they are in the slow solar wind, leading Bame to use the term ``structure-free'' for describing it. It was only the extended time periods Ulysses spent in the polar streams that led to the detection of some structure, the microstreams. From remote observations of the Sun it is clear that the high latitude corona is quite unstructured. The most remarkable features are the polar plumes, which are well detectable because of their higher density and brightness. Also, they are characterized by a difference in composition relative to the coronal hole plasma. These features should in principle be observable in interplanetary space, e.g. by the SWICS mass spectrometer, in the form of abundance variations of heavy ions as well as variations in their charge state composition, which serves as a proxy for the coronal temperature at the site where the stream originated. Using the unique data set of SWICS we examine to what extent polar plumes contribute to fast, coronal hole associated wind. We also study the possible connection between microstreams and polar plumes. Title: Identification of trailing edge solar wind stream interfaces: A comparison of Ulysses plasma and composition measurements Authors: Burton, M. E.; Neugebauer, M.; Crooker, N. U.; von Steiger, R.; Smith, E. J. Bibcode: 1999JGR...104.9925B Altcode: Measurements of the specific entropy argument of the solar wind protons, T/nγ-1, reveal that nearly every occurrence of a high-speed stream seen at Ulysses in 1992-1993 is characterized by an abrupt interface at its trailing edge. These observations, made by the solar wind plasma instrument (SWOOPS), at a heliocentric range of 4.5 to 5 AU show that there is a discontinuous drop in specific entropy at the interface from a high value in the high-speed wind to a lower value in the slow interstream wind. This interface is coincident with, but much more abrupt than, compositional changes measured by the Solar Wind Ion Composition Spectrometer (SWICS) [Geiss et al., 1995]. These results suggest that a relatively thin interface can be identified which separates two plasmas of distinctly different origins as determined by the compositional measurements. A superposed epoch analysis performed on seventeen events reveal the interface is characterized by (1) an abrupt drop in entropy by a factor of ~1/3 due to an enhancement in density along with gradually declining temperature, (2) a distinct drop in the alpha/proton ratio from a value of ~5%, typical of the fast wind, to ~4% characteristic of the slow solar wind, and (3) relative changes in Mg10+/O6+ at the interface which are as large as the variations in the total Mg/O ratio and the freezing-in temperature derived from O7+/O6+. The specific entropy argument, a combination of commonly measured solar wind parameters, gives a strong signature of the trailing edge interface which is preserved as far out in the heliosphere as 5 AU and may provide useful information regarding the coronal origin of solar wind streams. Title: Solar wind stream interfaces in corotating interaction regions: New SWICS/Ulysses results Authors: Wimmer-Schweingruber, Robert F.; von Steiger, Rudolf; Paerli, Raoul Bibcode: 1999JGR...104.9933W Altcode: We have analyzed data from the solar wind ion composition spectrometer (SWICS)/Ulysses instrument taken between August 1996 and May 1997. In this period the Ulysses spacecraft traveled from 28° to 11°N and encountered a highly regular pattern of high-speed streams alternating with slow solar wind. Heliocentric distance varied between 4.3 and 5.1 astronomical units (AU). Using proton and alpha-particle kinetic parameters (density, speed, and kinetic temperatures) as well as charge state and elemental composition data, we identify the stream interfaces in the corotating interaction regions (CIRs) observed in this period. As Wimmer-Schweingruber et al. [1997] previously reported for a similar period in 1992/1993, stream interfaces are the sites of compositional changes between values typical of the slow solar wind and values typical of high-speed streams. During that period, Ulysses traveled from 13° to 34°S and from 4.5 to 5.4 AU. In spite of the similarity of the heliospheric regions probed during 1992/1993 and 1996/1997 the corotating interaction regions observed in 1996/1997 are quite different from those observed in 1992/1993. We observe fewer (11) CIRs in 1996/1997 than in the previous period (15); the CIRs are less evolved, i.e., the kinetic signatures at the stream interface are less clear; and mainly, only 3 out of the 11 CIRs are bounded by forward-reverse shock pairs, whereas in 1992/1993, 13 out of 15 were. This may have important consequences for particle acceleration in CIRs in the inner heliosphere. Title: The Transition Between Fast and Slow Solar Wind from Composition Data Authors: Zurbuchen, T. H.; Hefti, S.; Fisk, L. A.; Gloeckler, G.; von Steiger, R. Bibcode: 1999SSRv...87..353Z Altcode: The transition between coronal hole associated fast solar wind and slow solar wind is studied using data from the high resolution mass spectrometer SWICS on ACE. We discuss the data in the framework of a recent theory about the global heliospheric magnetic field and conclude that the data are consistent with magnetic connections between field-lines in the fast and in the slow wind. Title: Origin, Injection, and Acceleration of CIR Particles: Observations Authors: Mason, G. M.; Von Steiger, R.; Decker, R. B.; Desai, M. I.; Dwyer, J. R.; Fisk, L. A.; Gloeckler, G.; Gosling, J. T.; Hilchenbach, M.; Kallenbach, R.; Keppler, E.; Klecker, B.; Kunow, H.; Mann, G.; Richardson, I. G.; Sanderson, T. R.; Simnett, G. M.; Wang, Y. -M.; Wimmer-Schweingruber, R. F.; Fränz, M.; Mazur, J. E. Bibcode: 1999cir..book..327M Altcode: No abstract at ADS Title: Corotating Interaction Regions at High Latitudes Authors: Kunow, H.; Lee, M. A.; Fisk, L. A.; Forsyth, R. J.; Heber, B.; Horbury, T. S.; Keppler, E.; Kóta, J.; Lou, Y. -Q.; McKibben, R. B.; Paizis, C.; Potgieter, M. S.; Roelof, E. C.; Sanderson, T. R.; Simnett, G. M.; von Steiger, R.; Tsurutani, B. T.; Wimmer-Schweingruber, R. F.; Jokipii, J. R. Bibcode: 1999cir..book..221K Altcode: No abstract at ADS Title: Differences in the O7+/O6+ ratio of magnetic cloud and non-cloud coronal mass ejections Authors: Henke, T.; Woch, J.; Mall, U.; Livi, S.; Wilken, B.; Schwenn, R.; Gloeckler, G.; von Steiger, R.; Forsyth, R. J.; Balogh, A. Bibcode: 1998GeoRL..25.3465H Altcode: On its trajectory to Jupiter and over the poles of the Sun the Ulysses spacecraft has observed a considerable number of Coronal Mass Ejection (CME) transients in slow and in fast solar wind streams. The analysis of the magnetic field topology and the O7+/O6+ charge state ratio of 56 of these events has yielded strong evidence for a systematic connection between the two features. Coronal mass ejections with magnetic cloud structure have an increased O7+/O6+ ratio with respect to the ambient solar wind whereas non-cloud CMEs do not show enhanced O7+/O6+ ratios. We discuss possible mechanisms based on the freezing-in concept that can account for the observation. Title: Spatial structure of the solar wind and comparisons with solar data and models Authors: Neugebauer, M.; Forsyth, R. J.; Galvin, A. B.; Harvey, K. L.; Hoeksema, J. T.; Lazarus, A. J.; Lepping, R. P.; Linker, J. A.; Mikic, Z.; Steinberg, J. T.; von Steiger, R.; Wang, Y. -M.; Wimmer-Schweingruber, R. F. Bibcode: 1998JGR...10314587N Altcode: Data obtained by instruments on the Ulysses spacecraft during its rapid sweep through >90° of solar latitude, crossing the solar equator in early 1995, were combined with data obtained near Earth by the Wind spacecraft to study the spatial structure of the solar wind and to compare to different models of the interplanetary magnetic field derived from solar observations. Several different source-surface models matched the double sinusoidal structure of the heliospheric current sheet (HCS) but with differences in latitude as great as 21°. The source-surface model that included an interplanetary current sheet gave poorer agreement with observed current-sheet crossings during this period than did the other source-surface models or an MHD model. The differences between the calculated and observed locations of the HCS were minimized when 22° of solar rotation was added to the constant-velocity travel time from the source surface to the spacecraft. The photospheric footpoints of the open field lines calculated from the models generally agreed with observations in the He 10,830 Å line of the locations of coronal holes with the exceptions that (1) in some places, open field lines originated outside the coronal hole boundaries and (2) the models show apparently closed-field regions just inside some coronal hole boundaries. The patterns of mismatches between coronal hole boundaries and the envelopes of open field lines persisted over at least three solar rotations. The highest-speed wind came from the polar coronal holes, with the wind originating deeper within the hole being faster than the wind coming from near the hole boundary. Intermediate and slow streams originated in smaller coronal holes at low latitudes and from open field regions just outside coronal hole boundaries. Although the HCS threaded regions of low speed, low helium abundance, high ionization temperature, and a high ratio of magnesium to oxygen densities (a surplus of an element with low first-ionization potential), there was a great deal of variation in these parameters from one place to another along the HCS. The gradient of speed with latitude varied from 14 to 28 kms-1deg-1. Title: Composition Aspects of the Upper Solar Atmosphere Rapporteur Paper III Authors: von Steiger, R. Bibcode: 1998SSRv...85..407V Altcode: This rapporteur paper discusses the solar corona and the solar wind in the context of their chemical composition. The abundances of elements, both obtained by optical and by in situ observations, are used to infer the sources of the slow solar wind and of the fast streams. The first ionisation potential (FIP) fractionation effect is also discussed, in particular the agreed basics and the open questions. Title: The Expansion of Coronal Plumes in the Fast Solar Wind Authors: Del Zanna, L.; von Steiger, R.; Velli, M. Bibcode: 1998SSRv...85..349D Altcode: Coronal plumes are believed to be essentially magnetic features: they are rooted in magnetic flux concentrations at the photosphere and are observed to extend nearly radially above coronal holes out to at least 15 solar radii, probably tracing the open field lines. The formation of plumes itself seems to be due to the presence of reconnecting magnetic field lines and this is probably the cause of the observed extremely low values of the Ne/Mg abundance ratio. Title: Foreword Authors: Fröhlich, C.; Huber, M. C. E.; Solanki, S. K.; von Steiger, R. Bibcode: 1998SSRv...85...11F Altcode: No abstract at ADS Title: O5+ in High Speed Solar Wind Streams: SWICS/Ulysses Results Authors: Wimmer-Schweingruber, Robert F.; von Steiger, Rudolf; Geiss, Johannes; Gloeckler, George; Ipavich, Fred M.; Wilken, Berend Bibcode: 1998SSRv...85..387W Altcode: Recent observations with UVCS on SOHO of high outflow velocities of O5+ at low coronal heights have spurred much discussion about the dynamics of solar wind acceleration. On the other hand, O6+ is the most abundant oxygen charge state in the solar wind, but is not observed by UVCS or by SUMER because this helium-like ion has no emission lines falling in the wave lengths observable by these instruments. Therefore, there is considerable interest in observing O5+ in situ in order to understand the relative importance of O5+ with respect to the much more abundant O6+. High speed streams are the prime candidates for the search for O5+ because all elements exhibit lower freezing-in temperatures in high speed streams than in the slow solar wind. The Ulysses spacecraft was exposed to long time periods of high speed streams during its passage over the polar regions of the Sun. The Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses is capable of resolving this rare oxygen charge state. We present the first measurement of O5+ in the solar wind and compare these data with those of the more abundant oxygen species O6+ and O7+. We find that our observations of the oxygen charge states can be fitted with a single coronal electron temperature in the range of 1.0 to 1.2 MK assuming collisional ionization/recombination equilibrium with an ambient Maxwellian electron gas. Title: Primordial nuclei and their Galactic evolution. Proceedings. 4th ISSI Workshop, Bern (Switzerland), 6 - 10 May 1997. Authors: Prantzos, N.; Tosi, M.; von Steiger, R. Bibcode: 1998SSRv...84.....P Altcode: The following topics are dealt with: early Universe, extragalactic objects, low-Z stars, Galactic disk and Galactic evolution, solar nebula, and the local interstellar medium. Title: Solar Composition and Its Evolution -- From Core to Corona Authors: Fröhlich, C.; Huber, M. C. E.; Solanki, S. K.; von Steiger, R. Bibcode: 1998sce..conf.....F Altcode: No abstract at ADS Title: MHD models of coronal plumes Authors: Del Zanna, L.; Hood, A.; Velli, M.; von Steiger, R. Bibcode: 1998ESASP.421..359D Altcode: 1998sjcp.conf..359D No abstract at ADS Title: Cosmic rays in the heliosphere. Proceedings. ISSI (International Space Science Institute) Workshop, Bern (Switzerland), 17 - 20 Sep 1996 and 10 - 14 Mar 1997. Authors: Fisk, L. A.; Jokipii, J. R.; Simnett, G. M.; von Steiger, R.; Wenzel, K. -P. Bibcode: 1998SSRv...83.....F Altcode: The following topics were dealt with: solar modulation; solar wind; magnetic fields; heliosphere; galactic cosmic rays; anomalous cosmic rays. Title: O5+ in High Speed Solar Wind Streams: SWICS/Ulysses Results Authors: Wimmer-Schweingruber, R. F.; von Steiger, R.; Geiss, J.; Gloeckler, G.; Ipavich, F. M.; Wilken, B. Bibcode: 1998sce..conf..387W Altcode: No abstract at ADS Title: Primordial Nuclei and their Galactic Evolution Authors: Prantzos, Nikos; Tosi, Monica; von Steiger, Rudolf Bibcode: 1998pnge.conf.....P Altcode: No abstract at ADS Title: Composition Aspects of the Upper Solar Atmosphere Authors: von Steiger, R. Bibcode: 1998sce..conf..407V Altcode: No abstract at ADS Title: Latitude Manifestations of the Solar Wind Authors: von Steiger, R. Bibcode: 1998HiA....11..842V Altcode: Dependencies of solar wind parameters as a function of latitude are presented and discussed, based on measurement of the Ulysses mission during times of declining or minimum solar activity. The heliosphere is found to be structured into a band of slow solar wind at low latitudes and two large high-speed streams from the polar coronal holes. Only small trends of solar wind parameters with heliolatitude are found within these streams. A small but significant temperature difference is seen between the south and the north polar coronal hole. Title: Solar composition and its evolution - from core to corona. Proceedings. ISSI (International Space Science Institute) Workshop, Bern (Switzerland), 26 - 30 Jan 1998. Authors: Fröhlich, C.; Huber, M. C. E.; Solanki, S. K.; von Steiger, R. Bibcode: 1998SSRv...85.....F Altcode: The following topics were dealt with: solar composition, solar evolution, the solar interior, helioseismology, photosphere, chromosphere, solar corona, solar wind, the Sun as a Sun-like star. Title: The Expansion of Coronal Plumes in the Fast Solar Wind Authors: del Zanna, L.; von Steiger, R.; Velli, M. Bibcode: 1998sce..conf..349D Altcode: No abstract at ADS Title: Solar wind stream interfaces in corotating interaction regions: SWICS/Ulysses results Authors: Wimmer-Schweingruber, Robert F.; von Steiger, Rudolf; Paerli, Raoul Bibcode: 1997JGR...10217407W Altcode: Motivated by the well-known differences in charge state and even elemental composition of the slow solar wind as compared to high-speed streams, we have analyzed observations made by the Solar Wind Ion Composition Spectrometer (SWICS)/Ulysses mass spectrometer of the series of corotating interaction regions (CIRs) encountered by Ulysses in 1992/1993 at 4.5-5.4 AU from the Sun. Stream interfaces (SIs) are first identified within each CIR using the kinetic parameters (density and thermal speed) of the main components, protons and alpha particles. We then show that SIs are also the location of the expected compositional changes in the heavy ion components, such as the freezing-in temperatures of C and O and the strength of FIP fractionation as given by the Mg/O abundance ratio, to within the time resolution with which these parameters may be obtained by SWICS. The changes in freezing-in temperatures are so clear that they in turn may be used as a robust indicator of the SI location and even reveal that some of the SI crossings were in fact multiple. We conclude that the heavy ion composition of the solar wind changes abruptly at the SI and remains well preserved out to large heliocentric distances. Title: Composition of the Solar Wind Authors: von Steiger, R.; Geiss, J.; Gloeckler, G. Bibcode: 1997cwh..conf..581V Altcode: 2006mslp.conf..581V No abstract at ADS Title: Search for the Origin of Quiet-Time Particle Fluxes in the Inner Heliosphere Authors: Kiraly, P.; Bothmer, V.; Kecskemety, K.; Keppler, E.; Kudela, K.; Kunow, H.; Logachev, Yu. I.; sMüller-Mellin, R.; Rodriguez-Pacheco, J.; von Steiger, R.; Torsti, J.; Valtonen, E.; Zeldovich, M. A. Bibcode: 1997ICRC....2..477K Altcode: 1997ICRC...25b.477K No abstract at ADS Title: Foreword by the volume editors Authors: von Steiger, R.; Lallement, R.; Lee, M. Bibcode: 1996SSRv...78D..13V Altcode: No abstract at ADS Title: The heliosphere in the local interstellar medium. Proceedings. 1. ISSI (International Space Science Institute) Workshop, Bern (Switzerland), 6 - 10 Nov 1995. Authors: von Steiger, R.; Lallement, R.; Lee, M. A. Bibcode: 1996SSRv...78.....V Altcode: The following topics were dealt with: outer heliosphere, solar wind-heliosphere interaction, interstellar pickup ions, interplanetary magnetic field, radio emissions, ionization processes, the termination shock, the local interstellar medium, interstellar dust. Title: Origin of C+ ions in the heliosphere Authors: Geiss, J.; Gloeckler, G.; von Steiger, R. Bibcode: 1996SSRv...78...43G Altcode: C+ pickup ions were investigated with the SWICS instrument along the trajectory of Ulysses, covering a broad range of solar latitude and distance. Whereas nearly all the observed H+, He+, N+, O+ and Ne+ pickup ions are created from the interstellar gas penetrating deep into the heliosphere, C+ comes primarily from an “inner source” which is located at a solar distance below a few AU and extends over all heliospheric latitudes investigated up to now. We present evidence that the C+ originates from carbon compounds evaporating from interstellar grains. This inner source also produces some O+ and N+ with estimated relative abundances ofC+/O+ ∼ 1 and N+/O+ ∼ 0.2. However, the total amount of O+ and N+ produced by this inner source is only of the order of 10-3 as compared to the total production of O+ and N+ from the interstellar gas in the heliosphere, respectively. Thus the inner source does not significantly contribute to oxygen or nitrogen in the anomalous cosmic rays (ACR) but its contribution to ACR-carbon may not be negligible. Title: Coronal hole differential rotation rate observed with SWICS/Ulysses Authors: Zurbuchen, Th.; Bochsler, P.; von Steiger, R. Bibcode: 1996AIPC..382..273Z Altcode: We discuss the latitude variation of the coronal hole differential rotation investigating persistent structures in high speed streams as observed from SWICS Ulysses during its first passage of the southern polar hole in 1993-1994. We find a slower rotation rate near the ecliptic than what is inferred from averaged photospheric features, e.g. from sunspots. At intermediate latitudes we find a rate similar to the equatorial rotation rate indicating a quasi-rigid rotation of the polar coronal hole. At latitudes >65° no persistent structures to determine the polar rotation have been observed. For the passage of the southern heliosphere in 1993/94 we find a latitudinal dependence of the sidereal rotation rate of the coronal hole which can be approximated by ωSW=[13.13+1.94 sin2(Θ)]°/day, where Θ denotes the solar latitude. Title: Solar wind composition and charge states Authors: von Steiger, R. Bibcode: 1996AIPC..382..193V Altcode: The abundances and charge states of the heavy ions present in the solar wind are important tracers for conditions and processes in the solar corona and chromosphere. The elemental abundances are known to be fractionated with respect to the photosphere, with the fractionation being organized best by the first ionization time. Since the first ionization occurs in the upper the chromosphere, the solar wind abundances are indicative for the conditions at this site. On the other hand, the solar wind charge states provide information about the coronal temperature, where they are frozen-in at altitudes between 1.5 and 3.5 solar radii. The charge state distributions of different elements can thus be used to infer a coronal temperature profile. The two types of steady solar wind, fast streams from coronal holes and slow, interstream wind, are significantly different in both of these signatures. This implies that they are separated by a boundary extending through the corona and down into the chromosphere, i.e. that the slow wind is not merely emanating from the coronal hole boundary regions. Title: Kinetic temperature ratios of O6+ and He2+: Observations from Wind/MASS and Ulysses/SWICS Authors: Cohen, C. M. S.; Collier, M. R.; Hamilton, D. C.; Gloeckler, G.; Sheldon, R. B.; von Steiger, R.; Wilken, B. Bibcode: 1996GeoRL..23.1187C Altcode: We present results from a two spacecraft study of the ratio of O6+ and He2+ kinetic temperatures as a function of solar wind speed. Data from the Wind/MASS and Ulysses/SWICS instruments both indicate the O6+/He2+ kinetic temperature ratio increases with increasing solar wind speed, peaking near 500 km/s. Above 500 km/s, the ratio appears to decrease slightly. Values near unity were obtained for slow solar wind while fast wind yielded ratios substantially higher than what is expected from the general rule FD1 TiTj≈MiMj.(1) Although averaging over all data would result in the nominal ratio of 4, deviations from equation (1) appear to be common and the assumption of equal thermal velocities should not be made a priori. Title: Solar wind abundances from ULYSSES Authors: von Steiger, R. Bibcode: 1996ASPC..109..491V Altcode: 1996csss....9..491V No abstract at ADS Title: Proton Temperatures, Electron Temperatures and Outflows in the Extended Solar Corona. Authors: Kohl, J. L.; Gardner, L. D.; Strachan, L.; Cohen, C. M. S.; Galvin, A. B.; Gloeckler, G.; Guhathakurta, M.; Fisher, R. R.; Ko, Y. -K.; Geiss, J.; von Steiger, R. Bibcode: 1996ASPC..109...99K Altcode: 1996csss....9...99K No abstract at ADS Title: Element fractionation by diffusion in the solar chromosphere. Authors: Marsch, E.; von Steiger, R.; Bochsler, P. Bibcode: 1995A&A...301..261M Altcode: A new mechanism to explain the observed first ionization potential (FIP) fractionation of coronal and solar wind element abundances is proposed. By the FIP fractionation, low-FIP (<10eV) elements are enriched in the solar corona and solar wind relative to the photosphere. This effect has been located earlier to take place in the chromosphere, at densities of N =~10^16^-10^18^m^-3^ and a temperature of T=~10^4^K, where a large fraction of the gas is still neutral. We discuss a new mechanism for the FIP fractionation in the form of a stationary diffusion model. It is based on a weakly stratified chromospheric layer of constant density of the element hydrogen and constant temperature. This layer is permeated everywhere by ionizing photons and contains a homogeneous vertical magnetic field. Otherwise, our model does not invoke any particular geometry or special set up of the system. It is thus founded solely on robust and well understood atomic collisional physics. Technically, a boundary value problem of four coupled differential equations is solved for each chemical element, i.e. a continuity equation and a momentum equation for both atoms and singly ionized particles. By splitting the system into a main gas (hydrogen) and trace gases (16 elements from He to Xe), an analytical solution for the former can be found. This then serves as a background for the numerical integration of each trace gas system, for which we consider collisions between its atoms and ions with the main gas, i.e. protons and hydrogen. Boundary conditions are such that the gas is neutral at the bottom of the slab and fully ionized at its top, as a result of irradiation by the solar coronal EUV. Starting with a uniform density at the bottom of the layer, we find that, after a few hydrogen diffusion lengths, each minor species asymptotically approaches a constant density. The ratios of these density values to some reference trace element reproduce the observed FIP fractionation pattern of heavy elements remarkably well. The step between low-FIP and high-FIP element abundances is about a factor of 5, and He is somewhat depleted relative to the high-FIP elements, in agreement with the observations. The model fractionation pattern proves to be remarkably stable against changes in the external parameters (within reasonable chromospheric values), particularly N and T. Title: Radial gradients of ion densities and temperatures derived from SWICS/Ulysses observations Authors: Liu, S.; Marsch, E.; Livi, S.; Woch, J.; Wilken, B.; von Steiger, R.; Gloeckler, G. Bibcode: 1995GeoRL..22.2445L Altcode: Mean density and temperature gradients of solar wind protons and α particles are derived from SWICS/Ulysses observations between 1.2 and 5.4 AU in the ecliptic plane during declining solar activity. All parameters are sorted in solar wind speed classes. The radial gradients show a similar behavior for both ion species. In the slow solar wind protons as well as α particles are found to expand adiabatically all the way out to many AUs, while in the fast wind ions evolve non-adiabatically and are heated by interplanetary sources. The α particle to proton temperature and density ratios are also determined. They do not show any clear radial dependence. Title: Observations of the solar wind and interstellar pick-up ion populations in the heliosphere with ULYSSES Authors: Gloeckler, G.; Geiss, J.; von Steiger, R. Bibcode: 1995AdSpR..16i.343G Altcode: 1995AdSpR..16..343G The solar wind (SW) and interstellar pick-up ions (IPI) are the dominant ion populations in the heliosphere. While SW ions are by far the most abundant at low thermal energies and closer to the sun, IPI ions with thermal speeds exceeding the SW bulk speed become dynamically more and more important beyond a few AU. Measurements of the characteristics (composition, charge states and distribution functions) of these ion populations provide essential information about (1) solar abundances, acceleration of the solar wind and conditions in the corona, (2) local heliospheric processes that shape the distribution functions of SW ions and IPI, (3) conditions in the outer heliosphere, including acceleration processes that produce the anomalous cosmic rays, and (4) characteristics and composition of the local interstellar cloud. The orbit and timing of Ulysses is particularly well suited for these observations: Polar passes of Ulysses at solar minimum allow us to study the solar wind from polar coronal holes under the simplest conditions. Extended time periods at heliocentric distances between ~3 and 5 AU make it possible to observe in addition to He^+ a number of new IPI species (H^+, O^+, N^+, Ne^+, and He^++). We will discuss a number of results based on ion composition and energy spectra measured from 0.6 to 60 keV/e with the time-of-flight vs. energy Solar Wind Ion Composition Spectrometer (SWICS). We find that (a) the composition of the solar wind from coronal holes is least biased compared to the solar photospheric composition and (b) the composition in the interstellar medium deduced from IPI measurements resembles to better than a factor of two solar system abundances. These observations show that SW and IPI are a relatively unbiased samples of the solar and interstellar material respectively which can be used to study the isotopic and chemical compositions in these remote regions. Title: Abundance variations in the solar wind Authors: von Steiger, R.; Schweingruber, R. F. Wimmer; Geiss, J.; Gloeckler, G. Bibcode: 1995AdSpR..15g...3V Altcode: 1995AdSpR..15Q...3V The solar wind (SW) allows us to probe the solar material in situ, particularly its composition, without the need to fly a spacecraft to inhospitably small heliocentric distances. However, it turns out that this plasma source is biased with respect to the photosphere. Elements with a low first ionization potential (FIP) are overabundant by a factor of 3-5 relative to high-FIP elements in the slow SW, but only by a factor of 1.5-2 in the fast streams emanating from coronal holes. It is thus important to have a good understanding of this FIP fractionation effect, which operates between the photosphere and the corona. Such a theory may improve on our understanding of the solar atmosphere and SW acceleration. We present SW measurements, concentrating on results of the SWICS mass spectrometer on Ulysses, which is currently sampling the SW on a highly inclined orbit. In 1992/93, Ulysses was traversing a recurrent high-speed stream once per solar rotation, alternating with slow SW, providing an unique opportunity to compare these two SW types. We find a strongly positive correlation of low- to high-FIP element ratios (such as Mg/O) with coronal temperature, which in turn is anticorrelated with the SW speed. The correlation of these three parameters--one chromospheric, one coronal, and one from the SW--points at a common cause for their variations, and provides a challenge to theorists to model these three domains in an unified approach. Further, abundance variations found in the SW from coronal streamers and in coronal mass ejections are presented and discussed. Finally, we address the question of abundance variations within the fast streams, looking for abundance gradients with heliographic latitude. Title: Dynamic properties of helium ions in the solar wind Authors: Zurbuchen, Th.; Bochsler, P.; von Steiger, R. Bibcode: 1995sowi.conf...73Z Altcode: We characterize the dynamic properties of He ions of the solar wind. Because of the non-negligible abundance and the significant fraction of momentum flux inherent in helium ions, this species has an influence on the state of turbulence. Especially, we analyze the helium dynamic properties of different solar wind types. After a discussion of the influence of measurement errors on the statistical analysis of He bulk velocities, we investigate the structure function dependency on the solar wind state. We find a self-similar sealing in the range of minutes to days with characteristic structure function slopes deviating from the canonical Kolmogorov values. For comparison with previous studies, we also analyze H structure functions of the same time periods and discuss differences of coinciding He and H structure functions in the framework of the concept of intermittency. Title: Large-scale variations of solar wind elemental composition and charge states with heliospheric latitude Authors: Woch, J.; Wilken, B.; Livi, S.; von Steiger, R.; Geiss, J.; Gloeckler, G. Bibcode: 1995sowi.confQ..74W Altcode: The Solar Wind Ion Composition Spectrometer (SWICS) onboard Ulysses allows determination of the elemental composition of the solar wind and the charge states of all major solar wind ion species. Ulysses left the ecliptic plane in early 1992, crossed the Sun's south polar region in late 1994 and made a fast approach back towards the ecliptic in the first half of 1995. Data from this period were investigated for long-term variations in the solar wind composition. At midlatitudes Ulysses encountered periodically the fast solar wind stream emerging from the south coronal hole. As a consequence, dramatic variations in the charge-states arise, between high charge-states dominating in the current sheet solar wind and low charge states in the coronal hole stream. However, the initial analysis indicates that from midlatitudes onwards, with Ulysses permanently immersed in the coronal hole stream, the charge state and elemental abundance ratios of the major solar wind ion species stayed essentially constant. This implies that the temperature profile in the coronal hole at solar wind source altitudes exhibit no variation with solar latitude. It confirms that the south coronal hole is essentially unstructured down to scale lengths of several degrees in solar latitude. Title: The Southern High-Speed Stream: Results from the SWICS Instrument on Ulysses Authors: Geiss, J.; Gloeckler, G.; von Steiger, R.; Balsiger, H.; Fisk, L. A.; Galvin, A. B.; Ipavich, F. M.; Livi, S.; McKenzie, J. F.; Ogilvie, K. W.; Wilken, B. Bibcode: 1995Sci...268.1033G Altcode: The high-speed solar wind streaming from the southern coronal hole was remarkably uniform and steady and was confined by a sharp boundary that extended to the corona and chromosphere. Charge state measurements indicate that the electron temperature in this coronal hole reached a maximum of about 1.5 million kelvin within 3 solar radii of the sun. This result, combined with the observed lack of depletion of heavy elements, suggests that an additional source of momentum is required to accelerate the polar wind. Title: Solar wind helium isotopic composition from SWICS/ULYSSES Authors: Bodmer, R.; Bochsler, P.; Geiss, J.; von Steiger, R.; Gloeckler, G. Bibcode: 1995SSRv...72...61B Altcode: This is the first study of the isotopic composition of solar wind helium with the SWICS time-of flight mass spectrometer. Although the design of SWICS is not optimized to measure3He abundances precisely,4He/3He flux ratios can be deduced from the data. The long term ratio is 2290±200, which agrees with the results obtained with the ICI magnetic mass spectrometer on ISEE-3 and with the Apollo SWC foil experiments. The ULYSSES spacecraft follows a trajectory which is ideal for the study of different solar wind types. During one year, from mid-1992 to mid-1993, it was in a range of heliographic latitudes where a recurrent fast stream from the southern polar coronal hole was observed every solar rotation. Solar wind bulk velocities ranged from 350 km/s to 950 km/s which would, in principle allow us to identify velocity-correlated compositional variations. Our investigation of solar wind helium, however, shows an isotopic ratio which does not depend on the solar wind speed. Title: Solar Wind Charge States Measured by Ulysses/SWICS in the South Polar Hole Authors: Galvin, A. B.; Ipavich, F. M.; Cohen, C. M. S.; Gloeckler, G.; von Steiger, R. Bibcode: 1995SSRv...72...65G Altcode: The Ulysses mission now has an extensive data base covering several passes of the south polar coronal hole as the spacecraft proceeds to higher latitudes. Using composition measurements from the SWICS experiment on the Ulysses spacecraft, we have obtained charge state distributions, and hence inferred coronal ionization temperatures, for several solar wind species. In particular, we present an overview of Oxygen ionization temperature measurements, based on the O7+/O6+ ratio, for the period January 1993 until April 1994 (∼23°S to ∼61°S heliographic latitude), and detailed Oxygen, Silicon and Iron charge state distributions of the south polar hole during a two month period of nearly continuous hole coverage, Dec 1993 Jan 1994 (∼45°S to 52°S heliographic latitude). Title: Kinetic Properties of Heavy Ions in the Solar Wind From SWICS/Ulysses Authors: von Steiger, R.; Geiss, J.; Gloeckler, G.; Galvin, A. B. Bibcode: 1995SSRv...72...71V Altcode: The kinetic properties of heavy ions in the solar wind are known to behave in a well organized way under most solar wind flow conditions: Their speeds are all equal and faster than that of hydrogen by about the local Alfvén speed, and their kinetic temperatures are proportional to their mass. The simplicity of these properties points to a straightforward physical interpretation; wave-particle interactions with Alfvén waves are the probable cause. With the SWICS sensor on board Ulysses, it is now possible to investigate the kinetic properties of many more ion species than before. Furthermore, the transition of Ulysses into the fast stream emanating from the south polar coronal hole since 1992 allows us to study these properties both in the slow, interstream solar wind, as well as in an unambiguously identified fast stream. We present data from SWICS/Ulysses on the dominant ions of He, C, O, Ne, and Mg. As a result we find that, both in the slow wind and in fast streams, the isotachic property is obeyed even better than it could be determined by the ICI instrument on ISEE-3. The mass proportionality ofT kin is also shown to hold for these ions, including the newly identified C and Mg. Title: Origin of the Solar Wind From Composition Data Authors: Geiss, J.; Gloeckler, G.; von Steiger, R. Bibcode: 1995SSRv...72...49G Altcode: The ESA/NASA spacecraft Ulysses is making, for the first time, direct measurements in the solar wind originating from virtually all places where the corona expands. Since the initial two polar passes of Ulysses occur during relatively quiet solar conditions, we discuss here the three main regimes of quasi-stationary solar wind flow: the high speed streams (HSSTs) coming out of the polar coronal holes, the slow solar wind surrounding the HSSTs, and the streamers which occur at B-field reversals. Comparisons between H-α maps and data taken by Ulysses demonstrate that as a result of super-radial expansion, the HSSTs occupy a much larger solid angle than that derived from radial projections of coronal holes. Data obtained with SWICS-Ulysses confirm that the strength of the FIP effect is much reduced in the HSSTs. The systematics in the variations of elemental abundances becomes particularly clear, if these are plotted against the time of ionisation (at the solar surface) rather than against the first ionisation potential (FIP). We have used a superposed-epoch method to investigate the changes in solar wind speed and composition measured during the 9-month period in 1992/93 when Ulysses regularly passed into and out of the southern HSST. We find that the patterns in the variations of the Mg/O and O7+/O6+ ratios are virtually identical and that their transition from high to low values is very steep. Since the Mg/O ratio is controlled by the FIP effect and the O7+/O6+ ratio reflects the coronal temperature, this finding points to a connection between chromospheric and coronal conditions. Title: New Results for Outflow and LOS Velocities in the Solar Wind Acceleration Region of the Corona Authors: Strachan, L.; Gardner, L. D.; Kohl, J. L.; Guhathakurta, M.; Fisher, R. R.; Cohen, C. M. S.; Galvin, A. B.; Gloeckler, G.; Ko, Y. -K.; Geiss, J.; von Steiger, R. Bibcode: 1995SPD....26..719S Altcode: 1995BAAS...27..970S No abstract at ADS Title: C+ pickup ions in the heliosphere and their origin Authors: Geiss, J.; Gloeckler, G.; Fisk, L. A.; von Steiger, R. Bibcode: 1995JGR...10023373G Altcode: C+ pickup ions were discovered with the solar wind ion composition spectrometer flying on Ulysses. Whereas the other nonlocally occurring pickup ions are produced from the interstellar gas penetrating deep into the heliosphere, C+ comes from an ``inner source'' which is located at a solar distance of a few AU and extends over all heliospheric latitudes investigated so far. The total production of C+, N+, and O+ by this inner source is of the order of 10-3 relative to the total production of O+ from the interstellar gas in the heliosphere. Thus the inner source does not significantly contribute to oxygen or nitrogen in the anomalous cosmic rays (ACR), but its contribution to ACR carbon may not be negligible. We propose that the inner source material is carbon compounds evaporating from grains. At this time, the evidence points to interstellar grains as the major source, but we do not want to exclude yet a contribution from grains of solar system origin. Title: Kinetic Properties of Heavy Ions in the Solar Wind From SWICS/Ulysses Authors: von Steiger, R.; Geiss, J.; Gloeckler, G.; Galvin, A. B. Bibcode: 1995hlh..conf...71V Altcode: No abstract at ADS Title: Fractionation of the solar wind Authors: von Steiger, R. Bibcode: 1995HiA....10..310V Altcode: No abstract at ADS Title: Origin of the Solar Wind From Composition Data Authors: Geiss, J.; Gloeckler, G.; von Steiger, R. Bibcode: 1995hlh..conf...49G Altcode: No abstract at ADS Title: Solar Wind Charge States Measured by Ulysses/SWICS in the South Polar Hole Authors: Galvin, A. B.; Ipavich, F. M.; Cohen, C. M. S.; Gloeckler, G.; von Steiger, R. Bibcode: 1995hlh..conf...65G Altcode: No abstract at ADS Title: Solar Wind Helium Isotopic Composition from SWICS/Ulysses Authors: Bodmer, R.; Bochsler, P.; Geiss, J.; von Steiger, R.; Gloeckler, G. Bibcode: 1995hlh..conf...61B Altcode: No abstract at ADS Title: Solar and Heliospheric Processes from Solar Wind Composition Measurements Authors: Geiss, J.; Gloeckler, G.; von Steiger, R. Bibcode: 1994RSPTA.349..213G Altcode: Composition measurements in the solar wind provide important information for solar system science and astrophysics. We show in this report how ion composition data are used to investigate chromospheric and coronal processes. Isotopic abundances in the Sun can best be derived from solar wind measurements. 3He/4He is an isotopic ratio with far-reaching implications. It allows us to determine the deuterium abundance in the proto-solar nebula, which in turn leads to an estimate of deuterium production in the early universe. The interstellar gas is the second most important source of heliospheric ions. Atomic abundances in the local interstellar gas are derived from ion composition measurements, and processes in the solar wind termination region and beyond are studied. Title: Diffusive fractionation in the chromosphere Authors: von Steiger, R.; Marsch, E. Bibcode: 1994SSRv...70..341V Altcode: A new mechanism for the FIP fractionation in the solar wind in the form of a stationary diffusion model is proposed. It is based on a weakly stratified chromospheric layer of constant density and temperature, permeated everywhere by ionizing photons and a homogeneous magnetic field. Our model does not invoke any particular geometry or special set up of the system and is founded solely on robust and well understood atomic collisonal physics. Technically, a boundary value problem of four coupled differential equations is solved for each chemical element, i.e. a continuity equation and a momentum equation for both atoms and singly ionized particles. For the main gas (hydrogen), an analytical solution can be found. This then serves as a background for the numerical integration of each trace gas system (several elements from He to Fe). We find that, after a few hydrogen diffusion lengths, each minor species asymptotically approaches a constant density. The ratios of these density values to some reference element reproduce the observed FIP fractionation pattern remarkably well. Title: Acceleration of interstellar pickup ions in the disturbed solar wind observed on Ulysses Authors: Gloeckler, G.; Geiss, J.; Roelof, E. C.; Fisk, L. A.; Ipavich, F. M.; Ogilvie, K. W.; Lanzerotti, L. J.; von Steiger, R.; Wilken, B. Bibcode: 1994JGR....9917637G Altcode: Acceleration of interstellar pickup H+ and He+ as well as of solar wind protons and alpha particles has been observed on Ulysses during the passage of a corotating interaction region (CIR) at ~4.5 AU. Injection efficiencies for both the high thermal speed interstellar pickup ions (H+ and He+) and the low thermal speed solar wind ions (H+ and He++) are derived using velocity distribution functions of protons, pickup He+ and alpha particles from <1 to 60 keV/e and of ions (principally protons) above ~60 keV. The observed spatial variations of the few keV and the few hundred keV accelerated pickup protons across the forward shock of the CIR indicate a two stage acceleration mechanism. Thermal ions are first accelerated to speeds of 3 to 4 times the solar wind speed inside the CIR, presumably by some statistical mechanism, before reaching higher energies by a shock acceleration process. Our results also indicate that (1) the injection efficiencies for pickup ions are almost 100 times higher than they are for solar wind ions, (2) pickup H+ and He+ are the two most abundant suprathermal ion species and they carry a large fraction of the particle thermal pressure, (3) the injection efficiency is highest for protons, lowest for He+, and intermediate for alpha particles, (4) both H+ and He+ have identical spectral shapes above the cutoff speed for pickup ions, and (5) the solar wind frame velocity distribution function of protons has the form F(w)=FOw-4 for 1<w<~5, where w is the ion speed divided by the solar wind speed. Above w~5-10 the proton spectrum becomes steeper. These results have important implications concerning acceleration of ions by shocks and CIRs, acceleration of anomalous cosmic rays, and particle dynamics in the outer heliosphere. Title: Interstellar oxygen, nitrogen and neon in the heliosphere Authors: Geiss, J.; Gloeckler, G.; Mall, U.; von Steiger, R.; Galvin, A. B.; Ogilvie, K. W. Bibcode: 1994A&A...282..924G Altcode: Oxygen, nitrogen and neon pick-up ions of interstellar origin were detected for the first time with the Solar Wind Ion Spectrometer (SWICS) on board Ulysses. The interstellar origin of these ions is established by the following criteria: (a) they are singly charged, (b) they have the broad velocity distributions characteristic of pick-up ions, with an upper limit of twice the solar wind speed, (c) their relative abundance as a function of distance from the sun corresponds to the theoretical expectation, and (d) there is no relation to a planetary or cometary source. The interstellar abundance ratios He(+)/O(+), N(+)/O(+), Ne(+)/O(+) were investigated. At approximately 5.25 AU in the outermost part of Ulysses' trajectory He(+)/O(+) = 175+70-50 N(+)/O(+) = 0.13+0.05-0.05 and Ne(+)/O(+) = 0.18+0.10-0.07 were determined. For the interstellar gas passing through the termination region and entering the heliosphere (He/O)0 = 290+190-100, (N/O)0 = 0.13+0.06-0.06 and (Ne/O)0 = 0.20+0.12-0.09 were obtained from the pick-up ion measurements. Upper limits for the relative abundances of C(+) and C were also determined.