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National Space Society of Australia

presents

6th

Australian Space Science Conference July 19 - 21, 2006

supported by

Mars Society of Australia

Astra Australis

6th ASSC Chairman’s Welcome

On behalf of the National Space Society of Australia and the organising committee it is my pleasure to welcome you to the 6th Australian Space Science Conference. The program this year shows the progress of some continuing work, as well as some new directions in space-related research in Australia, with a range of speakers and topics that underlines the diversity of endeavours and disciplines contingent on space. We have included also special sessions in the program on commercialisation and public outreach. There will a be special presentation on the NCSS Decadal plan for Space Science Research in Australia (which will be followed by a workshop). During the lunch and coffee breaks, I would also encourage you to take advantage of the networking opportunities that the ASSC enables. I would like to thank our sponsors for their support and the Organising Committee for giving generously of their time and efforts. We trust that you will find the 2006 Conference enjoyable and informative.

Wayne Short

Chairman, 6th Australian Space Science Conference

Vice-President, National Space Society of Australia (NSSA)

HYATT HOTEL – Canberra

Floor Plan

DAY 1 - Wednesday 19th July 2006

Time Session Title

9:15 am Opening Kirby Ikin – APAC / NSSA

Opening Address / Conference Welcome (joint with ASDC)

9:30 am Dr Ron Huisken – Strategic Studies Centre (ANU)

Australia's Economic and Social Dependencies on Space

10:15 am Morning Tea

And Networking

10:45 am Wayne Short - NSSA Conference Opening - ASSC Session Stream 1 –

Geochemistry 1

11:00 am Antti Kallio - ANU Differentiation of terrestrial planets: insights from the volatile alkali elements rubidium and cesium

11:30 am Dr Charley Lineweaver - ANU

Estimating the composition of extrasolar terrestrial planets

12:00 pm Professor Rob Pidgeon – Curtin University

Timing of early events in The evolution of the Earth and the Moon : Evidence from zircon U-Pb Dating

Session Stream 2 – Outreach

11:00 am Carol Oliver - ACA New hi-tech virtual reality tool opens access to ‘science in the making’ to students and the public

11:30 am Glen Nagle – Deep Space Tracking Station

Education and Outreach with Mars Rover Mission

12:00 pm Naomi Mathers - VSSEC Victorian Space Science Education Centre: An Exciting New Facility for Science Education

12:30 pm Lunch Lunch Presentation: Australian Security Dependencies on Space Technology Mr. Brett Biddington, Cisco Systems (Australia)

Session Stream 1 – Planetary Science

2:00 pm Iain Brown – Sydney

University Mission planning for Space Debris Retrieval

2:30 pm Jonathan Mordech -

RMIT

Nano-Satellite Design for Inflatable Antenna System Prototype Demonstration

DAY 1 - Wednesday 19th July 2006 (continued)

Time Session Title

Session Stream 2 – Observation & Remote Sensing

2:00 pm Dr Jeremy Bailey - ACA Probing the Atmosphere of Venus using Infrared Spectroscopy

2:30 pm Alex Bevan – Museum of WA

The Desert Fireball Network: An All-Sky Camera Network in the Western Australian Nullarbor

3:00 pm Afternoon Tea

And Networking

A Plan for Space

Science and

Technology in

Australia

Join Session with ASDC

3:30 pm Dr Brian Boyle - ANTF Astronomical Decadal Plan 4:00 pm Professor Peter Dyson –

Latrobe University Space Science Decadal Plan

4:30 pm Dr Naomi Mathers VSSEC 5:30 pm

- 7:30pm

Cocktail Function

Murrumbidgee Room: Stream 1 & Main Conference Activities

Black Mountain Room: Stream 2 Activities

Federation Ballroom: Joint ASDC Sessions (Day 1 only)

DAY 2 - Thursday 20th July 2006

Time Session Title

9:00 am Panel Chair: Dan Faber - SpaceQuest Panel: Roger Franzen - Auspace Professor Peter Dyson - Latrobe University Dr Andrew Parfitt – UniSA / CRSS Dr Andrew Bell - ComDev

New Space Missions and Instruments


And Networking

Session Stream 1 – Planetary Science 1

11:00 am Dr Vickie Bennett - ANU Rapid Accretion and Formation of the Terrestrial Planets

11:30 am Dr Matilda Thomas – Geoscience / Mars Society

The nature and rates of landscape change on Earth and Mars

12:00 pm Dr Jeremy Bailey – ACA The Inner Solar System Cataclysm, the Origin of Life, and the Return to the Moon

Session Stream 2 – Commercialisation

11:00 am William Hulsey – University of Texas

Space Industry Intellectual Property Management: Rules and A Roadmap of Rising Relevance

11:30 am John Fick – Capital Technic Group

Space Business

12:00 pm Linda Di Mauro – AusIndustry

Commercial Ready Program, Commercialising Emerging Technologies (COMET), the R&D Tax Concession and the Industry Cooperative Innovation Program

12:30 pm Lunch Lunch Presentation: Mr. John Hargreaves MLA, Minister, ACT Government (Australia)

DAY 2 - Thursday 20th July 2006 (continued)

Time Session Title

Session Stream 1 – Geochemistry 2

2:00 pm Dr Trevor Ireland – ANU Isotopic composition of the Sun 2:30 pm Dr David Nelson – Curtin

University Short-lived radionuclides: stellar sources and early solar system chronology

Session Stream 2 – Human

Exploration

2:00 pm Dr Jon Clarke – GeoScience / Mars Society

A Conservative, Practical Architecture for Exploration-Focused Manned Mars Missions Using Chemical Propulsion, Solar Power, and ISRU.

2:30 pm Dr Marc Norman – ANU Why on Earth are we going back to the Moon?


And Networking

3:30 pm Workshop Professor Peter Dyson – Latrobe University

Space Science Decadal Plan

5:30 pm

- 10:00 pm

Pre-Dinner Drinks

& Joint Conference

Gala Dinner

Dinner Speaker: John Keating, COMDEV



DAY 3 - Friday 21st July 2006

Time Session Title

New Propulsion

Methods

9:30 am Dr Christine Charles - ANU

From Aurorae to Mars, the Australian Helicon Double Layer Thruster

10:00 am Dr Orson Sutherland - ANU

Design and Testing of a Dual Stage Ion Engine for Deep Space Applications


And Networking

Session Observation and Remote Sensing 2

11:00 am Erin Anania - UTS Using Mars Global Surveyor and Mars Odyssey telemetry to reconstruct the volcano-tectonic history of Phaethontis region, Mars

11:30 am Dr Graziella Caprarelli - UTS

Mars Express High Resolution Stereo Camera: results of observations of north Tyrrhena Terra, Mars

12:30 pm Lunch Lunch Presentation: Developments in Small Satellite Capabilities Mr. Daniel Faber, SpaceQuest, (Canada)

Session Stream 1 – Space Engineering 2

2:00 pm Jason Cromarty - RMIT Data Mining Techniques for GAIA Data Processing and Analysis

2:30 pm Nick Ward – QUT Short-lived radionuclides: stellar sources and early solar system chronology

Session Stream 2 – Planetary Science 2

2:00 pm Jose Robles - ANU How anomalous is the Sun? 2:30 pm Dr Noel Jackson -USQ Preliminary Graphical and Statistical

Analysis of Lunar Iron (FeO) and Titanium (TiO2): Results of Megaregolith and Subsurface Investigations

DAY 3 - Friday 21st July 2006 (continued)

Time Session Title


And Networking

Session Planetary Science 3 3:30 pm Nathan Parrott – Sydney

University Intelligent control of liquid-fuelled bi-propellant premix rocket motors

4:00 pm Ian Bryce - ASRI Rocket Development and Operations within the Australian Space Research Institute

4:30 pm Closing Remarks



PROPULSION SYSTEMS

From Aurorae to Mars, the Australian Helicon Double Layer Thruster

Authors

Christine Charles and Rod Boswell Space Plasma, Power and Propulsion group,

Research School of Physical Sciences and Engineering, The Australian National University (ANU), Canberra, ACT 0200, Australia

Abstract

The Helicon Double Layer Thruster (HDLT) is a radically different space plasma engine that is based on

our recent discovery of a current free electric double layer in an expanding plasma. Electric double layers

are like cliffs of potential which can energise charged particles falling through them. They exist in the

plasma environment of the earth and the stars and can cause phenomena as diverse as aurorae,

electromagnetic radiation from rotating neutron stars called pulsars and ion heating in the magnetic funnels

of the solar corona.

We have discovered such a double layer in our laboratory plasma systems and measured the energy of the

highly supersonic ions it has accelerated. This ion acceleration can be used for thrust in a spacecraft. The

Space Plasma, Power and Propulsion group at ANU has developed the first HDLT prototype, in

collaboration with the CRC for Satellite Systems and AUSPACE, and funded by a DEST Innovation access

grant. In April 2005, a successful test campaign was carried out at the European Space Agency development

centre (ESTEC, The Netherlands).

The HTLT is simple, has no moving or degradable parts, no electrodes and no need for a neutraliser. Its

advantages are high fuel and power efficiency, increased lifetime, simplicity, scalability and safety, making

it a very attractive candidate for deep space travel. The ANU group is developing its own Space Simulation

Chamber facility for further testing. Both the research and space development efforts are being carried out

by a team of scientists and Ph D students in collaboration with astrophysicists, rocket scientists, and plasma

physicists around the world.

Design and Testing of a Dual Stage Ion Engine for Deep Space Applications

Authors:

Orson Sutherland, Peter Alexander, Dennis Gibson, Christine Charles and Rod Boswell

Space Plasma, Power and Propulsion Group Research School of Physical Sciences and Engineering

The Australian National University Canberra, 0200

Roger Walker, Pierre-Etienne Frigot and Marika Orlandi ESA-ESTEC

Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands

Abstract:

A small, relatively low-power experimental laboratory model of a novel gridded ion thruster, the “Dual-Stage 4-Grid”(DS4G) thruster, has been designed and manufactured by the Australian National University (ANU) and proven under laboratory conditions at the European Space Agency (ESA) Electric Propulsion Test Facility in the Netherlands. The DS4G concept is able to operate at very high specific impulse, power and thrust densities, well in excess of conventional 3-grid ion thrusters. The principal purpose of the prototype was to prove the feasibility of the concept for space propulsion, to demonstrate the performance predicted by analytical and simulation models, and to investigate critical design parameters and technological challenges in preparation for any future spacecraft integration. In this presentation, the basic concept of the DS4G ion thruster is presented, along with the design, operating parameters and measured performance obtained from the first and second phases of the experimental campaign. Finally, the implications of these findings for future gridded ion thruster developments and future mission applications are addressed.

Biography – Orson Sutherland

Orson Sutherland has been working in the design and development of space propulsion for 6 years having

participated on several development projects and test campaigns with NASA's Advanced Space Propulsion

Laboratory (ASPL) and ESA's Advanced Concepts Team (ACT) and Electric Propulsion Laboratory (EPL).

These test campaigns have spanned three key next generation technologies for future space propulsion and

comprise NASA's VASIMR rocket concept, the ANU's Helicon Double Layer Thruster (HDLT) and

ANU/ESA's Dual Stage Four Grid (DS4G) thruster.

Orson has been the Technical Director of the DS4G thruster prototype for the past year, which was

commissioned by and tested at the European Space Agency. It demonstrated the world's first successful dual

stage gridded ion thruster operation as well as breaking several efficiency and thrust/power density records.

Orson's primary area of expertise is in plasma physics and ion optics which he has adapted both to the

development of high brightness plasma ion sources for the semiconductor industry as well as high

performance plasma/ion thrusters for the space industry.

SPACE ENGINEERING

Intelligent Control of Liquid Fuelled Bi-propellent Premix Rocket Motors

Authors:

Nathan Parrott: University of Sydney, Aerospace and Mechatronics Department Jason Held: ARC Centre of Excellence in Autonomous Systems, Australian Centre for Field Robotics

Abstract:

The Intelligent control of rocket propulsion systems offers the same incentives of performance and efficiency as the arrival of engine control units in automobiles. The reason for their absence in smaller rocket propulsions systems of the past is the result of a number of factors prevalent at the time. Firstly rocket propulsion systems suffered from a lack of mechanical reliability and safety allowing for cheaper mechanical opportunities to improve engine performance. Secondly computational power to weight ratio was not yet good enough to justify the inclusion of bulky computer hardware at the expense of reduced payload. Finally the added complexity of including engine control systems to the already overwhelming engineering feat of rocket engine design was only seen to further increase instabilities in the motors of the time. As time has progressed however these factors have been overcome, and engine control units now serve as the primary unit to further increase performance, efficiency, stability and safety of rocket engine propulsion systems. In conjunction with the University of Sydney’s Ogoun project (the design and construction of a small liquid fuelled bi-propellent premix rocket motor) an intelligent control system is to be designed and constructed to achieve a number of higher order objectives to increase the performance and efficiency of the motor during static hot testing. The inclusion of an onboard health management system will serve to diagnose potential issues and take remedial action to reduce the need for ‘in-flight’ shutdowns as well as offer information related to suggested maintenance scheduling and part cycling thus reducing the overall maintenance cost of the engine. A description of this intelligent control system and its primary objectives will be presented with initial results given.

Biography – Mr Nathan Parrott

Nathan Parrott is a fourth year mechatronic engineering student at the University of Sydney. A member of

the University’s rocket society (RocketSoc) he has taken an interest to the space engineering curriculum

provided by the Uni and is currently playing a leading role in the development of the Ogoun project test

stand and control system. He is currently doing his undergraduate honours thesis on the intelligent control of

a liquid fuelled bi-propellent premix rocket motor.

Mission Planning for Space Debris Retrieval

Authors:

Jason Held, ARC Centre of Excellence for Autonomous Systems, Australian Centre for Field Robotics Iain Brown, ARC Centre of Excellence for Autonomous Systems, Australian Centre for Field Robotics Igor

Vainshstein, Adept Connections, Inc.

Abstract:

Space debris is a steadily growing industry problem with few mitigation methods. First are restrictions on engineering to minimize debris created from launch. Second is on-orbit End of Life (EOL) control of the spacecraft, either supersynching or deorbiting (controlled reentry) a nearly dead spacecraft. Neither method guarantees a space clear of debris, resulting in increasingly cluttered commonly used orbits. Likewise, there is an increasing need for a method to clear commonly used (and expensive) orbits. This paper discusses the requirements to actively mitigate, retrieve, and possibly reuse space debris from a mission planning and analysis perspective. Active method of retrieval using an automated (or semiautonomous) spacecraft has several advantages. Orbital paths/positions may be pre-prepped for safer arrival of a new spacecraft. Spacecraft near their EOL may be returned to the International Space Station for refuelling and refit, which may be less expensive than construction and launch of a new system. Finally, destroyed or seriously degraded components (such as initial stages) may be stored for future construction or scientific use. This represents a key component to future space logistics infrastructures—a possible inventory of reusable mechanical parts. With a goal of low cost retrieval and safe mission operations, mission parameters, orbits, and conceptual spacecraft design are conducted to determine how active retrieval can be done in a cost effective manner using current automation techniques. Results will present basic mission and engineering requirements for several “common need” sample retrieval missions.

Biography – Mr Iain Brown

Iain Brown is a technical officer working at the Australian Centre for Field Robotics. He is a graduate from the University of Sydney in Aeronautical (Space) Engineering. He has worked on a variety of engineering projects from assisting in the management of the ongoing CASsat program, run in collaboration with the University of Sydney, to recent work on cooperative autonomous UAVs, to being a team member of the winning design team of the 2002 International ‘Health Care Without Harm’ Medwaste Design Competition.

Nano-Satellite Design for Inflatable Antenna System Prototype

Demonstration

Authors:

Jonathan Mordech : School of Aerospace, Mechanical & Manufacturing Engineering, RMIT University

Lachlan Thompson : School of Aerospace, Mechanical & Manufacturing Engineering, RMIT University Assoc. Professor

Abstract :

Introduction: Increasing innovation within educational institutions augments the need for adaptable, effective, low budget-rapid schedule system prototype demonstration. A nano-class satellite is being designed to conduct the deployment of an inflatable antenna prototype developed at RMIT University. Methods: System engineering and project management principles are being used to achieve integrated project development. The design process, consisting of multiple reviews, is supported by robust system and subsystem requirements which ensure that mission and performance specifications are met. Extensive research, trade studies and modeling are being employed. Results: Nano-DemoSat, 1kg spin-stabilized type nano satellite, is being designed. Its light weight and low volume enable its integration into a multi-payload adapter, facilitating a piggy-back into low earth orbit. There, Nano-DemoSat is able to monitor the antenna’s operational performance and configuration during a 48 hour mission in space. Following separation and orbit insertion, the inflation process is visually recorded by CCDV camera. Its payload of pressure, radio displacement, thermal and vibration sensors collect operational data and transmit it to a basic ground station. Conclusion: The design concept of Nano-DemoSat is easily applied to other developing satellite technologies, particularly inflatable and gossamer-type structures. As such, the viability of low cost system prototype demonstration will be established, thereby increasing the scope of university-based space development and innovation.

Data Mining Techniques for GAIA Data Processing and Analysis

Authors:

Jason Cromarty1, Cees Bil2 , Robin Hill3, Lachlan Thompson4 1 School of Aerospace, Mechanical and Manufacturing Engineering

RMIT University GPO Box 2476V Melbourne, Victoria 3001 Australia Email: [email protected]

2, 4 The Sir Lawrence Wackett Centre for Aerospace Design Technology RMIT University GPO Box 2476V Melbourne, Victoria 3001 Australia

Ph: +613-96454536, Fax: +613-9645 4534 Email: [email protected], [email protected]

3 School of Mathematical and Geospatial Sciences RMIT University GPO Box 2476V Melbourne, Victoria 3001 Australia

Ph: +613-99253161, Fax: +613-99251748 Email: [email protected]

Abstract:

Data mining techniques are proving to be one of the top ten burgeoning technologies. With ever expanding worldwide scientific databases, data mining methodologies will be relied upon to extract and discover previously invisible conclusions and facts that are contained in these complex and large relational databases. In the field of astronomy these data mining techniques will be particularly valuable. Contained in this paper is a discussion on data mining techniques that are potentially applicable to the data sets of the European Space Agency (ESA) Gaia universe surveying spacecraft, which is due to be launched in 2012. The paper discusses specific data mining applications for the large amount of astronomical data to be collected by Gaia and also details preliminary research into mining algorithms.

Biography - Jason Cromarty

Jason Cromarty is an Aerospace Engineering undergraduate student at the Royal Melbourne Institute of

Technology (RMIT). He is currently Vice President of the Aerospace Students Association and is a research

assistant at the Sir Lawrence Wackett Centre for Aerospace Design Technology.

Reduced Gravity Testing and Research Capabilities at

Queensland University of Technology

Authors:

Dr. Ted Steinberg, Nick R. Ward

Phenomena in µ-Gravity Lab

School of Engineering Systems

Faculty of Built Environment & Engineering

Queensland University of Technology

Brisbane, Queensland, Australia

[email protected]

Abstract:

The industrial and commercial development of space-related activities and often the ability to better characterise many important terrestrial phenomena is intimately linked to the capability to conduct reduced gravity research. Reduced gravity experimentation is important to many diverse fields of research in the understanding of fundamental and applied aspects of physical phenomena. Both terrestrial and extra-terrestrial experimental facilities are currently available to allow researchers access to reduced gravity environments. This paper provides a short summary of the Queensland University of Technology’s 2.0 second drop tower, including its specifications and operational procedures. Information concerning the current areas of research being conducted is also presented and discussed. These research areas include: 1) Fluid Dynamics, 2) Nanomaterials and 3) Biomedical science and 4) Combustion (with focus given to the development of an understanding of the unique heterogeneous burning mechanism of bulk metallic materials in oxygen). A short description of available research opportunities will also be presented with emphasis on both collaborative research and the provision of reduced gravity test services.

BIOGRAPHY: Mr. Nicholas Ward

Nick is a post-graduate student from the Phenomena in Microgravity Laboratory at the Queensland University of Technology, in Brisbane, Australia. Nick conducts fundamental research in the field of reduced-gravity metals combustion. Nick’s work contributes to an improved understanding of heterogeneous burning phenomena, for improved oxygen system fire safety in space and on the ground. Before beginning the PhD program, Nick completed an undergraduate degree at the University of Queensland, majoring in Mechanical and Space Engineering.

Rocket Development and Operations within the Australian Space Research

Institute

Authors:

Ian Bryce

Director, Australian Space Research Institute

Abstract:

ASRI originated from groups of students, engineers and enthusiasts working since 1991 to promote space

and launch activities in Australia. This paper will describe our background, our rise to Research Institute

status, our past achievements and present projects.

ASRI has provided hundreds of thesis projects for university students, who learn the design-build-test cycle

while ASRI obtains components of rockets and payloads.

The Ausroc family of home-designed liquid-fuelled rockets ranges from the small Ausroc 1 flown in 1987 to

the proposed Ausroc 4 space launch vehicle. The current project is Ausroc 2.5, under construction around

Australia and indeed the world, slated for a 2007 launch to 30 km altitude.

Our small solid rocket program (SSRP) makes use of surplus missile motors from the defense forces,

conducting accredited launch campaigns at Woomera twice a year. They form a testbed for technology

development including control systems and procedures, safe-and-arms, separation systems, parachutes, and

telemetry. The flights provide students with the opportunity to launch payloads, including eight flown on

two contracted launches for the International Space University.

SSRP also enables University of Queensland students to fly propulsion experiments, and collaborations

include the Hyshot hypersonics program. ASRI members learn skills which assist them to go on to key

space industry positions.

HUMAN EXPLORATION

A Practical Architecture for Exploration-Focused Manned Mars Missions Using Chemical Propulsion, Solar Power Generation and In-Situ Resource

Utilization.

Authors:

David Willson (1) and Jonathan D. A. Clarke (2) (1) SEMF 2nd floor 45 Murray St, Hobart. Tasmania 7000, Australia

(2) Australian Centre for Astrobiology, Macquarie University, NSW 2109, Australia

Abstract:

Many manned Mars missions and spacecraft concepts have been proposed in the past 50 years. These have included Von Braun’s ‘Das Marsproject’ in the 1950’s (winged vehicles and chemical propulsion), NASA proposals of the 60’s (nuclear rockets and conical landers), the Soviet Mars plans in the 1980’s (Soyuz and Mir-derived hardware), Niehoff’s ‘VISIT’ cycler orbit scenario also in the 1980’s and Zubrin’s ‘Mars Direct’ (tuna-can modules, in-situ resource utilization (ISRU), nuclear power generation and chemical propulsion) in the early 1990’s. Most recent have been an ESA proposal (chemical propulsion, no ISRU and limited Mars surface stay) and the various ‘Design Reference Missions’ from NASA using ‘Semi-Direct’ mission architectures relying extensively on nuclear power for propulsion, power generation and ISRU. These mission architectures and vehicle concepts were based on the best-available knowledge regarding spacecraft design and the Mars environment. The science and exploration objectives were also fashionable for the time. This paper aims to add an alternative mission architecture using biconic and horizontally landed bent biconic vehicle design concepts. The design aims are to provide a manned Mars mission at minimum cost while maximising safety, reliability and science outcomes and provide infrastructure on the Mars surface suitable to build a long life station. In the process key choices involving mission architectures and vehicle design are explored and quantified. These choices include options for orbital trajectories, Mars orbit insertion techniques, whether or not to adopt Phobos as a base, the provision of an ISRU plant on the Martian surface, the number of crew, nuclear or solar power, nuclear, chemical or electric propulsion, the level of recycling and the type of structures best suited to build a long term base. Finally we provide a family of vehicle design concepts with associated mass estimates suitable for planning the infrastructure required for a future manned Mars mission.

Biography : Mr. David Willson

David Willson is a Director of Mars Society Australia and has managed the MARS-OZ project for the past two years, two papers by David and others on MARS-OZ have been published this year in the Journal of the British Interplanetary Society. He also took part in the Expedition 2 to Arkaroola in 2004. David is currently senior mechanical engineer with SEMF Pty, Ltd, based in Hobart. He has a background in industry for the last 12 years as a design manager, projects engineer, responsible mechanical engineer, site engineer and mechanical design engineer. David has tendered, designed, commissioned and implemented projects worth up to $15m. The projects have covered power plant infeed systems, mineral processing plants, mining and wharf bulk handling systems, shiploaders, stackers, mobile equipment and aircraft ground support maintenance management procedures. Detailed experience includes design in fluid mechanics, steam, pneumatics, hydraulics, processing dangerous chemicals, winches, bogies, electrical installation, commissioning writing manuals and training operators and maintenance staff. A recent project, a shiploader at Esperance WA won a WA. Institution of Engineers environmental design award and a Tasmanian Institution of Engineers design award.

Why on Earth Are We Going Back to the Moon: Scientific and Cultural

Rationales?

Authors:

Marc Norman1*, Paul Spudis2, Harrison Schmitt3, Carle Pieters4

1. Australian National University

2. Applied Physics Laboratory

3. University of Wisconsin

4. Brown University

* Corresponding Author: [email protected]

Abstract:

The Moon is the cornerstone of our understanding about the formation of terrestrial planets and the future exploration of the Solar System. Australian scientists lead by Ted Ringwood, Ross Taylor and Bill Compston played a major role in understanding the origin and evolution of the Moon through studies of lunar samples returned to Earth by the Apollo program. The current exploration environment will provide new opportunities for all avenues of research in Australia ranging from geosciences to remote sensing, biomedics, technology development, and information management.

Science: 4.5 billion years of geology are readable in samples from the lunar surface. Global datasets for key parameters such as major and trace element chemistry can be linked with detailed laboratory analysis of lunar samples. The lunar crust provides spectacular evidence of early global differentiation, and bombardment by asteroid-size planetesimals.

Resources: The Moon contains reservoirs of material and energy required for space operations. High concentrations of hydrogen occur in permanently shadowed regions near the poles. This hydrogen may exist as ice or implanted in reactive surfaces of mineral grains from which water can be extracted. Permanently lit areas near the poles may provide continuous solar power without the need for overnight storage.

International cooperation: Exploring the Moon presents opportunities for unprecedented levels of international cooperation. The national and scientific rationales for planetary exploration are recognized by many nations. World leaders will need to acknowledge the creative and competitive spirit that will drive the long-term exploration of the Moon and other planets.

Inspiration: Challenges inherent in planetary exploration will require an educated, technically literate, and youthful workforce. Exploration demands not only the best technical knowledge but also the best imaginations. Creativity is the core renewable resource of a vibrant society; it functions best by confronting and surmounting unknowns and challenges of new frontiers. The Moon is a staging ground, supply station and classroom for voyages to Mars and beyond.

The Inner Solar System Cataclysm, the Origin of Life, and the Return to the

Moon

Author:

Jeremy Bailey

Australian Centre for Astrobiology, Macquarie University

[email protected]

Abstract:

The Apollo lunar missions have provided a means of studying the early impact history of the Moon (and hence other solar system bodies) by calibrating cratering records using radiometric dates. However, the interpretation of the data has been the subject of considerable debate. While some argue that the data are consistent with a steadily declining impact rate, the preponderance of impact-melt dates around 3.9Ga has led others to conclude that there was a cataclysmic bombardment during the period 3.8-4.0Ga, with much lower impact rates at earlier times. This is known as the Lunar Cataclysm, or Late Heavy Bombardment. More recent evidence suggests that this cataclysm affected the entire inner solar system. It has recently been suggested that the cataclysm is due to a different population of impactors to those responsible for subsequent cratering, and that the cataclysm may have been triggered by the readjustment of the orbits of the giant planets. The cataclysm occurred at a time just before the earliest evidence for life on Earth and has important implications for the origin and early evolution of life. The cataclysm theory leads to much lower total impact rates on the very early Earth than the “steady decline” model. This opens up the possibility that life on Earth could have started very early, and survived through the cataclysm. Alternatively the cataclysmic bombardment may itself have played a role in the origin of life, through delivery of organics to the Earth, creation of temporary environments, or transferring material between planets. The new NASA Vision for Space Exploration, with its plans for renewed robotic and human exploration of the Moon will provide an opportunity to obtain much better sampling of the lunar surface and to establish the detailed impact history of the early solar system.

Biography - Dr Jeremy Bailey

Jeremy Bailey is the Associate Director of the Australian Centre for Astrobiology at Macquarie University, Sydney, and leads a research group that studies the atmospheres and surfaces of planets using remote-sensing techniques and atmospheric modelling. He is originally from the UK, and has previously worked at the Anglo-Australian Observatory and the Joint Astronomy Centre, Hawaii. He represented Australia at the recent NASA Exploration Strategy workshop in Washington DC.

PLANETARY SCIENCE

Rapid Accretion and Formation of the Terrestrial Planets

Authors:

Vickie C. Bennett

Research School of Earth Sciences, The Australian National University, Canberra ACT 0200. [email protected]

Abstract:

Studies of meteorites and theoretical studies of nebular evolution reveal that planetary bodies form very early in solar system history. What the “age” of a planet means, however, can have many different answers. It may refer to volatile depletion during accretion, initial melting and formation of an igneous crust, or the timing of major planetary differentiation such as separation of metallic cores from silicate mantles. Ages determined from terrestrial and lunar rocks and meteorites using a diverse array of radioactive decay schemes combined with theoretical models can now provide constraints on the timing of major planetary events including accretion, core formation and crustal growth on the Earth, Moon, Mars, and igneous asteroids. Spurred by analytical advances and the acquisition of larger planetary sample suites including new localities representing the early Earth, an increasingly detailed view of the timing and processes responsible for early planetary differentiation is emerging. For example, decay schemes based on now extinct isotopes such the decay of 146-samarium to 142-neodymium (half-life 103 million), and 182-tungsten to 182-hafnium (half-life 9 million years) are providing new insights into early events that shaped the terrestrial planets. Here I review the planetary chronologies of the Moon, Mars and the early Earth from an isotopic perspective. Accretion of rocky planetesimals was synchronous with some of the earliest datable events in the solar nebula as recorded by primitive meteorites. Large-scale melting and internal differentiation of proto-planetary bodies occurred on timescales of 10’s of millions of years. This contrasts dramatically with the prevailing view of just a few decades ago in which planets heated slowly over billions of years by accumulation of internal heat from long-lived radioactive decay. Rapid timescales of planet formation implies dynamic accretion probably involving large collisions between protoplanetary bodies and short-lived radioactive heat sources.

The Nature and Rates of Landscape Change on Earth and Mars

Authors:

Colin Pain1, Jonathan D.A. Clarke2*, Matilda Thomas2 1 4 Sticht Place, Florey ACT 2615, Australia

2 Australian centre for Astrobiology, Macquarie University * Corresponding Author: [email protected]

Abstract:

One of the driest places on Earth is the Atacama Desert of southern Peru in the region around Nazca, although the landscape is fluvial, with rounded hillslopes and alluvial plains including dry river channels. The 1500 year-old human-made Nazca lines cross many of the channels without a break, showing that most of these channels have not seen flowing water for at least 1500 years. Occasionally yellow streaks are observed in the middle of channels, evidence of the movement of water and sediment down the valley floor. Where a streak crosses a line, it wipes it out. The only major activity is aeolian reworking of the fine fraction of alluvial sediments. In 1500 years aeolian activity has only slightly modified the landscape. Fluvial and aeolian features are superimposed on a much older large scale fluvial landscape whose shaping has been shown by cosmogenic dating to have been completed 25 million years ago. Some regions on Mars also seem to be a result of a period of rapid large scale fluvial activity followed by a much longer period of aeolian activity that has done little to modify fluvial landscapes. An intense terminal epoch of widespread fluvial activity” occurred during the Noachian Period up to the beginning of the Hesperian, about 3.5 Ga. Small scale and localised water flows from snow melt and spring discharge may have continued episodically through to the present, without significantly modifying the larger fluvial features. Comparison between the Nazca landscape and similarly eroded features on Mars indicate that the period of very of slow modification of the large scale fluvial martian landscape is 140 times longer than at Nazca, one of the oldest well preserved landscapes on earth.

Preliminary Graphical and Statistical Analysis of Lunar Iron (FeO) and

Titanium (TiO2): Results of Megaregolith and Subsurface Investigations

Authors:

Noel W. Jackson1*

, Brad D. Carter1

1Department of Biological and Physical Sciences, University of Southern Queensland, Toowoomba Queensland 4350 *Corresponding Author: [email protected]

Abstract:

In this work we examine the relationships of FeO and TiO2 in the ejecta of 2059 lunar craters in the Highland, Mare, and South Pole Aitken basin. The data was processed from Clementine Imagery. This analysis provides a statistical overview of the iron and the titanium trends in these three terranes, providing a guide for future analysis. The distribution of FeO in the Highland terrane indicates a broad decrease in weight percentage values with depth that correlates with TiO2 values. The Highland II iron-enhanced regions exhibit unexpected high levels of iron, although concentrations still decline with depth. The Mare terrane exhibits a decrease and a levelling of FeO values and then an increase in value providing a graphical broad “U” shape. This suggests that there are 3 layers of iron-rich basalt overlaying iron-poor material, possibly a basalt / anorthosite mix, in turn overlying a mafic layer. The TiO2 content of Mare exhibits an even distribution with depth and then an increase. This outcome might be as a result of two populations of ejecta, one in the titanium-poor mare and the other in titanium-rich mare. Not all maria are covered with titanium-rich basalts. Meteorite analysis indicate only barely significant traces of Ti at most, therefore impactors are unlikely to be a significant source. The FeO content in the South Pole Aitken basin displays no discernable trend, but the TiO2 content shows a constant distribution with depth and a decrease at greatest depth of between 2 and 3 kilometres, that may suggest that the Ti source was outside this region.

Biography - Dr Noel Jackson Noel was born in Brisbane Australia, attending Primary and High School in Brisbane. Noel completed

matriculation at Evening Classes and also undertook preparatory studies for University entrance. He studied

for a Bachelor in Applied Science (Geology major, Physics sub-major) at the Queensland University of

Technology, Brisbane, graduating in 1991. In 1993 he graduated with a Graduate Diploma in Remote

Sensing and then in 1995 Bachelor of Sciences (Honors – Applied Geology) from the University of New

South Wales, Sydney. The years 1996 to 1998 saw Noel studying for a Master of Science (Geology- lunar

research thesis) at the Old Dominion University in Norfolk Virginia USA, graduating in 1999. Subsequently

returned to Australia and undertook casual tutoring and lecturing and then in 2001 commenced a PhD

(Physical Sciences – lunar research) at the University of Southern Queensland in Toowoomba Australia –

graduating in 2005. Since graduation Noel has been a Research Associate at the University of Southern

Queensland.

Noel’s research and interests lay in Planetary Studies and Remote Sensing of planetary bodies.

How Anomalous is the Sun?

Authors:

Jose Robles1-2*, Charley Lineweaver1-2

1 Planetary Science Institute, Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT, Australia

2 Research School of Earth Sciences, Australian National University, Canberra, ACT, Australia * Corresponding Author

Abstract:

Is the Sun an average star? Or is it anomalous in some way that is associated with habitability and led to our existence? Might life only be possible around special stars? To determine if the Sun is special in any important way, we make the most comprehensive comparison of the fundamental parameters of the Sun to those of other stars. These parameters include: mass, age, metallicity, elemental composition, carbon to oxygen ratio, other elemental ratios, position and velocity with respect to other stars in the Milky Way Galaxy. We present the distributions of these parameters from carefully selected representative samples of stars and then compare the Sun’s value of the parameter to these distributions. Thus, we quantify the extent to which the Sun is special. We show that the Sun is normal with respect to most parameters and mildly anomalous with respect to several others.

Biography - Mr Jose Robles Jose did a summer physics research internship on 2002 at Fermi National Accelerator, IL, USA. He completed his B.S. in Physics at the Universidad de las Americas at Puebla City, Mexico with honors in Astronomy in 2003. Participated at the LAPLACE Astrobiology Graduate Winter School at the University of Arizona in January 2006. Jose is currently studying for his PhD at the Australian National University.

GEOCHEMISTRY

Differentiation of terrestrial planets: insights from the volatile alkali elements rubidium and cesium

Authors:

Kallio, A. P. A.1*, Ireland, T. R.1 1 Research School of Earth Sciences, Australian National University,

Canberra ACT 0200, Australia * Corresponding Author:

Abstract:

Refractory lithophile elements occur in constant ratios in chondritic meteorites and the silicate portions of the Earth, Moon and Mars. In contrast, the moderately volatile alkali elements show larger variations in and between these bodies, reflecting variable thermal histories and differing amounts of aqueous activity. Of special interest for differentiated planets such as Earth, Mars, and the Moon are the budgets and ratios of the highly incompatible alkali elements rubidium (Rb) and cesium (Cs), as they are not fractionated to a large degree by mantle melting or crystallization of ferromagnesian minerals (olivine, pyroxene, spinel). The Earth has major fractionated reservoirs. The mantle and the continental crust have significantly different Rb/Cs ratios that can only be produced by the formation of hydrous minerals such as clays, and preferential partitioning of these elements during formation of continental crust. The Rb/Cs ratios of lunar rocks and martian meteorites are slightly elevated relative to chondritic (assumed to represent average solar system) and show relatively little variation, despite the large difference in the volatile contents of these bodies. This implies little role for water during crust-mantle differentiation on Mars and the Moon. To better constrain the Rb/Cs systematics of the Earth’s mantle through time, we assembled basaltic samples with a wide range of ages and found olivine-hosted melt inclusions in several samples that erupted 3.3-1.9 billion years ago. We developed techniques for analysing Rb, Cs and other trace elements from single inclusions using SHRIMP ion microprobe and laser ablation plasma-source mass spectrometry. These melt inclusions show smooth primitive mantle-normalised patterns for immobile incompatible trace elements that are consistent with depletion of the mantle by melting. Primitive basalts show a Rb-Cs range of compositions consistent with diverse processes including dry melting, hydrous alteration, crustal contamination or fluid-mobility in the mantle.

Estimating the Compositions of Extrasolar Terrestrial Planets

Authors:

Charley Lineweaver1-2

*, Jose Robles1-2

1 Planetary Science Institute, Research School of Astronomy and Astrophysics, Australian National

University, Canberra, ACT, Australia 2 Research School of Earth Sciences, Australian National University, Canberra, ACT, Australia

*Corresponding Author

Abstract:

The Earth is a devolatilized piece of the Sun left over from the Sun’s formation. That is, if we did not know which star was ours, we could recognize it from a comparison of the refractory elemental compositions of the Earth and of the stars. The main idea is that extrasolar terrestrial planets will be devolatilized pieces of their host stars as well. If this is correct (and we will argue that it is) we can infer the elemental compositions of extrasolar terrestrial planets from spectroscopic measurements of the elemental compositions of other stars. An important part of this procedure is to quantify the devolatilization and chemical fractionation processes that occurred in our Solar System 4.5 billion years ago. To do this we compare the elemental abundances in the Sun to the major features of the elemental abundances of the rocky planets in our Solar System. Under the reasonable assumption that these fractionation processes are universal features of rocky planet formation, we make estimates of the chemical composition of extrasolar terrestrial planets from measurements of the elemental abundances of other stars. We will discuss the appropriateness of various stellar surveys being used as “representative” samples. These surveys include Edvardsson et al. (1993; Astron. & Astrophys. 275, 101); Reddy et al. (2003; Mon. Not. Roy. Astro. Soc.340, 304); and Valenti and Fischer (2005, ApJS 159, 141).

Biography – Dr Charley Lineweaver

Charles H. Lineweaver is the coordinator of the ANU Planetary Science Institute and holds a joint appointment as an associate professor in the Research School of Astronomy and Astrophysics and the Research School of Earth Sciences. He obtained an undergraduate degree in physics from Ludwig Maximillians Universitat, Munich, Germany and a PhD in astrophysics from the University of California at Berkeley. He was a member of the COBE team, led by George Smoot, that discovered the temperature fluctuations in the cosmic microwave background. Before his appointment at ANU, he held post-doctoral positions at Strasbourg Observatory and the University of New South Wales where he taught one of the most popular general studies courses “Are We Alone?” His research areas include cosmology (determination of the age and composition of the universe) exoplanetology (the statistical analysis of exoplanets) and astrobiology ( using our new knowledge of cosmology to constrain life in the Universe). His research has been published in Science, Nature, the Astrophysical Journal, Astrobiology, Scientific American, American Journal of Physics, and Microbiology Australia.

The coincidence of U-Pb ages of ancient zircons on the Earth and the Moon

Authors:

R.T.Pidgeon1*, A.A. Nemchin

2

1 Department of Applied Geology, Curtin University of Technology, Perth, Western Australia. 2 W.A. School of Mines, Curtin University of Technology, Perth, Western Australia.

* Corresponding Author: [email protected]

Abstract:

In recent years new opportunities have arisen for investigating the timing of the earliest events in the history of the Earth and the Moon. In particular the discovery of zircon in many lunar breccias has opened the way to date zircon-forming events on the Moon by measuring U-Pb ages of small parts of single zircon crystals using the SHRIMP ion microprobe. Zircon U-Pb ages are known to be extremely robust compared with other radiometric techniques such as Ar-Ar and Rb-Sr, which are more easily disturbed by thermal events associated with impacts or the Pb-Pb technique which is confounded by the extremely radiogenic Pb in lunar rocks. Our present studies of lunar zircons, combined with earlier reports, show that U-Pb ages of zircons from lunar breccias fall within the range 4380 to 3900 million years. It is an exceptional coincidence that this age range is almost identical with that determined on detrital zircons from ca 3000 million year old sediments from Mt Narryer and the Jack Hills in the Yilgarn Craton of Western Australia. Zircons older than 4000 million years are not found anywhere else on Earth and consequently these are the only known surviving material of the earliest period of Earth history. The significance of the coincidence of the age range of the ancient terrestrial and lunar zircons is not yet understood. Our current research is directed towards an understanding of the early ages by determining the fine structure in the timing of events in the lunar and terrestrial zircons and to use this and the chemistry of the zircons to place limits on the nature and timing of the earliest events in the Earth -Moon system.

Biography - Robert T. Pidgeon

Presently adjunct Professor at the Curtin University of Technology. He has had a career in geochronological

research beginning with his PhD studies at the ANU under Bill Compston, followed by post docs at Caltech

with Lee Silver and at the ETH with Marc Grünenfelder. Then spent seven years in charge of the isotope

geology laboratory at the Scottish Universities Research and Reactor Centre in east Kilbride, returning to the

ANU for three years and then to the Curtin University of Technology. Presently interests include the timing

of events and processes involved in the early evolution of the Earth and the Moon.

Isotopic Composition of the Sun

Authors:

Trevor Ireland1*, Martin Asplund1,2 1 Research School of Earth Sciences, ANU, [email protected]

2 Research School of Astronomy and Astrophysics, ANU, [email protected] *Corresponding Author: [email protected]

Abstract:

To understand isotopic systems in the solar system, the composition of the Sun must be determined. Oxygen is notable as there is a 5% range in 18O/16O and 17O/16O due primarily to mixing of a 16O-rich reservoir in the early solar system with isotopically normal (terrestrial) oxygen. Two popular models for the solar isotopic composition have been identifed. A normal composition is suggested by scaling in the solar system where increasingly large bodies (asteroids to Mars and Earth) show a similar 16O abundance. Alternatively, refractory inclusions from the early solar system with elevated 16O abundance are interpreted as solar condensates. We determined solar oxygen isotopic composition by two means. Firstly, we measured the isotopic composition of oxygen implanted into Fe-metal grains that have little intrinsic oxygen. Secondly, we measured oxygen isotopes from the solar photosphere by observational means. The oxygen isotopic composition measured from the lunar grains is enriched in 17O and 18O by 5.3 (±0.3)% relative to terrestrial oxygen. This is in good agreement with our new measurement of the solar photosphere that indicates !

18O=+4 (±6) %. The relatively large errors are consistent with a normal (terrestrial) oxygen isotopic composition, but do not support a 16O-rich composition for the Sun. These observations suggest that the bulk protonebular oxygen isotopic composition differs from the composition of the residual planetary system. Such a situation will arise if there is a difference in isotopic composition between the dust and gas of the primordial molecular cloud. While the planetary system is wholely sourced from the dust component, the Sun obtains a substantial fraction of its oxygen from carbon monoxide gas. The dust brings the refractory element inventory to the Sun, hence CI chondrites are a good representation of the solar abundances of the non-volatile elements.

Short-lived radionuclides: stellar sources and early solar system chronology

Authors:

David R. Nelson School of Physical Sciences

Curtin University of Technology GPO Box U1987, Perth, Australia, 6000

[email protected]

Abstract:

Investigations of short-lived (half-lives "100 Ma) radioactive decay systems in meteorite, terrestrial and lunar samples have enabled establishment of a remarkably detailed chronology of early condensation, accretion and planetary differentiation events in our solar system. Short-lived radionuclides have also been detected in 3 Ma-old deep-sea sediments; such radioactive fallout from space may have played a significant rôle in Earth’s mass extinction and climate history. Radiogenic decay products of #12 short-lived radionuclides have been identified within primitive meteorites, affirming that a stellar nucleosynthesis event occurred #2 Ma of onset of formation of our solar system and may have triggered its formation. The nature of the last stellar source that contaminated our solar system’s precursor molecular cloud with freshly synthesized elements may be inferred from the relative abundance of short-lived nuclides in meteorites. Leading contenders are a thermally pulsing Asymptotic Giant Branch star, a Type Ia or Type II supernova, or a Wolf-Rayet star (a massive star that ends its short life as a supernova). An additional “Galactic Uniform Production” contribution from earlier nucleosynthesis events is also required to account for abundances of longer-lived radionuclides. Nucleosynthesis yields within stars are currently not well constrained, principally due to uncertainties associated with key nuclear reaction rates. Fortunately, yields of several short-lived nuclides and the GUP rate may be determined by direct observation. Recent gamma-ray observations using NASA’s RHESSI and ESA’s INTEGRAL satellites have facilitated refinement of current quantitative stellar nucleosynthesis models of the short-lived nuclides 26Al and 60Fe. Analytical methods developed using the Curtin SHRIMP ion microprobe are currently being applied to determine the abundance ratios of short-lived nuclides that are diagnostic of nucleosynthesis processes within AGB stars and supernovae. This will enable identification of the stellar source of the short-lived nuclides detected within early solar system materials.

Biography – Dr David Nelson

David R. Nelson has an extensive record of innovative research in the application of stable and radiogenic isotopic analytical techniques, documented in more than 150 scientific publications. He is currently Curtin Fellow, John de Laeter Centre of Excellence in Mass Spectrometry and member of staff, Discipline of Applied Physics, Curtin University.

OBSERVATION AND REMOTE SENSING

Probing the Atmosphere of Venus using Infrared Spectroscopy

Author:

Jeremy Bailey Australian Centre for Astrobiology, Macquarie University

[email protected]

Abstract:

The surface and lower atmosphere of Venus is largely hidden from direct view by the dense sulphuric acid clouds that extend up to 70km altitude. During the 1980s Australian astronomer David Allen, using the Anglo-Australian Telescope at Siding Spring, discovered a means of seeing through these clouds by observing the nightside of the planet at near-infrared wavelengths. Through “windows” at certain infrared wavelengths it is possible to see thermal radiation from the lower atmosphere, and surface. This makes it possible to study the atmospheric composition and properties in regions that would be hard to reach using in-situ probes because of the extreme temperatures and pressures. This Australian developed technique is now being exploited by the ESA Venus Express spacecraft, now in orbit around Venus. We are also using this technique for continued studies of Venus from the Anglo-Australian Telescope using its new infrared spectrometer IRIS2. I will present some of the latest results from our ground-based observations of Venus and show how infrared observations can be used to probe different levels of the Venus atmosphere, and how they can complement the data obtained by Venus Express. We are using the data to study the composition of the atmosphere near the surface, to study the composition and circulation of the cloud layers, and to follow the highly variable oxygen airglow emission, which provides a probe of upper atmosphere chemistry and dynamics.

Biography - Dr Jeremy Bailey

Jeremy Bailey is the Associate Director of the Australian Centre for Astrobiology at Macquarie University, Sydney, and leads a research group that studies the atmospheres and surfaces of planets using remote-sensing techniques and atmospheric modelling. He is originally from the UK, and has previously worked at the Anglo-Australian Observatory and the Joint Astronomy Centre, Hawaii. He represented Australia at the recent NASA Exploration Strategy workshop in Washington DC.

The Desert Fireball Network: An All-Sky Camera Network in the Western

Australian Nullarbor

Authors:

P.A. Bland1, A.W.R. Bevan2, P. Spurny3, and T. McClafferty4

1 Department of Earth Science and Engineering, Imperial College London, SW7 2AZ. 2 Department of Earth and Planetary Sciences, Western Australian Museum, Perth, WA 6000. 3 Ondrejov Observatory, Astronomical Institute, Academy of Sciences of

the Czech Republic, 251 65 Ondrejov. 4 Western Australian Museum, Kalgoorlie-Boulder, 17 Hannan Street Kalgoorlie, WA 6433. e-mail [email protected]

Abstract:

Introduction: There are over 30,000 meteorites in collections world-wide. Although we can analyse these samples to gain clues to the origins of our Solar System, we only have an approximate knowledge of where most meteorites come from: only 8 meteorites have known orbits. Spectroscopic surveys reveal a diversity of asteroids, each with a distinct inferred surface mineralogy. Meteorite collections sample at least 135 different compositional types. An expanded collection of meteorite orbits would allow us to relate some samples to specific regions within the asteroid belt, providing us with a spatial context for interpreting meteorite composition. Methodology: Camera networks, designed to observe fireballs, calculate orbits, triangulate fall positions, and recover meteorites, have been established in several northern-hemisphere nations in the past, and have logged over 40 years of operation. Although hundreds of fireballs associated with large (>100 gram) meteorites were observed, only 3 samples were recovered (the orbit of 5 others, were constrained from amateur video). The poor success rate is due to the location of the networks, as vegetation makes looking for small meteorites extremely difficult. Until now, no camera network has been established in an area, such as a desert, where meteorites can be recognised easily. Projected results: Since late 2005 an autonomous fireball camera network has been established in the Nullarbor of Western Australia. Three satellite monitored cameras designed to operate in deserts have been developed and deployed. Orbits are calculated from fireballs, and meteorite fall positions (over an area of approximately 400,000 km2) are determined for later recovery. Data from a prototype camera operating over a two year period indicates that 10-12 meteorite falls may be detected per year. In the sparsely vegetated Nullarbor, we would expect to recover around 4 new meteorites per year. This will dramatically increase the number of meteorites with known orbits.

Mars Express High Resolution Stereo Camera: results of observations of

north Tyrrhena Terra, Mars

Authors:

Graziella Caprarelli1-2*, Monica Pondrelli3, Stefano Di Lorenzo3, Lucia Marinangeli3, Gian Gabriele Ori3, Gerhard Neukum4

1 Department of Environmental Sciences, University of Technology, Sydney. PO Box 123, Broadway, NSW 2007, Australia. 2 Computational Research Support Unit, Faculty of Science, University of Technology, Sydney. PO Box 123, Broadway, NSW

2007, Australia. 3 International Research School of Planetary Sciences, Università d’Annunzio, Viale Pindaro 42, 65127 Pescara, Italy

4 Institut für Geologische Wissenschaften, Freie Universität Berlin, Malteserstrasse 74-100, 12249 Berlin, Germany * Corresponding Author: [email protected]

Abstract:

Details of the Martian surface are revealed by satellite imagery and altimetry. Interpretations in the context of the evolutionary history of Mars are dependent on imagery and altimetry resolution. Various satellite imagery datasets yield different resolutions. The ESA Mars Express High Resolution Stereo Camera (HRSC) is a multiple scanner instrument that provides high resolution orthorectified imaging (~ 25 m per pixel) and altimetry (DTM) data. HRSC data fill the gap between high resolution small footprints MOC narrow angle (1.4-5 m/pixel), and low resolution large swath imagery THEMIS IR (100 m/pixel) and MOC wide angle data. THEMIS visual images (18 m/pixel) have comparable resolution to the HRSC data, but their coverage is scattered. The HRSC good resolution and large data coverage provides a favorable combination to study flat and apparently featureless areas, including north Tyrrhena Terra. Our study area extends from 0° to 2°S and from 110°E to 112°E, covering about 104 km2. The most outstanding element is the transition between a highly cratered surface and a flat smooth surface, already visible in earlier Viking imagery. We carried out observations of the transition using HRSC data, choosing from orbits h0962 and h0951 suitable transects. We processed raw data using the HRSC processing software developed in VICAR environment, and analysed resulting 2D and 3D images by ArcGIS desktop. Where available, MOC narrow angle images were overlaid and rectified on the HRSC maps, to show fine textural details. We identified subtle morphological and structural features consistent with fissure eruption of lava and crustal extension. By relative chronology based on surface morphologies, we reconstructed a timeline for the complex sequence of volcano-tectonic events, culminating in lava flooding all low elevation areas. Further studies in neighboring areas are under way and will add fundamental knowledge to our understanding of the broad planetary evolution of Mars.

Using Mars Global Surveyor and Mars Odyssey telemetry to reconstruct the

volcano-tectonic history of Phaethontis region, Mars

Authors:

Erin M. Anania 1*, Graziella Caprarelli

1-2, Michael Lake

2, Stefano Di Lorenzo

3

1 Department of Environmental Sciences, University of Technology, Sydney. PO Box 123, Broadway, NSW 2007, Australia.

2 Computational Research Support Unit, Faculty of Science, University of Technology, Sydney. PO Box 123, Broadway, NSW 2007, Australia.

3 International Research School of Planetary Sciences, Università d’Annunzio, Viale Pindaro 42, 65127 Pescara, Italy * Corresponding Author: [email protected]

Abstract:

Detailed mapping of the surface of planets helps to establish models of planetary evolution, providing clues to the evolution of the solar system. Mars has been extensively studied using satellite data. The Phaethontis region of Mars has so far been poorly investigated. Our study aims to fill the gap by focusing specifically on volcanic and tectonic features of Phaethontis, that are particularly impressive in this region. In the MOLA reference map Phaethontis lays in quadrant MC-24, and is centered at 48ºS, 210ºE. We use Mars Odyssey THEMIS visual data and Mars Global Surveyor MOLA (altimetry) and MOC Narrow angle data to describe geological units, crater and relative chronology, and to carry out a detailed morphometric analysis. The collected evidence and its interpretation allows us to define the geological history of Phaethontis, and to relate it to that of the proximal and much studied Tharsis region. MOLA, MOC and THEMIS data are processed using Integrated Software for Imagers and Spectrometers (ISIS), and referred to the Mars IAU 2000 ellipsoid prior to their input into ArcGIS desktop for study and analysis. Morphological features are identified and described, and geometry and abundance of key topographic elements is measured. Spatial analysis is carried out to determine the statistics of the identified features. Crater chronology is also based on outputs from the statistical analysis. 3D analysis allows us to determine topographic evolution. Results from the morphological description, the morphometric analysis, and the crater chronology are synthesized in geological maps of the surface. Our investigation identified subtle volcanic features and a complex tectonic history, comprising two separate episodes of extension and one compressional episode, age-defined by continuous cratering. Interpretation of the volcano-tectonic features is the last step in the study and relates to the broader crustal evolution of the southern hemisphere of Mars.

OUTREACH

New hi-tech virtual reality tool opens access to ‘science in the making’ to students

and the public

Authors:

Oliver, C.A, Australian Centre for Astrobiology, Macquarie University, North Ryde, NSW 2109. E-mail: [email protected]

Fergusson, J., Macquarie ICT Innovations Centre, Macquarie University, North Ryde, NSW 2109. E-mail: [email protected]

Geoffrey Bruce, NASA Learning Technologies, NASA Ames Research Center, Moffet Field, California, USA. E-mail: [email protected]

Tom Gaskins, NASA Learning Technologies, NASA Ames Research Center, Moffet Field, Calfornia, USA. E-mail:

[email protected]

Abstract:

In June/July, 2005, an international field trip to a key Mars analog site, the Pilbara in Western Australia, served to create and inform a new addition to a suite of virtual ‘lenses’ and tools, developed by NASA, aimed at students and the public. The result was Virtual Field Trip tool, co-developed between NASA and Macquarie University in Sydney, and launched on the NASA portal on May 23, 2006, together with a dedicated Pilbara Wiki site, and a US Public Broadcasting System (PBS) and NASA TV documentary made by the New Jersey-based production company Passport to Knowledge. A team of educators and communicators, including the Passport to Knowledge documentary TV crew, joined 30 geologists, microbiologists, geochemists and other experts in a field trip aimed at establishing the degree of certainty to which 3.5 billion year-old stromatolite structures found in the Pilbara could be considered the earliest evidence of life on Earth. The NASA-Macquarie University Pilbara Education Project captures ‘science in the making’ during the field trip. It uses the Virtual Field Trip tool, and employs other ‘lenses’ and tools already developed by NASA Learning Technologies, including World Wind, Virtual Lab and What’s the Difference?. In addition the Pilbara Wiki site at http://pilbara.mq.edu.au supports data searching and basic background information. It is normally accessed via the Virtual Field Trip tool but can also be found via the Australian Centre for Astrobiology’s website http://aca.mq.edu.au. Widespread use of the Internet combined with access to inexpensive, but very powerful, desktop computing makes these technological visualisations freely accessible to all. The project is now going to field testing with high schools, with an eventual possible outcome that the tools will be linked together and accessed via World Wind.

Biography – Carol Oliver

Carol Oliver is a science communicator and the Assistant Director (Management and Outreach) of the Australian Centre for Astrobiology at Macquarie University in Sydney. She holds a research Masters in Science Communication from Central Queensland University and is in the final year of her communications doctorate with Macquarie University entitled ‘Communicating Astrobiology in Public’. She is a passionate advocate for a higher levels of science literacy among a broad range of audiences, including high school students, general public and science policy makers. The role of emerging hi-tech visualisation and interpretation tools in space exploration are key in making science more accessible to all, and she is part of a core team of four that developed and recently completed the NASA-Macquarie University Pilbara Education Project under a Space Act Agreement between the two institutions. Carol is active in all these areas in the international arena, both in her job and as a corresponding member of the International Academy of Astronautics where she is a member of its Commission VI (social sciences) and chairs the Future Directions in Education Study Group. She is also chair of the Public Outreach Working Group for the Australian Academy of Science National Space Science Committee’s Decadal Space Plan. Carol also engages in conference and workshop organization. She chaired the Local Organising Committee for the International Astronomical Union’s ‘Symposium 213 Bioastronomy 2002: Life Among the Stars’ held on Hamilton Island on the Barrief Reef, co-chaired the ‘Fulbright Symposium: Science Education in Partnership’ held in tandem with the Bioastronomy, and is on the Science Organising Committee for the Bioastronomy 2007 to be held in Puerto Rico. Carol finds herself involved in a range of other projects related to life in the universe. Her favourite remains being instrumental in getting a SETI experiment on the Parkes 64-metre radio telescope in New South Wales in 1998, and hopes to make Southern SERENDIP the forerunner of another long-term - but larger - SETI project in Australia sometime in the near to medium future.

EDUCATION & OUTREACH WITH THE MARS ROVER MISSION

Authors:

Glen Nagle Canberra Deep Space Communication Complex (CDSCC) at Tidbinbilla

[email protected]

Abstract:

The journey of the Mars Exploration Rovers has not only been exciting for scientists, but has also captured the public imagination. Billions of hits to the Mars Rover’ and related websites have shown that as humans we have not lost our fascination, nor our curiosity for exploration and discovery. Each new image, and every new clue about Mars and its meaning for the possibilities for life away from our planet, draws the public to the internet and facilities such as the Canberra Deep Space Communication Complex (CDSCC). The Mars Exploration Rovers not only a tool for the scientists, they can be a tool for educators to use to excite and teach students about the possibilities that await them in the future. The Rovers are simple explorers, acting as our legs, arms and eyes on another planet. Robotic geologists studying the rocks and soils of Mars. The students in school today (K-12) are the generation that will one day walk on Mars. Educators have an enormous responsibility to encourage them to consider such possibilities. Glen Nagle will illustrate and discuss the successes experienced at the CDSCC in educating students and the public about Mars and space through the eyes and instruments of the two NASA Rovers, and through simple objects such as rocks.

Biography – Mr Glen Nagle

Glen Nagle is the Education & Outreach Manager for the Canberra Deep Space Communication Complex (CDSCC) at Tidbinbilla. The Complex is a part of NASA’s Deep Space Network, giant antenna ‘dishes’ providing two-way communication support to dozens of spacecraft exploring the Solar System and beyond. His role is responsible for education programs seen by 70,000 members of the public each year, including 8,000 students on excursions. Glen has been involved in space science education and the promotion of space exploration for over 25 years. He has worked in a number of related fields, including science publishing, space industry advocacy, and as a commentator on space in the media. Outside his work at the CDSCC, Glen hosts a weekly TV program on ABC2 – ‘Skywatch’ - and features as a regular guest on many national and commercial radio stations.

Victorian Space Science Education Centre: An Exciting New Facility for

Science Education

Authors:

Mathers N, Pakakis M and Spencer P Victorian Space Science Education Centre

Abstract:

The Victorian Space Science Centre (VSSEC) is a AU$6.4 million facility in Melbourne, established to provide students and teachers with access to state of the art equipment, exciting and stimulating programs and continuous professional development within a new and exciting environment. Scenario-based programs, including a Mission to Mars and a Mission to the Space Station, are used to stimulate student’s enthusiasm for maths, science and technology across a broad range of topics and demonstrate their relevance and applications. VSSEC has established associations in both education and research with national and international organisations such as ESA, NASA, CSIRO, the Bureau of Meteorology, Universities and industry. These associations provide the highest level of support to direct, focus and extend the breadth of the curricula and in so doing deliver a blended learning environment giving support to the learner and the teacher. The involvement of universities and industry also demonstrates the relevance of space science beyond the classroom and potential career paths for students. Unlike the trend of edutainment space camps and centres, VSSEC’s programs are integrated into the school curriculum to provide an innovative and unique comprehensive learning experience using space as the vehicle to inspire, thus demonstrating the relevance and importance of space science and increasing the level of science expertise in the community.

Biography – Ms Naomi Mathers

Naomi Mathers joined the Victorian Space Science Education Centre (VSSEC) team at the beginning of

2006 from RMIT University where she was completing a PhD in Aerospace Engineering. Naomi has spent

many years combining her work in space structures with her passion for education. This included the

establishment of the RMIT Space Science Expo and participating in the Space Education and Awareness

Working Group of the Asia Pacific Regional Space Agency Forum (APRSAF) for the past two years. Naomi

has been working with VSSEC in an advisory capacity for a number of years and is excited to be joining the

team as a Research Scientist and Curriculum Development Officer.

COMMERCIALISATION

Authors:

Space Industry Intellectual Property Management:

Rules and A Roadmap of Rising Relevance

William N. Hulsey III

Principal, HULSEYIP Intellectual Property Lawyers, P.C.

Senior Research Fellow, IC2 Institute, University of Texas at Austin 1250 S. Capital of Texas Highway, Building 3, Suite 610

Austin, Texas 78746 [O] 512-7951295/[F]512-233-2602

[email protected]/www.HulseyIPLaw.com

Abstract:

Today, two different segments of the aerospace industry are becoming increasingly apparent: commercial space and privatized space. NASA’s Crew Exploration Vehicle, the U.S.’ Exploration Vision and similar international efforts, on the one hand, require the commercial space industry to develop new technologies for the Crew Exploration Vehicle and supporting systems. On the other hand, technology demands for private space vehicles (e.g., SpaceShipTwo and its progeny) are emerging in the nascent privatized space industries of space tourism, space manufacturing, and other non-governmental and non-NASA efforts. These growing areas of industrial development are receiving greater investments for research and development (R&D), resulting in accelerated space industry innovation and invention. Entities investing in such R&D will require patent and other intellectual property (IP) protection for the results they achieve. Because engineers, technology managers, and business leaders in these areas are the major stakeholders in such developments, a need arises for their understanding the rules of engagement in this IP-rich business environment. This presentation addresses these rules and provides a roadmap to help these major stakeholders succeed in today’s commercial and privatized space industries.

PROGRESS REPORT & WORKSHOP

INAUGURAL DECADAL PLAN FOR SPACE SCIENCE: PROGRESS REPORT

Authors:

Peter L. Dyson (1,2) , Iver H. Cairns (2,3) and the National Committee for Space Science (2)

(1) Department of Physics, La Trobe University, VIC 3086, Australia; [email protected]

(2) Australian Academy of Science, http://www.science.org.au/natcoms/ss-decadal.htm; [email protected]

(3) School of Physics, University of Sydney, NSW 2006, Australia; [email protected]

Abstract:

The National Committee for Space Science, chartered by the Australian Academy of Science, is in the process of developing the first Decadal Plan for Space Science in Australia. The purview is of the science, industry, and government needs associated with solar system phenomena and objects. The primary emphasis is on science associated with solar terrestrial physics, space weather, atmospheric forcing, remote sensing, and planetary science (including astrobiology). The focus is on Australian needs and benefits, but within a global context. The first stage of the process, viz. providing “strawman” science aims and projects and soliciting initial submissions, was completed early this year (see the web page at http://www.physics.usyd.edu.au/~ncss) and currently the detailed plan is being formulated through a steering committee and a number of working groups. The goals of this talk are to describe the current status and motivations for the Decadal Plan, and to discuss the scientific aims and projects of the draft Plan in the context of Australia’s needs, and the capabilities that could be developed for Australia, in space-related technologies.

Biography – Professor Peter Dyson

Professor Peter Dyson is in the Department of Physics at La Trobe University where he developed the B. Space Science degree. He has over thirty years experience in solar terrestrial and space weather research using HF radar, optical and satellite techniques. His specific research interest is geospace, the interface between the Earth’s environment and interplanetary space. Currently he leads the Australian Tasman International Geospace Environment Radar (TIGER) project that is a component of the Super Dual Auroral Radar Network (SuperDARN) that spans both Polar Regions and studies space weather phenomena. He uses the FedSat GPS receiver for tomographic studies of the plasmasphere and has optical instruments in Antarctica to study the aurora and other space weather features.

PANEL

New Space Missions and Instruments

This panel will provide an introduction to the "New Space Missions and Instruments working group" of the Decadal Plan for Space Science. The working group is soliciting ideas and concepts for consideration, and already has a number of proposals. Our panel of experts will discuss the type of instruments and missions that are desired by the Australian space science community, the resources necessary to carry out said missions, and the challenges of arranging support in an Australian context.

Confirmed Panelists: • DANIEL FABER - Panel Chair. Spacequest Canada • Professor PETER DYSON - Decadal Plan committee. Latrobe University • ROGER FRANZEN - Auspace • Dr ANDREW PARFITT - UniSA Institute For Telecommunications Research. Former • CRC-SS Director. • Dr ANDREW BELL – COMDEV (USA)

Biography – Daniel Faber

Daniel Faber is an engineer and protagonist in the micro-space and new-space sectors of the aerospace industry. His career has covered all aspects of space missions, from mission analysis and marketing to electronics assembly and spacecraft integration. Mr Faber operated the cutting-edge Canadian MOST space telescope, and was the systems engineer on the world's smallest astronomy satellites – the series of 5 kilogram BRITE nanosatellite. His recent engineering work at Spacequest Canada has involved power management electronics, data networks for large spacecraft and attitude control sensors and actuators. Having grown up in Tasmania, Daniel founded the BLUEsat project at the University of New South Wales and became a director of the National Space Society of Australia. He is the current president of the Canadian Space Society and a founding member of the Canadian Space Chamber of Commerce. He is also involved in a number of entrepreneurial new-space companies pushing the bounds of launch technology and nuclear fusion.

national space society of australia - nssa home behalf of the national space society of australia...

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