Invited speakers:
Pawel Artymowicz, StockholmObs., Sweden
Mailing Address: Stockholm Observatory, SCFAB, SE-106 91 Stockholm, Sweden
E-Mail:
Alan Boss, CIW, DTM, USA
Mailing Address: 5241 Broad Branch Road, NW, Washington, DC20015-1305U.S.A.
E-Mail:
Adam Burrows, U. Arizona, USA
Mailing Address: Department of Astronomy, University of Arizona, Tucson, AZ85721USA
E-Mail:
Mark Harrison, RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Ray Jayawardhana, U. Michigan, USA
Mailing Address: University of Michigan Astronomy Department, 953 Dennison Building, Ann Arbor, MI48109-1090USA
E-Mail:
Laurie Leshin, Arizona State U., USA
Mailing Address: Arizona State University Department of Geological Sciences, Box 871404, Tempe, AZ85287-1404USA
E-Mail:
Doug Lin, UC Lick Observatory, USA
Mailing Address: UCO/Lick Observatory, University of California, Santa Cruz, CA95064USA
E-Mail:
Jonathan Lunine, LPL, AZ, USA
Mailing Address: LPL,1629 E. University Blvd., Tucson, AZ85721-0092USA,Office location: Space Sciences 522
E-Mail:
Kevin McKeegan, UCLA, USA
Mailing Address: Dept. of Earth & Space Sciences, UCLA, 595 Young
Drive, Los Angeles, CA. 90095-1567 USA
E-mail:
Frank H. Shu,National Tsing Hua U., Taiwan
Mailing Address: NationalTsingHuaUniversity 101, Sec. 2, Kuang Fu Road, Hsichu30013, Taiwan, R.O.C.
E-Mail:
Chris Tinney, Anglo-Australian Obs., Australia
Mailing Address: PO Box 296, Epping 1710 Australia
E-mail:
Contributed talks:
Francis Albarede, Ecole Normale Sup. de Lyon, France
Mailing Address:Ecole Normale Supérieure de Lyon 46, Allee d'Italie 69364 Lyon Cedex 7, France
E-Mail:
Yuri Amelin, Geological Survey of Canada
Mailing Address: Geological Survey of Canada, 601 Booth St., Ottawa, ON, Canada, K1A 0E8
E-Mail:
Jeremy Bailey, AAO, Australia
Mailing Address: Anglo-Australian Observatory, PO Box 296, Epping,
NSW 1710
E-mail:
Victoria C. Bennett, RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Mike Bessell, RSAA, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-Mail:
Brad Carter, U. of Southern Queensland, Australia
Mailing Address: Centre for Astronomy, Solar Radiation and Climate, Department of Biological and Physical Sciences, Faculty of Sciences, University of Southern Queensland, ToowoombaQueensland 4350, Australia
E-Mail:
Geoff Davies, RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Ulyana Dyudina, RSAA, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-mail:
Justin Freeman, RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Andrew Glikson,RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Karl E. Haisch Jr., U. Michigan, USA
Mailing address: Dept. of Astronomy, Univ. of Michigan, 830 Dennison Bldg., Ann Arbor, Michigan48109-1090 USA
E-mail:
Masahiko Honda, RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Trevor Ireland, RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Ing-Guey Jiang, Astronomy, National Central U., Taiwan
Mailing Address: Institute of Astronomy, NationalCentralUniversity, No. 300, Jungda Rd, JungliCity, Taoyuan, Taiwan 320, R.O.C.
E-Mail:
Warrick Lawson , UNSW@ADFA, Australia
Mailing address: School of PEMS/Physics, UNSW@ADFA, Canberra ACT 2600
E-mail:
Kurt Liffman, CSIRO and Monash U., Australia
Mailing Address: Energy & Thermofluids Engineering, CSIRO/MIT P.O. Box 56, Graham Rd, Highett VIC 3190 AUSTRALIA
E-mail:
Charley Lineweaver, UNSW, Australia
Mailing Address: School of Physics, University of New South Wales, Sydney, NSW 2052
Email:
Sarah Maddison, Swinburne U., Australia
Mailing Address: Centre for Astrophysics and Supercomputing, School of BSEE, Swinburne University of Technology, PO Box 218, Hawthorn, 3122 Victoria, Australia
E-Mail:
Rosemary Mardling, CSPA, Monash U., Australia
Mailing Address: School of Mathematical Sciences, MonashUniversity, 3800
E-mail:
Franklin Mills, RSPhysSE,ANU, Australia
The Research School of Physical Sciences and Engineering, Building 60, ANU Campus, Canberra ACT 0200
E-Mail:
Louis Moresi, Monash U., Australia
Mailing address: School of Mathematical Sciences Building 28, MonashUniversity, Clayton 3800, Victoria, Australia
E-mail:
James Murray, Swinburne U., Australia
Mailing Address: Centre for Astrophysics and Supercomputing, SwinburneUniversity of Technology, PO Box 218, HawthornVictoria 3122, Australia
E-Mail:
Marc Norman,RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Allen Nutman, RSES,ANU, Australia
Mailing address: ResearchSchool of Earth Sciences, AustralianNationalUniversity, Canberra, ACT 0200, Australia
E-mail:
Andrew Prentice, Monash U., Australia
Mailing Address: Room 329, Building 28, School of Mathematical Sciences, MonashUniversity Vic 3800, Australia
E-Mail:
Penny D. Sackett, RSAA, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-Mail:
Thomas Sharp, Arizona State U., USA
Mailing Address: Arizona State University Department of Geological Sciences, Box 871404, Tempe, AZ85287-1404USA
E-Mail:
Therese Schneck, Consulting Civil Engineer,France
Mailing Address: 11/13 Rue Lobineau 75006 Paris
E-Mail:
Robert G. Smith,UNSW@ADFA, Australia
Mailing Address: School of Physical, Environmental & Mathematical Sciences, University of New South Wales at The AustralianDefenceForceAcademy, Canberra, ACT 2600
E-mail:
Dave Stegman. Mathematical Sci., Monash U., Australia
Mailing Address: School of Mathematical Sciences, MonashUniversityBuilding 28 Victoria 3800 Australia
E-Mail:
Ross Taylor, Geology, ANU, Australia
Mailing Address: Geology Department, The AustralianNationalUniversity, Canberra 0200 ACT Australia
E-Mail:
Mark Wardle, Macquarie U, Australia
Mailing Address: Department of Physics, MacquarieUniversity, Sydney NSW 2109
E-mail:
David Wark, MonashU., Australia
Mailing Address: School of Geosciences, Building 28 Monash UniversityVictoria 3800,Australia
E-Mail:
Peter Wood, RSAA, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-Mail:
Chris Wright, ADFA@UNSW, Australia
Mailing Address: School of Physical, Environmental & Mathematical Sciences, University of New South Wales at The AustralianDefenceForceAcademy, Canberra, ACT 2600
E-Mail:
Li-Chin Yeh, National Hsinchu Teachers College, Taiwan
Mailing Address: Department of Mathematics, NationalHsinchuTeachers College, Hsin-Chu, Taiwan
E-mail:
Williaml Zealey,U. of Wollongong, Australia
Mailing Address: Faculty of Engineering, University of Wollongong, Wollongong, NSW2500
E-mail:
Students:
Daniel Bayliss, MSO, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-mail:
Adrian Brown, Macquarie U, Australia
Mailing address: Dept of Earth and Planetary Sciences, Macquarie Uni, NSW 2109
E-mail:
Andres Carmona,ESO Garching.,Heidelberg U., Germany
Mailing Address: European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei Muenchen, Germany
E-mail:
Marie Gibbon, Monash U., Australia
Mailing Address: 42 Park Street, Seaford Vic 3198
E-mail:
Antti Kallio, RSES, ANU, Australia
Mailing Address: RSES, Building 61, The AustralianNationalUniversity, Canberra ACT 0200 Australia
E-Mail:
Gareth Kennedy, Monash U., Australia
Mailing Address: 2/33 Golf Links Ave, Oakleigh, Vic, 3166
E-mail:
A-Ran Lyo, UNSW@ADFA, Australia
Mailing address: School of PEMS/Physics, UNSW@ADFA, Canberra ACT 2600
E-Mail:
Marco M. Maldoni, UNSW@ADFA, Australia
Mailing address: School of PEMS/Physics, UNSW@ADFA, Canberra ACT 2600
E-Mail: .
Charles Morgan, Monash U., Australia
Mailing Address: School of Mathematical Sciences, MonashUniversity, Clayton, Vic. 3800
E-mail:
Craig O'Neill, U. Sydney, Australia
Mailing Address: The School of Geosciences, Department of Geology and GeophysicsEdgeworthDavidBuilding F05, The University of Sydney, NSW 2006
Dr. John Patten, Unaffiliated Student, Australia
Kala Perkins, SRES, ANU, Australia
Postal Address: School of Resources, Environment and Society, AustralianNationalUniversity, Canberra 0200 Australia
E-Mail:
Tamara Rogers, U. Santa Cruz, USA
Mailing Address: 5350 S. Morning Sky Ln, Tucson, AZ. 85747
E-mail:
Raquel Salmeron, U. Sydney, Australia
Mailing Address: School of Physics A28, University of Sydney, NSW 2006, Australia
E-Mail:
Patrick Scott, MSO, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-Mail:
Christine Thurl, MSO, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-Mail:
Miguel de Val Borro, Stockholm U., Sweden
Mailing Address: StockholmUniversity, AlbaNovaCenter, Department of Astronomy, 10691 Stockholm
E-mail:
David Weldrake, RSAA, ANU, Australia
Mailing Address: MountStromlo Observatory, Cotter Road, Weston, ACT 2611, Australia
E-Mail:
Abstracts
Yuri Amelin (1), Alexander Krot (2) and Eric Twelker (3)
1) Geological Survey of Canada
2)Hawaiian Institute of Geophysics and Planetology, SOEST, University of Hawaii at Manoa,
3)Juneau
Duration of the chondrule formation interval: a Pb isotope study
Chondrules are among the earliest solid objects that formed in the solar system.
We have determined the ages of chondrules from several carbonaceous chondrites using the Pb-Pb isochron method. High precision Pb isotope dates are obtained for three silicate clasts (large chondrules) from the CBa (Bencubbin-like) chondrite Gujba. Additional analyses of chondrules from the CV3 chondrite Allende allowed to improve precision of the age. The summary of precise Pb-Pb ages of chondrules from primitive chondrites is shown below:
MeteoritePb-Pb isochron age, MaComment
Allende (CV3)4566.7±1.0this study
Acfer 059 (CR2)4564.7±0.7Amelin et al. (2002)
Gujba (CBa)4562.7±0.5this study
From these data, we deduce that the period of chondrule formation started simultaneously with, or shortly after the CAI formation [4567.2±0.6 Ma (Amelin et al., 2002)], and continued for at least 4.0±1.5 m.y. If the dates of the chondrules reflect their timing of formation, then there were probably a variety of processes occurring over at least 4-5 m.y. that we now combine under the umbrella name of "chondrule formation". More high-precision Pb-Pb and extinct nuclide dating, as well as geochemical and petrologic studies of chondrules from primitive meteorites, will be required to understand individual processes of chondrule formation.
Pawel Artymowicz
Stockholm Univ
Migration of bodies in disks: Timescales and unsolved problems
Solid bodies with size ranging from dust to planets are present in protoplanetary disks, with which they couple via processes involving gas drag, radiation pressure, and gravitational torques of several types (due to Lindblad and corotational resonances). As a result, several size-dependent migration modes exist, operating on timescales shorter than the lifetime of the disks. Theory of migration studies the role of mobility in accumulation of solids, origin of the orbital distance distribution of extrasolar planets, and the ring-like appearence of some circumstellar dust disks. This talk presents an overview of the underlying physics, timescales, and the outcomes of migration in the scenarios of planetary system formation. We discuss in some detail a newly discovered, fast migration mode of protoplanets (timescale ~1000 yr), dependent on corotational torques (tentatively named type III).
Jeremy Bailey
AAO
Evolution of Terrestrial Planet Atmospheres
Time when the process started in the solar system: -4.5 byr
Time when it ended: still continuing
The planets Venus, Earth and Mars have developed very different atmospheres over 4.5 billion years of evolution, although we suspect that their early atmospheres may have been quite similar. Mars has a very thin (7 mbar) and dry atmosphere of mostly CO2. The Earth's 1 bar atmosphere is predominantly nitrogen and oxygen with very low CO2 content, and Venus has a 90 bar atmosphere of mostly CO2 in which a runaway greenhouse effect has heated the planets surface to 720K. I will review some of the processes which have operated on the three planets to control the evolution of their atmospheres, and discuss issues including the "early faint Sun" problem, "snowball Earth" events and the rise of oxygen in the Earth's atmosphere.
Jeremy Bailey (1,2), Sarah Chamberlain (2), Malcolm Walter (2) and David Crisp (3)
(1)AAO
(2)Australian Centre for Astrobiology, MacquarieUniversity
(3)Jet Propulsion Laboratory, Caltech
Poster: IR Observations of Mars during the August 2003 opposition
We present some preliminary results of observations obtained during the very favourable opposition of Mars in August 2003 using the UIST instrument on the United Kingdom Infrared Telescope (UKIRT) at Mauna Kea, Hawaii. We obtained narrow band images which we believe are probably the sharpest ever obtained with a ground-based telescope, as well as spectral scans of the disk at a range of near-IR wavelengths and resolving powers. The observations include absorption features due to atmospheric gases, CO2 ice at the south pole, and water ice clouds in the north. We can use the CO2 band strength to image the distribution of surface atmospheric pressure and hence topography.
The data may be used to search for absorption features due to hydrated clay minerals, carbonates and sulphates which might provide evidence for the past presence of surface water.
Jeremy Bailey (1), Phil Lucas (2), Jim Hough (2) and Motohide Tamura (3)
(1)AAO & Australian Centre for Astrobiology, MacquarieU.
(2)University of Hertfordshire
(3)National Astronomical Observatory, Japan
Poster: Direct Detection of Extrasolar Planets by Polarimetry
Despite the detection of more than 100 extrasolar planets by the radialvelocity method, no extrasolar planet has yet been seen directly by its emitted or reflected light. Detections by spectroscopic techniques have so far been unsuccessful while photometric detection requires accuracies which are beyond current ground-based photometry.
However, we believe that planets orbiting close to their stars (Hot Jupiters) might be detected by means of the polarization of the light scattered from their atmospheres. While the resulting polarization of the combined light of the planet and star is small, polarization measurements can in principle be made with very high sensitivity since polarimetry is adifferential measurement and is not limited by the stability of the Earth's atmosphere as photometry is.
We have designed and built a stellar polarimeter which should be capable of achieving the required sensitivity. The instrument is now being tested, and on a 4m or larger telescope should be capable of detecting the polarization signature of bright hot Jupiter systems such as Tau Boo, Upsilon And or 51 Peg.
Daniel Bayliss, Ulyana Dyudina and Penny Sackett
RSAA, ANU, Australia
Modeling of Reflected Light from Extra Solar Planets with Eccentric Orbits
An extra solar planet will shine by reflecting light from its parent star. As the planet orbits the star the amount of light reflected will vary as the phase of the planet changes with respect to the observer, resulting in a light curve with a periodicity equal to the orbital period of the planet. We model the reflected light from extra solar planets at different phases based the reflective properties of Jupiter and Saturn obtained by the Pioneer space probes. Since a large proportion of the known extra solar planets display highly elliptical orbits, our models include changes in angular velocity and orbital distance resulting from such elliptical orbits. Current Earth based photometry is limited to a precision of about 100ppm of the parent's stars luminosity due to atmospheric extinction. However, new space photometers such as MOST and Kepler, are expected to have precisions down to less than 10ppm. At these new sensitivities the light curves from many known extra solar planets should be detectable. These light curves should give us information not only on the size and orbital properties of the planet, but also on atmosphericparticle size, cloud cover, and the presence of rings. We discuss the likelihood of these properties being extracted from the light curves with the data from space and earth based instruments in the next 5-10 years.
Alan Boss
Carnegie Institution
The Formation of Giant Planets
[All times relative to formation of the protosun and solar nebula]
Time core accretion started: 0 MyrError bar: 0 Myr
Time core accretion finished: 5 MyrError bar: 2 Myr
Time disk instability started: 0 MyrError bar: 0.1 Myr
Time disk instability finished: 0.1 MyrError bar: 0.1 Myr
Two very different mechanisms have been proposed for the formation of the gas and ice giant planets. The conventional explanation forthe formation of gas giant planets, core accretion, presumes that a gaseous envelope collapses upon a roughly 10 Earth-mass, solid core that was formed by the collisional accumulation of planetary embryos orbiting in the solar nebula. The more radical explanation,diskinstability, hypothesizes that the gaseous portion of the nebula underwent a gravitational instability, leading to the formation ofself-gravitating clumps, within which dust grains coagulated and settledto form cores. Core accretion appears to require several million years or more to form a gas giant planet, implying that only long-lived disks would form gas giants. Disk instability, on the other hand, is so rapid (forming clumps in thousands of years), that gas giants could form in even theshortest-lived disks. Core accretion has severe difficulty in explaining the formation of the ice giant planets, unless two extra protoplanets areformed in the gas giant planet region and thereafter migrate outward.
Recently, an alternative mechanism for ice giant planet formation has been proposed, based on observations of protoplanetary disks in the Orion: disk instability leading to the formation of four gas giant protoplanets with cores, followed by photoevaporation of the disk and gaseous envelopes of the protoplanets outside about 10 AU by a nearby OB star, producing ice giants. In this scenario, Jupiter survives unscathed, whileSaturn is a transitional planet.
Adrian Brown
Dept of Earth and Planetary Sciences, MacquarieUniversity
Evidence for the earliest Hydrothermal System on Earth in the East Pilbara Granite-Greenstone Terrane
Time when the process you describe started in the solar system: 3.45 Gy
The error bar on the start time: 100 My
Time when this process ended: 3.46
The error bar on the end time: 100 My
The East Pilbara Granite Greenstone Terrane is a well preserved Archaean succession of domical granite batholiths surrounded by thick greenstone synclinoria. The North Pole Dome region in postulated to be a granite dome predominantly covered by greenstones of the Warrawoona Group. Following intrusion of the granite and eruption of the felsic Panorama Formation around 3.45 Gya, it is hypothesized that a hydrothermal event took place, utilising the felsic magma conduits to propel water to the palaeosurface, thereby creating an epithermal hydrothermal deposit at Miragla Creek. The alteration caused by this event is in the process of being mapped using airborne hyperspectral sensing as part of a three year PhD project. It provides an opportunity to examine one of the earliest hydrothermal events in the history of the Earth.
The 600 sq. km hyperspectral dataset was captured in October 2002 and covers the wavelengths from 400 to 2400 nm at 5m resolution. Mapped litholgies so far include sericite, chlorite and pyrophyllite alteration zones, along with a serpentine-rich komatiite flow at the base of the Apex Basalt. These will be discussed and implications of the event, including its possible links with putative stromatolite structures within the 3.42 Gyr Strelley Pool Chert, which overlies the Panorama Formation.