ESA Science & Technology - Publication Archive

A paper originally presented by EADS Astrium at the 54th IAC in Bremen in September 2003.

On 28 January 2003, EADS Astrium officially signed the Venus Express contract with the European Space Agency (ESA) worth 82.4 million Euros for the design and development of the spacecraft. This will be the first European spacecraft to visit the planet Venus. Venus Express is scheduled for launch from the Baikonour Cosmodrome in Kazakhstan in November 2005. It will be launched by a Soyuz-Fregat rocket and put immediately into its transfer orbit to Venus.

Gaia in 2003, a status report prepared by the Gaia Project Scientist, summarises the status of the Gaia project at the end of 2003, describes the progress achieved in 2003, and summarises the major ongoing and planned activities.

Abstract
Since ten years ASTRIUM has developed sintered Silicon Carbide (SiC) technology for space applications. Its unique thermo-mechanical properties, associated with its polishing capability, make SiC an ideal material for building ultra-stable lightweight space based telescopes or mirrors. SiC is a cost effective alternative to Beryllium and the ultra-lighweighted ULE. In complement to the material manufacturing process, ASTRIUM has developed several assembly techniques (bolting, brazing, bonding) for manufacturing large and complex SiC assemblies. This technology is now perfectly mature and mastered. SiC is baselined for most of the telescopes that are developed by ASTRIUM. SiC has been identified as the most suitable material for manufacturing very large crygenic telescopes. In this paper we present the development of a 3.5m-diameter telescope for the Herschel Mission. Herschel's main goal is to study how the first stars and galaxies were formed and evolved. The Herschel Space telescope, using silicon carbide technology will be the largest space imagery telescope ever launched. The Herschel telescope will weight 300 kg rather than the 1.5 tons required with standard technology. The Herschel telescope is to be delivered in 2005 for a launch planned for 2007.

Four transits of the planet orbiting the star HD209458 were observed with the STIS spectrograph on board HST. The wavelength domain (1180-1710A) includes HI as well as CI, CII, CIV, NV, OI, SI, SiII, SiIII and SiIV lines. During the transits, absorptions are detected in HI, OI and CII (5+/-2%, 13+/-4.5% and 7.5+/-3.5%, respectively). No absorptions are detected for other lines. The 5% mean absorption over the whole HI Lyman alpha line is consistent with the previous detection at higher resolution (Vidal-Madjar et al. 2003). The absorption depths in OI and CII show that oxygen and carbon are present in the extended upper atmosphere of HD209458b. These species must be carried out up to the Roche lobe and beyond, most likely in a state of hydrodynamic escape.

We investigate intense whistler-mode chorus emissions which occurred during the geomagnetic storm on 31 March 2001. We use multipoint measurements obtained by the Cluster spacecraft in the premidnight equatorial region outside the plasmasphere at a radial distance of 4 Earth radii (L = 4.0 - 4.2). Observed spatio-temporal variations of the direction of the Poynting flux manifest a consistent pattern: the central position of the chorus source fluctuates at time scales of minutes within 1000-2000 km of the geomagnetic equator. We demonstrate that estimates of the electromagnetic planarity can be used to characterize the extent of the source, obtaining a range of 3000-5000 km. Discrete wave packets of chorus are observed to rise in frequency between 0.13 and 0.5 of the local electron cyclotron frequency, at a rate up to 20 kHz/s, having the maximum peak amplitudes of <20 mV/m. We observe a fine structure of subpackets with large amplitudes embedded in the interior of the wave packets. This fine structure has a typical delay of a few milliseconds between the two neighboring maxima of the wave amplitude. Longer delays occur with a decreasing probability density.

Mariner 10 has been the only spacecraft to visit the innermost planet Mercury. Its three flybys, more than 25 years ago, yielded the first view of this little-understood world. With advances in spacecraft technology and a growing realization of how important Mercury is to our understanding of the solar system and its formation, two missions are now in development for more intensive Mercury exploration. The first is the MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) mission, competitively selected under the NASA Discovery Program, that will send a spacecraft to fly by Mercury in 2007 and 2008 and to orbit Mercury for one Earth year beginning in April 2009. The second is the more comprehensive BepiColombo mission, consisting of three elements: the Mercury Planetary Orbiter (MPO), the Mercury Magnetospheric Orbiter (MMO), and the Mercury Surface Element (MSE). Still in final definition stage, BepiColombo is a partnership between the European Space Agency (ESA) and the Japanese Institute of Space and Astronautical Science (ISAS). With one or two launches (depending upon the final mission architecture) BepiColombo will use solar electric propulsion to send two orbiters (MPO from ESA and MMO from ISAS) and a lander (MSE) to Mercury as early as 2011. The BepiColombo orbiters, in orbits complementary to that of MESSENGER, will extend geochemical, spectral, and photometric mapping of the planet. With its factor-of-ten larger downlink, BepiColombo will complete the intensive study of Mercury begun with the exploration by MESSENGER. Synergistic strategies of exploration will enable efficient use of BepiColombo resources in a more detailed study of the planet than can be accomplished by MESSENGER alone. - Remainder of abstract is truncated -

The superconducting differential accelerometers both for the Equivalence Principle experiment and geodesy within the European STEP mission have common design principles. The test masses are suspended by stable superconducting magnetic levitation. The suspension design makes all the degrees of freedom of the masses stiff, except for the axial differential mode which is made compliant in order to obtain a high intrinsic sensitivity of the differential accelerometer, < 10^-14m s^-2Hz^-1/2. Trimming of persistent currents circulating in the levitation system allows to achieve rejection ratios for the unwanted common and radial accelerations > 10⁶. Two separate superconducting circuits couple the axial displacements of the test masses to two SQUIDs. Persistent currents are stored in the two circuits such that one SQUID is only coupled to the differential displacement while the other only senses the common one. By differencing the signal before its detection, one highly reduces the dynamic range needs of the SQUIDs, of the following amplifiers and of the final A/D converters.

Few facts in science are more surprising and none has had a longer history than the apparent equivalence of the two kinds of mass in physics, gravitational and inertial. From Galileo and Newton to Eötvös and Einstein, it has been a compelling issue both theoretically and experimentally. Ground-based tests have now a precision of about 1 part in 10¹². Even with this extraordinary agreement, there are profound theoretical reasons for carrying the measurements further. Our generation has the unique oppurtunity to make an advance of a factor of a million in testing the Equivalence Principle in space.

A special ESA publication to coincide with the 1st annivsary of the launch of the INTEGRAL spacecraft. Contribution were made by various members of the entire mission and project teams to give a unique account of a year in the life of a spacecraft.

Electric and magnetic field observations on the Polar satellite at the subsolar magnetopause show that the magnetopause current is often striated. The largest of the resulting current channels are interpreted as electron diffusion regions because their widths are several electron skin depths and the electron flow U_e within them does not satisfy E + U_e x B = 0. The data suggest that the magnetopause contains many such electron diffusion regions and that they are required because E x B/B² drifting electrons cannot carry the large filamentary currents imposed on the local plasma. The most probable interpretation of E + U_e x B is not equal to 0 is that the pressure term on the right side of the generalized Ohm's law balances this inequality.

In November 1993, the International Rosetta Mission was approved as a Cornerstone Mission in ESA's Horizons 2000 Science Programme. Since then, scientists and engineers from all over Europe and the United States have been combining their talents to build an orbiter and a lander for this unique expedition to unravel the secrets of a mysterious mini ice world – a comet.

Table of contents:

• Rosetta: Europe's comet chaser
• Why 'Rosetta'
• Life and survival in deep space
• The cosmic billiard ball
• The long trek
• Rendezvous with a comet
• Debris of the Solar System: asteroids
• Debris of the Solar System: Comet 67P/Churyumov-Gerasimenko
• The Rosetta orbiter
• Science from the orbiter
• The Rosetta lander
• Long-distance communication
• Rosetta overview

Note: a more recent Rosetta mission brochure (ESA BR-321) is available here.

We report the detection with the BeppoSAX Wide Field Cameras of a superburst from 4U 1254-69. The superburst is preceded by a normal type-I X-ray burst, has a decay time that is the longest of all eight superbursts detected so far and a peak luminosity that is the lowest. Like for the other seven superbursts, the origin is a well-known type-I X-ray burster with a persistent luminosity level close to one tenth of the Eddington limit. Based on WFC data of all persistently bright X-ray bursters, the average rate of superbursts is 0.51 +/- 0.25 per year per persistently bright X-ray burster. Some systems may have higher superburst rates. For all superbursters, we present evidence for a pure helium layer which is burnt in an unstable as well as a stable manner.

We describe the "Monitor e Imageador de Raios-X" (MIRAX), an X-ray astronomy satellite mission proposed by the high-energy astrophysics group at the National Institute for Space Research (INPE) in Brazil to the Brazilian Space Agency. MIRAX is an international collaboration that includes, besides INPE, the University of California San Diego, the University of Tubingen in Germany, the Massachusetts Institute of Technology and the Space Research Organization Netherlands.

The ESA Annual Report 2002 contains a summary of all the activities undertaken by ESA during 2002.

This Special Letters Issue features the INTEGRAL observatory. About one year after its successful launch, this series of 75 publications describe the mission, the various instruments and their performance, as well as first scientific results from the spacecraft, ranging from gamma-ray bursts to Galactic sources.

Several important INTEGRAL events took place during the last two months.

We celebrated the first launch anniversary, on 17 October, with the spacecraft in excellent shape. Unfortunately, recent high solar activity substantially interrupted the observing programme, for the first time.

Although the research of cosmic rays began nearly 100 years ago much is still unknown especially with regard to their origins and the mechanisms providing the particles nearly the speed of light. That is why the cosmic ray research continues to be one of the most fascinating adventures of modern space science. This article is based on publications of the International Space Science Institute on cosmic rays, which are strongly recommended for further reading.

The Lynx arc, with a redshift of 3.357, was discovered during spectroscopic follow-up of the z=0.570 cluster RX J0848+4456 from the ROSAT Deep Cluster Survey. The arc is characterized by a very red R-K color and strong, narrow emission lines. Analysis of HST WFPC2 imaging and Keck optical and infrared spectroscopy shows that the arc is an H II galaxy magnified by a factor of ~10 by a complex cluster environment. The high intrinsic luminosity, the emission-line spectrum, the absorption components seen in Lyalpha and C IV, and the rest-frame ultraviolet continuum are all consistent with a simple H II region model containing ~10⁶ hot O stars. The best-fit parameters for this model imply a very hot ionizing continuum (T_BB~= 80 000 K), a high ionization parameter (logU~=-1), and a low nebular metallicity (Z/Z_solar~=0.05). The narrowness of the emission lines requires a low mass-to-light ratio for the ionizing stars, suggestive of an extremely low metallicity stellar cluster. The apparent overabundance of silicon in the nebula could indicate enrichment by past pair-instability supernovae, requiring stars more massive than ~140 M_solar.

Presentation given during the 5th IAA International Conference on Low Cost Planetary Missions on 24th September 2003 by Bernard Foing