ExoMars Trace Gas Orbiter (TGO) Science Ground Segment (SGS)

The ExoMars Trace Gas Orbiter (TGO) Science Ground Segment (SGS), comprised of payload Instrument Team, ESA and Russian operational centres, is responsible for planning the science operations of the TGO mission and for the generation and archiving of the scientific data products to levels meeting the scientific aims and criteria specified by the ESA Project Scientist as advised by the Science Working Team (SWT). The ExoMars SGS builds extensively upon tools and experience acquired through earlier ESA planetary missions like Mars and Venus Express, and Rosetta, but also is breaking ground in various respects toward the science operations of future missions like BepiColombo or JUICE. A productive interaction with the Russian partners in the mission facilitates broad and effective collaboration. This paper describes the global organisation and operation of the SGS, with reference to its principal systems, interfaces and operational processes.     

Psychological, psychiatric, and interpersonal aspects of long-duration space missions

America's future in space calls for manned missions that are of long duration and increasing complexity. Under these conditions, psychological and interpersonal stressors will take on added importance in affecting the safely of the crew and the outcome of the mission. Through an analysis of reports from manned American and Soviet space missions and Earth-bound simulations, several psychological, psychiatric, and interpersonal issues can be identified that could affect the success of the space station and other long-duration space ventures. Psychological issues include sleep problems, alteration in time sense, demographic effects, career motivation, transcendent experiences, homesickness, and alteration in perceptual sensitivities. Psychiatric issues include anxiety, depression, and psychosis, psychosomatic symptoms, emotional problems related to the stage of the mission, and postflight personality changes. Interpersonal issues include interpersonal tension, decreased cohesiveness over time, need for privacy, and task vs emotional leadership. Steps can be taken to minimize the impact of these issues, both before and during the mission.     

Psychological health maintenance on Space Station Freedom

The scheduling of crew rotations for up to 180 days on Space Station Freedom presents a special challenge for behavioral scientists who are tasked with providing psychological support for the crews, their families, and mission flight controllers. Preflight psychological support planning may minimize the negative impact of psychological and social issues on mission success, as well as assist NASA management in making real-time mission planning decisions in the event of a significant social event (for example, the death of a family member). During flight, the combined psychological, emotional, and social stressors on the astronauts must be monitored, along with other aspects of their health. The Health Maintenance Facility (HMF) will have the capability of providing preventive, diagnostic, and therapeutic assistance for significant psychiatric and interpersonal problems which may develop. Psychological support will not end with the termination of the mission. Mental health professionals must be part of the team of medical personnel whose job will be to facilitate the transition--physical and mental--from the space environment back to planet Earth. This paper reviews each phase of mission planning for Space Station Freedom and specifies those factors that may be critical for psychological health maintenance on extended-duration space missions.     

Conversations. With Norman Thagard [interview by Johan Benson

This article is an interview with U.S. astronaut Norman Thagard. He was on the Russian Mir 18 mission. Launched to the space station from Baikonur on March 14, 1995, he returned to Earth on the Shuttle 115 days later. With the completion of that mission, Thagard holds the U.S. record for the most time spent in space. Topics of discussion during the interview include: the cultural isolation faced by an American astronaut on a Russian space facility; the physiological and psychological effects of long-duration space flight; the problems of loss of bone and the radiation environment; readaptation to gravity on Earth; and, recommendations to the designers of the Alpha station.     

US, Russian suits serve diverse EVA goals

U.S. astronauts and Russian cosmonauts both use space suits when performing extravehicular activity (EVA), but these have been developed independently due to the diverse goals of each country's space program. The current versions of the U.S. and Russian space suits were compared when the author tested both suits on the same day. The similarities and differences are noted, as well as the strengths and limitations of each. Determination of the compatibility of these suits is important as increased cooperation between the U.S. and Russia has occurred (for example, astronauts and cosmonauts are flying together on Shuttle/Mir missions) and as the international space station becomes reality.     

Comments on the Communication and Data Problems Associated with a Mars Trip During a Conjunction Phase

The analysis and comments presented in this paper are meant to establish the general communication parameters associated with Martian flyby probes and with lander and manned vehicles. Fundamental data transfer problems are reviewed to define comparisons and trends of tradeoffs for future studies. Selected focal points are based upon the long propagation path length, with inherent time delays, and the high noise produced by the sun. These problems are magnified because large quantities of data must be obtained to satisfy the needs of the scientific community and the curiosity of an interested public. A comparison of two communication systems is provided: the microwave spectrum and the optical spectrum, as represented by the microwaves at 2.3 GHz and the laser at 6328 ?. A method of cost effectiveness or value received from space missions (a criterion of power input for data quantity received) is also presented.     

The design of a nuclear power supply with a 50 year lifeexpectancy: the JPL Voyager's SiGe MHW RTG

Between 25 and 30 years ago, the IECEC Proceedings carried a series of papers by the present authors and other members of a JPL team on the problems and the desirable design features associated with the MHW RTGs to be used to power JPL's Voyager I and II spacecraft. The Voyager I and II spacecraft successfully completed their original 12 year missions 10 years ago and are at distances of over 55 AU and 70 AU from the sun. The power systems worked almost precisely as predicted. The Voyager spacecraft seem to have several decades of life left to make measurements outside the solar system. This paper gives a technical overview of the design process and problems     

Chemical Composition of Icy Satellite Surfaces

Much of our knowledge of planetary surface composition is derived from remote sensing over the ultraviolet through infrared wavelength ranges. Telescopic observations and, in the past few decades, spacecraft mission observations have led to the discovery of many surface materials, from rock-forming minerals to water ice to exotic volatiles and organic compounds. Identifying surface materials and mapping their distributions allows us to constrain interior processes such as cryovolcanism and aqueous geochemistry. The recent progress in understanding of icy satellite surface composition has been aided by the evolving capabilities of spacecraft missions, advances in detector technology, and laboratory studies of candidate surface compounds. Pioneers 10 and 11, Voyagers I and II, Galileo, Cassini and the New Horizons mission have all made significant contributions. Dalton (Space Sci. Rev., 2010, this issue) summarizes the major constituents found or inferred to exist on the surfaces of the icy satellites (cf. Table 1 from Dalton, Space Sci. Rev., 2010, this issue), and the spectral coverage and resolution of many of the spacecraft instruments that have revolutionized our understanding (cf. Table 2 from Dalton, Space Sci. Rev., 2010, this issue). While much has been gained from these missions, telescopic observations also continue to provide important constraints on surface compositions, especially for those bodies that have not yet been visited by spacecraft, such as Kuiper Belt Objects (KBOs), trans-Neptunian Objects (TNOs), Centaurs, the classical planet Pluto and its moon, Charon. In this chapter, we will discuss the major satellites of the outer solar system, the materials believed to make up their surfaces, and the history of some of these discoveries. Formation scenarios and subsequent evolution will be described, with particular attention to the processes that drive surface chemistry and exchange with interiors. Major similarities and differences between the satellites are discussed, with an eye toward elucidating processes operating throughout the outer solar system. Finally we discuss the outermost satellites and other bodies, and summarize knowledge of their composition. Much of this review is likely to change in the near future with ongoing and planned outer planet missions, adding to the sense of excitement and discovery associated with our exploration of our planetary neighborhood.     

Lunar orbital science

Summary Orbital science has, to the present, concentrated on studies of force fields, particles, and visible photography. Cameras have been the major scientific instrument (it could be debated that for geodesy and gravity the entire spacecraft represents an instrument), and geology has been the principle benefactor. Photography has also been essential for the manned landing program, which would not have been possible on the schedule followed without the detailed Lunar Orbiter pictures.Orbital tracking data indicates that the Moon is almost homogeneous with perhaps a slight increase in density with depth. Significant analysis of the higher gravity harmonics have identified localized, near surface gravity highs that appear to be associated with circular maria. The Moon does not have a significant magnetic field of its own, and the solar wind appears to impinge directly on the surface. Russian and United States evidence on micrometeorite fluxes near the Moon is conflicting, but probably there is a decrease in flux compared to that near the Earth.Photographic evidence indicates that both impact and volcanic action has shaped the lunar surface. Mass movements of surface material and surface erosional effects are clearly evident. Surface water in the past, or near surface permafrost now, are definite possibilities to explain the sinuous rills. Faulting, both regional and local, is evident, as is probably horizontal layering near the surface.The United States space program is embarking on a broad program of orbital science including nearly the entire spectra of remote sensing. Approved orbital missions extend through 1972 and will be carried out in conjunction with manned landings. Emphasis will be placed on determining the extent and degree of surface variations between and within lunar provinces and the nature and strength of the lunar spectrum. Information obtained from the surface missions and the returned lunar samples will be invaluable in helping us to design orbital instruments and interpret the results.Missions after 1972 undoubtedly will carry more sophisticated instruments that will give us definitive information on the geochemical nature of the lunar surface and interior.Copies of NASA-issued documents may be obtained by writing to the Superintendent of Documents, U.S. Government Printing Office, Washington, D.C. 20402. Information about, and data from, U.S. space missions, including photographs, can be obtained from the National Space Science Data Center, Code 601, Goddard Space Flight Center, Greenbelt, Maryland 20771.     

Past,Present and Future of Active Radio Frequency Experiments in Space

Active ionospheric experiments using high-power, high-frequency transmitters, “heaters”, to study plasma processes in the ionosphere and magnetosphere continue to provide new insights into understanding plasma and geophysical proceses. This review describes the heating facilities, past and present, and discusses scientific results from these facilities and associated space missions. Phenomena that have been observed with these facilities are reviewed along with theoretical explanations that have been proposed or are commonly accepted. Gaps or uncertainties in understanding of heating-initiated phenomena are discussed together with proposed science questions to be addressed in the future. Suggestions for improvements and additions to existing facilities are presented including important satellite missions which are necessary to answer the outstanding questions in this field.     

载人火星探测进展及其EDL过程GNC关键技术

随着火星探测技术的不断发展和探测任务的不断推进，载人火星探测在未来将会成为火星探测的重要手段。首先，回顾了无人火星探测任务的发展历程，对比分析了部分无人火星探测器进入、下降与着陆（EDL）过程的参数。然后，结合无人火星探测、载人月球探测和载人航天再入过程，梳理了载人火星探测的特点及需求，系统地总结了前苏联/俄罗斯和美国的载人火星探测研究进展以及技术储备。接着，归纳了载人火星探测的体系构成、集结方式和主要的技术挑战。最后，概括了载人火星EDL过程面临的难题，重点阐述了EDL的导航、制导与控制（GNC）关键技术。     

Geodetic Methods for Calibration of GRACE and GOCE

It is beyond doubt that calibration and validation are essential tools in the process of reaching the goals of gravity missions like GRACE and GOCE and to obtain results of the highest possible quality. Both tools, although general and obvious instruments for any mission, have specific features for gravity missions. Therefore, it is necessary to define exactly what is expected (and what cannot be expected) from calibration and what from validation and how these tools should work in our case. The general calibration and validation schemes for GRACE and GOCE are outlined. Calibration will be linked directly to the instrument and the measurements whereas validation will be linked to data derived from the original measurements. Calibration includes on-ground, internal, and external calibration as well as error assessment. The calibration phase results in corrected measurements along with an a posteriori error model. Validation of e.g. calibrated measurements or geoid heights means checking against independent data to assess whether there are no systematic errors left and/or whether the error model describes the true error reasonably well. Geodetic methods for calibration typically refer to external calibration and error assessment, and will be illustrated with an example. This revised version was published online in August 2006 with corrections to the Cover Date.     

Hard X-Ray/Soft Gamma-Ray Experiments and Missions: Overview and Prospects

Starting from 1960s, a great number of missions and experiments have been performed for the study of the high-energy sky. This review gives a wide vision of the most important space missions and balloon experiments that have operated in the 10–600 keV band, a crucial window for the study of the most energetic and violent phenomena in the Universe. Thus it is important to take the stock of the achievements to better establish what we have still to do with future missions in order to progress in this field, to establish which are the technologies required to solve the still open issues and to extend our knowledge of the Universe.     

A Digital Map Set for the Night Attack Aircraft

There has been much interest recently in applying cartographic digital data bases to advanced avionics systems as a solution to specific problems associated with night attack aircraft missions. The tremendous computer horsepower required to accomplish this task in real-time in an airborne environment is well documented. Hardware implementation of complex algorithms traditionally has produced custom devices which accomplish a specific function on a specific data structure. Historically, this has resulted in powerful but inflexible systems incapable of adapting to the changing requirements of military missions. In an age of evolving technology, these pitfalls must be avoided by incorporating expected changes into the design of digital map systems. If they are made to accommodate a variety of cartographic data bases and allow for programmable manipulation of those bases, this new class of digital map sets can be reconfigured at the software level to meet the changing requirements of aircraft missions. This paper addresses current design concepts for such a map system on a Night Attack aircraft. The focus is on issues concerning the development and handling of existing map data products to meet current system requirements. This system, called the Digital Map Set (DMS), is being designed to accomplish the classical manipulations of Defense Mapping Agency Digital Land Mass System data. Additionally, aeronautical charts, aerial reconnaissance photos, flight plan data, and other two-dimensional bit mapped graphics also are accommodated. Mission requirements relating to the cartographic data bases shall be discussed along with ground support station and airborne system design issues.     

Orbits for radiatively cooled space telescopes

This paper first outlines the assumed mission requirements for a radiatively cooled space telescope such as EDISON. A summary of relevant characteristics (payload, operating orbit, launcher, lifetime, etc.) for current and proposed cooled telescope missions is then given. This summary includes cryogenic and radiatively cooled missions since in both cases the reduction of heat input to the telescope aperture is a dominant factor in the orbit choice. These missions span the entire range of possibilities from low earth circular, through higher elliptical and circular orbits out to deep space locations such as the Sun-Earth (S-E) libration points and the lunar surface.A full listing of the factors affecting mission selection is then given. The most important points are illustrated by reference to the orbits chosen for ISO, FIRST and SIRTF and those recommended in recent studies of EDISON. Launcher capabilities for direct insertion and the onboard propellant for large velocity changes associated with orbit raising are major constraints in achieving the large payload mass to high orbit which EDISON mission requires. Although it is fairly demanding in launch/boost energy, an orbit about the L2 S-E libration point offers important advantages for a radiatively cooled infrared telescope. Further studies of this orbit and the associated aspects of service module and payload design for the L2 location of EDISON are recommended.     

The geologic development of Mars: A review

The planet Mars has been the subject of a continuing program of exploration with the flyby missions of 1964 and 1969, the orbiter of 1971, and the present Viking Project with both orbiters and landers. The overall view of Mars has changed from Earthlike in the prespacecraft era to Moonlike following the flyby missions and finally to a planet with intermediate characteristics. There are many impact craters as on the Moon, but tectonic and volcanic features resembling structures on Earth are also present. However, there is a lack of evidence for the compressional deformation associated with terrestrial plate tectonics and continental drift.The current analyses indicate that Mars has a differentiated interior with a crust and mantle and perhaps a core. Whatever the nature of interior processes, whether overall mantle expansion, plumes, or full scale convection, the effects at the surface have been predominantly vertical with formation of broad regions of uplift and depression. One of the results is hemispheric asymmetry with cratered terrain in the south and younger uncratered plains in the north.     

Kelvin–Helmholtz Instability: Lessons Learned and Ways Forward

The Kelvin–Helmholtz instability (KHI) is a ubiquitous phenomenon across the Universe, observed from 500 m deep in the oceans on Earth to the Orion molecular cloud. Over the past two decades, several space missions have enabled a leap forward in our understanding of this phenomenon at the Earth’s magnetopause. Key results obtained by these missions are first presented, with a special emphasis on Cluster and THEMIS. In particular, as an ideal instability, the KHI was not expected to produce mass transport. Simulations, later confirmed by spacecraft observations, indicate that plasma transport in Kelvin–Helmholtz (KH) vortices can arise during non-linear stage of its development via secondary process. In addition to plasma transport, spacecraft observations have revealed that KHI can also lead to significant ion heating due to enhanced ion-scale wave activity driven by the KHI. Finally, we describe what are the upcoming observational opportunities in 2018–2020, thanks to a unique constellation of multi-spacecraft missions including: MMS, Cluster, THEMIS, Van Allen Probes and Swarm.     

Future Space Missions to Search for Terrestrial Planets

Since the first exoplanet was discovered more than 10 years ago, this field has developed rapidly. Currently we know of more than 200 external systems of stars and planets, apart from our own, but what has become the ‘holy grail’ of exoplanetary research is still eluding us. Here we are, of course, referring to solar systems like our own, containing a number of terrestrial or ‘rocky’ planets orbiting within the so-called ‘habitable zone’, and with giant planets such as Jupiter and Saturn—which mostly or totally consist of elements as H or He—at distance much further out from the central star. No such system have to date been discovered around anything resembling our Sun, albeit because of observational biases. Nevertheless, in order to develop the emerging science discipline of Comparative Planetology, we will have to utilize new techniques that will enable us to search for, and then study in detail such systems in an un-biased fashion. This paper describes the emerging techniques and space missions that will allow, finally, the investigation of planets capable of hosting life as we know it.     

Dynamo Models for Planets Other Than Earth

Observations from planetary spacecraft missions have demonstrated a spectrum of dynamo behaviour in planets. From currently active dynamos, to remanent crustal fields from past dynamo action, to no observed magnetization, the planets and moons in our solar system offer magnetic clues to their interior structure and evolution. Here we review numerical dynamo simulations for planets other than Earth. For the terrestrial planets and satellites, we discuss specific magnetic field oddities that dynamo models attempt to explain. For the giant planets, we discuss both non-magnetic and magnetic convection models and their ability to reproduce observations of surface zonal flows and magnetic field morphology. Future improvements to numerical models and new missions to collect planetary magnetic data will continue to improve our understanding of the magnetic field generation process inside planets.     

Outer Plasmaspheric Plasma Properties: What We Know from Satellite Data

Our understanding of the composition, density, and temperature structure of the outer plasmasphere has undergone several major revisions since the discovery of the plasmasphere over 35 years ago. Each new era of understanding was brought about by the launching of satellites carrying suites of plasma diagnostic experiments each more sophisticated than its predecessor. Instead of each new generation of missions providing incremental advancement in our knowledge of the plasmasphere's plasma properties, they most often than not, initiated a complete re-thinking of our understanding. There are still a number of observational "puzzles" and large gaps in our knowledge of how plasmaspheric structure and plasma properties change with geomagnetic storm and substorm activity. As we develop new missions to attempt to globally image the outer plasmasphere in order to put simultaneous multi-spacecraft observations into context, we undoubtedly will uncover new tantalizing observations that will cause us to re-think our mental picture of the plasmasphere. What we have learned from satellite data about the chemical composition, density, temperature and pitch-angle distribution properties and their variability is outlined in this review paper.