Planetary atmosphere observation analysis

Abstract:

New observations of Neptune’s clouds in the near infrared were acquired in October 2013 with SINFONI on ESO’s Very Large Telescope (VLT) in Chile. SINFONI is an Integral Field Unit spectrometer returning a 64 × 64 pixel image with 2048 wavelengths. Image cubes in the J-band (1.09 – 1.41 μm) and H-band (1.43 – 1.87 μm) were obtained at spatial resolutions of 0.1″and 0.025″per pixel, while SINFONI’s adaptive optics provided an effective resolution of approximately 0.1″. Image cubes were obtained at the start and end of three successive nights to monitor the temporal development of discrete clouds both at short timescales (i.e. during a single night) as well as over the longer period of the three-day observing run. These observations were compared with similar H-band observations obtained in September 2009 with the NIFS Integral Field Unit spectrometer on the Gemini-North telescope in Hawaii, previously reported by Irwin et al., Icarus 216, 141-158, 2011, and previously unreported Gemini/NIFS observations at lower spatial resolution made in 2011.

We find both similarities and differences between these observations, spaced over four years. The same overall cloud structure is seen with high, bright clouds visible at mid-latitudes (30 – 40°N,S), with slightly lower clouds observed at lower latitudes, together with small discrete clouds seen circling the pole at a latitude of approximately 60°S. However, while discrete clouds were visible at this latitude at both the main cloud deck level (at 2–3 bars) and in the upper troposphere (100–500mb) in 2009, no distinct deep (2–3 bar), discrete circumpolar clouds were visible in 2013, although some deep clouds were seen at the southern edge of the main cloud belt at 30–40°S, which have not been observed before. The nature of the deep sub-polar discrete clouds observed in 2009 is intriguing. While it is possible that in 2013 these deeper clouds were masked by faster moving, overlying features, we consider that it is unlikely that this should have happened in 2013, but not in 2009 when the upper-cloud activity was generally similar. Meanwhile, the deep clouds seen at the southern edge of the main cloud belt at 30 – 40°S in 2013, should also have been detectable in 2009, but were not seen. Hence, these observations may have detected a real temporal variation in the occurrence of Neptune’s deep clouds, pointing to underlying variability in the convective activity at the pressure of the main cloud deck at 2–3 bars near Neptune’s south pole and also in the main observable cloud belt at 30 – 40°S.

Abstract:

A consortium of international scientists and industry partners are proposing the Main Belt Inventory Mission as a candidate in the next forthcoming ESA medium class mission call. The inventory mission will characterise a broad range of statistically significant asteroid samples throughout the Main Asteroid Belt (MAB). A 0.5 m aperture space-based telescope will conduct a detailed spectroscopic survey, observing thousands of objects from a range of 0.1-0.5 AU, and perform basic flybys of pre-selected targets. Each flyby will target an asteroid of a different size, taxonomic (sub)classes and orbital families, where spatially resolved spectral mapping and spectroscopy will be performed. Smaller and fainter passing targets will also be discovered, through opportunistic science, with dedicated star tracker-like cameras. Examining the compositional diversity across the asteroid population will provide a key tracer to understanding the dynamic evolution of the solar system, offer an insight into its early history and the origins of life forming material. Furthermore, by combing visible, near-infrared and thermal spectroscopy, the mission will unlock information on the major rock forming minerals, hydrated minerals, organics and primitive material found throughout the asteroid belt. Coarse UV mapping capability will search for weak OH emission bands, providing evidence of buried volatile (water) reservoirs. This will provide an additional link to fully understanding the meteorite record on Earth, and more importantly, place the returned samples from the up-and-coming Hayabusa-2 (JAXA) and OSIRIS-REx (NASA) missions in a wider geological context. The mission will provide an accurate description of the present day MAB population, and further refinements of the origins and evolution models of Near Earth Asteroids. This paper will report on the scientific justification and focus on the (sub-)system spacecraft design to perform a detailed inventory mission of the MAB. It includes an evaluation of the different system options and architecture designs. The baseline design is then presented, and further broken down for each subsystem. The science and mission objectives have been developed within the scope of the expected boundary conditions of the forthcoming ESA medium class mission call. It therefore necessitates a high TRL spacecraft, ready for launch within the 2028/32 timeframe on either a Vega-C (or Ariane 6) launch vehicle. The mission and system design is currently being developed through an ongoing mission study. Analysis is performed by a consortium of OHB System AG, Cranfield University and an association of scientists from different institutes and organisations. Concurrent engineering techniques are used throughout.

Abstract:

The exploration of the asteroid main belt is of the utmost importance to address many of the fundamental questions in modern planetary science (e.g., Solar System formation and evolution theories). This paper investigates potential opportunities for medium-class asteroid belt survey missions in the timeframe of 2029+. The launch as assumed here corresponds to that of the forthcoming ESA call for medium class mission proposals. The study has been developed in support of the CASTAway Asteroid Spectroscopic Survey mission proposal, which is to be submitted to the aforementioned call. CASTAway envisages the launch of a small telescope with relatively straightforward (i.e. high TRL) remote sensing instrumentation to detect asteroids at a range of 0.1-0.5 AU. The spacecraft would then head towards the main belt with the following objectives: The mission should test Solar System evolution theories by; 1) performing a statistical survey of small asteroid belt objects previously unsampled (<1 to a few tens of metre-sized); 2) providing compositional information for 1000s of objects by obtaining spectral data over a wide range of wavelengths, including key regions not observable through the Earth's atmosphere; 3) studying the morphology and geological history from close flybys of a targeted sub-set of objects, at least doubling the number of currently visited main belt asteroids within one single mission (>9 fly-bys). This paper presents a challenging multi-objective optimization problem and discusses the feasibility of such a mission concept. Firstly, a set of competing performance indices are defined that consider the cost of the mission, the quality of the survey (i.e. number of new detections and spectral data) and the number of asteroid fly-bys. The fly-by combinatorial problem is then tackled using the Minimum Intersection Orbital Distance as an heuristic filter to prune out unfeasible targets. Genetic and evolutionary algorithms are used to globaly optimize impulsive transfers, considering also planetary fly-bys, deep space and Δv-leveraging manoeuvres. Low-thrust trajectories are considered, although long thrusting periods impact negatively in the available operational time for remote sensing operations. Shape-based methods are used to globally optimize the low thrust controls, while the GPOPS-II and IPOPT transcribe the continuous-time optimal control problem and solve the subsequent nonlinear programming problem, respectively.