Heating of Pickup and Solar Wind Ions at Jupiter’s Bow Shock

Interstellar pickup ions are dynamically important in the outer heliosphere where they mass‐load and heat the solar wind. Some of these pickup ions are transformed into energetic neutral atoms (ENAs) by charge exchange with the residual cold interstellar gas that is the primary constituent of the outer heliosphere. The most detailed measurements of interstellar pickup ions in the heliosphere are currently available only between ∼1 and ∼5 AU. Among the most interesting and least expected observations are those of ubiquitous suprathermal tails on the distribution of pickup and solar wind protons and all heavier ions that can be measured. Here we report new measurements of solar wind proton and alpha particle distributions and of pickup He+ spectra upstream and downstream of Jupiter’s bow shock. We find that in the magnetosheath, 27% of the total pickup H+ density is in the tail portion of the distribution, compared to only 0.4% in the upstream spectrum. For He+ the entire core distribution is apparently heated in crossing the shock. These results have important implications for particle acceleration at the heliospheric termination shock, and for predicting the fluxes of energetic neutral atoms in the inner heliosphere produced from solar wind and pickup ions heated and accelerated at the termination shock. © 2004 American Institute of PhysicsPeer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87300/2/201_1.pd

Ubiquitous statistical acceleration in the solar wind

One of the more interesting observations by ACE is the ubiquitous presence of higher energy tails on the distribution functions of solar wind and pickup ions. The tails occur continuously in the slow solar wind, but less so in fast wind. Their presence is not correlated with the passage of shock waves. It is pointed out that statistical acceleration by transit-time damping of propagating magnitude fluctuations in the magnetic field of the solar wind is a likely mechanism to yield the observed tails. © 2000 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87342/2/229_1.pd

Sources, injection and acceleration of heliospheric ion populations

A variety of heliospheric ion populations—from Anomalous Cosmic Rays (ACRs) to particles accelerated in Corotating Interaction Regions (CIRs)—have been observed and studied for several decades. It had been commonly assumed that the solar wind was the source for all of these populations, except for the ACRs, and that shock acceleration produced the energetic particles observed, including the ACRs. For the ACRs the source that had been proposed a long time ago was the interstellar gas that penetrates deep into the heliosphere. Recent measurements of the composition and spectra of suprathermal ions, primarily from Ulysses, ACE and Wind, indicate that pickup ions are likely to be an important source not only of the ACRs but for other heliospheric ion populations as well. In particular, the newly discovered “Inner Source” pickup ions may be a significant source for particles accelerated in the inner heliosphere and may also be the seed material for ACR C, Mg, Si and Fe. Furthermore, the omnipresent suprathermal tails seem to tell us that shock acceleration may not be the primary mechanism energizing particles to ∼0.1 MeV in the heliosphere. Explaining the origin of these persistent high velocity tails remains one of our challenges. © 2000 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87341/2/221_1.pd

Observations of non-thermal properties of heavy ions in the solar wind

Heavy ions in the solar wind are ideal for studying injection processes in the solar wind. We use composition data from Ulysses, ACE, and Wind to examine the properties of heavy ions from thermal energies to several 100 keVs. We show that these particles are observed to gain energy without any association with shocks. This paper provides a survey of recent observations of non-thermal properties of solar wind heavy ions which are consistent with the following picture: At thermal energies coherent wave-particle interactions preferentially heat and accelerate heavy ions with collisional processes limiting subsequent non-thermal properties. At higher energies heavy ion distribution functions are characterized by ubiquitous suprathermal tails. We argue that solar wind heavy ions are a good tracer for acceleration processes which are not directly associated with shocks. These stochastic processes are observed to be relevant for predisposing ions for shock acceleration. © 2000 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87338/2/215_1.pd

Rehabilitation for improving automobile driving after stroke (Protocol)

THIS IS NOT THE MOST RECENT VERSION OF THIS PROTOCOL please see: http://hdl.handle.net/2328/27805 Copyright © 2010 The Cochrane Collaboration. Published by John Wiley & Sons, Ltd. This review is made available in accordance with Cochrane Database of Systematic Review's repositories policyThis is a protocol for a Cochrane Review (Intervention). The objectives are as follows: This review aims to determine whether any intervention, with the specific aim of maximising driving skills or with an outcome of assessed driving skills, improves the driving performance for patients following stroke

The inner source for pickup ions

Pickup ions are observed by the Solar Wind Ion Composition Spectrometer on Ulysses which appear to have been picked up close to the Sun. A transport theory for the propagation of these ions is used to constrain the spatial profiles of the ion sources. The composition is like that of the solar wind which suggests that the inner source pickup ions result from solar wind particles that are embedded in dust grains and then released. Through comparison between modeled and observed distributions, it is possible to constrain the radial and latitudinal profiles of the inner source. Inner source protons are also observed and may constitute an energetically important population in the solar wind. © 1999 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87724/2/487_1.pd

Engaging Small and Medium-Sized Enterprises in Responsible Innovation

A significant part of responsible innovation is engagement with diverse groups of stakeholders; this remains true for projects investigating responsible innovation practices. This chapter discusses strategies for engaging small and medium-sized enterprises (SMEs) in co-creating visions of and plans for implementing responsible innovation, drawing on the example of engagement with United Kingdom cyber security companies. The key aspect of the engagement was building trust between the responsible innovation researchers and the companies. Trust was built by a movement away from traditional recruitment procedures for research projects, towards proactive engagement with the culture and traditions of the sector – participating in company sponsored talks and conferences, finding ways to communicate effectively, and ensuring a tailored message that fit the expectations and requirements of the sector. This chapter reviews the context in which the recruitment took place, the assumptions made prior to recruitment, the approaches taken, the revisions made to these approaches, and ultimately offers some general recommendations for industry engagement in responsible innovation activities

Protease Activity in Adult Aedes Aegypti Mosquitoes as Related to Feeding

Author Institution: Department of Zoology and Entomology, The Ohio State University, Columbus 1

Composition variations in fast solar wind streams

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. © 1999 American Institute of Physics.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87727/2/143_1.pd