C e n t r e f o r P l a n e t a r y S c i e n c e s 5
th
S u m m e r M e e t i n g 25 June 2015 Programme and Abstracts The Centre for Planetary Sciences at UCL/Birkbeck is delighted to welcome you to our fifth
annual summer meeting, which is being held on Thursday 25 June 2015 in UCL’s Front Quad
marquee.
Centre for Planetary Sciences Summer Meeting 2015
Programme
10:30 – 11:00
Arrivals / Coffee
Posters
11:00 – 11:15
Prof. Steve Miller
UCL Physics and Astronomy
Introduction; Europlanet Rides Again
11:15 – 11:45
Prof. Andrew Coates
Mullard Space Science Laboratory
Keynote: Updates from MSSL Planetary Science:
PanCam for ExoMars2018; The field-aligned
potential near Titan; and Ion pickup observed at
comet 67P with the Rosetta Plasma Consortium
11:45 – 12:00
Prof. Hilary Downes
Birkbeck Earth & Planetary Sciences
Dr Louise Alexander
Birkbeck Earth & Planetary Sciences
A bit of granite from another planet (maybe Mars?)
Dr Laura McKemmish
UCL Physics and Astronomy
Dr Nick Achilleos
UCL Physics and Astronomy
Effective discrimination of Apollo 12 basalts with
small sample sizes
Predicting Liquid-Vapour Phase Diagram of
MgSiO3 by First-Principles Molecular Dynamics
Simulation
What you need to know to use the ExoMol Line
Lists for Studying Exoplanetary Atmospheres
Modelling the Compressibility of Saturn's
Magnetosphere
Lunch
Posters
Jennifer Harris
Birkbeck Earth & Planetary Sciences
Dr Roberto Scipioni
UCL Earth Sciences
Dr Geraint Jones
Mullard Space Science Laboratory
Prof. Hilary Downes
Birkbeck Earth & Planetary Sciences
Prof. Graziella Branduardi Raymont
Mullard Space Science Laboratory
Quantitative spectral analysis of hydrothermal
deposits in Nili Patera, Mars
A Model for the Electronic conductivity of SiO2 at
extreme conditions
15:00 – 15:15
Coffee / Tea
Posters
15:15 – 15:30
Dr Pete Grindrod
Birkbeck Earth & Planetary Sciences
15:30 – 15:45
Amy Edgington
UCL Earth Sciences
15:45 – 16:00
Dr Anne Wellbrock
Mullard Space Science Laboratory
16:00 – 16:15
Prof. Ian Crawford
Birkbeck Earth & Planetary Sciences
The science case for Lunar Mission One
16:15 – 16:30
Dr Eliot Sefton-Nash
Birkbeck Earth & Planetary Sciences
ExoMars 2018 Rover Candidate Landing Sites: The
Aram Dorsum inverted channel and Hypanis Vallis
deltaic system
16:30
Wine reception
12:00 – 12:15
12:15 – 12:30
12:30 – 12:45
12:45 – 13:00
13:00 – 13:45
13:45 – 14:00
14:00 – 14:15
14:15 – 14:30
14:30 – 14:45
14:45 – 15:00
Dr Bing Xiao
UCL Earth Sciences
Directly-detected electron beams near Enceladus
Iron silicides in the Solar System
SMILE: Solar wind Magnetosphere Ionosphere Link
Explorer
Searching for Co-Seismic Displacement on Mars
through Sub-Pixel Image Co-Registration and
Correlation
The Properties of FeSSi and its Implications for
Mercury’s Core
Heavy negative ions observed during Cassini’s Titan
T16 flyby using the CAPS Electron Spectrometer
(ELS)
ORAL ABSTRACTS
Europlanet Rides Again
Prof. Steve Miller (s.miller@ucl.ac.uk)
Department of Physics and Astronomy, UCL
Barring any last, last (no, really, last) minute hitches, Europlanet will be funded once more as
a European Research Infrastructure (RI) in planetary science, a four-year project starting in
September 2015. Once more, the Centre for Planetary Sciences will play a key role in this
endeavour, now known as Europlanet 2020 RI. The CPS will contribute to creating a virtual
observatory for planetary science and a new "planetary space weather" service. It will lead
the project's efforts to generate real impact, particularly with industrial partners. And it will
run several networking and training events, including at least one workshop teaching
researchers how to use the Regional Planetary Information Centre, housed in the CPS offices
in UCL's Kathleen Lonsdale Building.
Keynote: Updates from MSSL Planetary Science: PanCam for
ExoMars2018; The field-aligned potential near Titan; and Ion pickup
observed at comet 67P with the Rosetta Plasma Consortium
Prof. Andrew Coates (a.coates@ucl.ac.uk)
Mullard Space Science Laboratory
The PanCam instrument for the ExoMars 2018 rover: science objectives and
instrument characteristics
A.J. Coates (1,2), A.D. Griffiths (1,2), C.E. Leff (1,2), R. Jaumann (3), N. Schmitz (3), J.-L.
Josset (4), G. Paar (5), M.Gunn (6), C.R. Cousins (7), and the PanCam team
The scientific objectives of the ExoMars 2018 rover are designed to answer several key
questions in the search for life on Mars. The PanCam instrument will set the geological and
morphological context for the mission. Here, we will describe the PanCam scientific
objectives in geology, atmospheric science and 3D vision. We will also describe the design of
PanCam, which includes a stereo pair of Wide Angle Cameras (WACs), each of which has a
filter wheel, and a High Resolution Camera for close up investigations. The cameras are
housed in an optical bench and electrical interface is via the PanCam Interface Unit (PIU).
We also discuss some results from PanCam testing during field trials.
A new upper limit to the field-aligned potential near Titan
A.J. Coates (1,2), A. Wellbrock (1,2), J.H. Waite (8), G.H. Jones (1,2)
Neutral particles dominate regions of the Saturn magnetosphere and locations near several of
Saturn’s moons. Sunlight ionizes neutrals, producing photoelectrons with characteristic
energy spectra. The Cassini CAPS electron spectrometer has detected photoelectrons
throughout these regions, where photoelectrons may be used as tracers of magnetic field
morphology. They also enhance plasma escape by setting up an ambipolar electric field, since
the relatively energetic electrons move easily along the magnetic field. A similar mechanism
is seen in the Earth’s polar wind and at Mars and Venus. Here, we present a new analysis of
Titan photoelectron data, comparing spectra measured in the sunlit ionosphere at ~1.4 Titan
radii (RT) and at up to 6.8 RT away. This results in an upper limit on the potential of 2.95 V
along magnetic fields lines associated with Titan at up to 6.8 RT, which is comparable to
some similar estimates for photoelectrons seen in Earth’s magnetosphere.
Ion pickup observed at comet 67P with the Rosetta Plasma Consortium (RPC):
similarities and differences with AMPTE releases
A.J. Coates (1,2), J.L. Burch (8), R. Goldstein (8), H. Nilsson (9), G. Stenberg Wieser (9), E.
Behar (9) and the RPC team
Since Rosetta’s arrival at comet 67P in August 2014, the Rosetta Plasma Consortium particle
instruments have shown that the low activity cometary environment is dominated by the solar
wind. This was expected in the early stages of the mission. In addition to the solar wind and
related He+ populations, a low energy pickup ion population is seen intermittently in the
early phase of the mission near the comet. The population is very time dependent, but at
times reaches higher energy approaching the solar wind energy. During these intervals, ICA
composition data indicate that the ions constitute a ‘spring’ of water group ions. The rising
energy signatures of these ions observed at times indicate that they are in the early phases of
the pickup process. Here, we compare these exciting pickup ion measurements with Giotto
measurements at the relatively weak (compared to Halley) comet Grigg-Skjellerup, where
early phase pickup was seen as non-gyrotropic cometary ions and with the AMPTE lithium
and barium releases. We find some striking similarities with the AMPTE releases,
particularly the early pickup signature (e.g. during the lithium release) and a momentum
balance between the pickup ions and the deflected solar wind (e.g. during a barium release).
In an AMPTE lithium release there was also evidence for less momentum being given to the
solar wind alpha particles than to the protons – another remarkable feature observed with IES
at 67P. Here we summarise the early measurements related to ion pickup from RPC, compare
them with the earlier relevant data, and discuss the similarities and differences in the ion
pickup physics.
(1) Mullard Space Science Laboratory, University College London, UK, (2) Centre for Planetary Science at
UCL/Birkbeck, UK, (3) German Aerospace Centre (DLR), Institute of Planetary Research, Berlin, Germany, (4)
Space Exploration Institute, (SPACE-X), Neuchâtel, Switzerland, (5) Joanneum Research, Graz, Austria, (6)
Computer Science Department, Aberystwyth University, UK, (7) Department of Earth and Environmental
Sciences, University of St Andrews, UK, (8) Southwest Research Institute, San Antonio, Texas, USA, (9) Swedish
Institute of Space Physics, Kiruna, Sweden.
A bit of granite from another planet (maybe Mars?)
Beard, A.D.1, Downes, H.1 and Chaussidon M.2
(h.downes@ucl.ac.uk)
1.
UCL/Birkbeck Centre for Planetary Sciences, and Department of Earth and Planetary
Sciences, Birkbeck, Malet Street, London, WC1E 7HX, UK.
2.
Institute of Physics of the Globe, 1 Rue Jussieu, Paris, France
The Earth is the only planet in the solar system in which granitic rocks are abundant. We
have discovered a microgranitic clast in an interior chip of EET 87720, a brecciated meteorite
known to contain numerous foreign rock fragments. The clast consists of a complex blebby
intergrowth of a pure SiO2 mineral (identified as tridymite) and albite feldspar, mantling a
single larger zoned oligoclase feldspar crystal (identified as an earlier-crystallising phase).
The intergrowth and the larger oligoclase crystal share a common margin, suggesting that the
clast was originally part of a larger fragment. An estimate of its bulk chemical composition is
equivalent to that of a granite (77 wt.% SiO2). Patches of high-Si K-bearing glass occur
interstitially within the granite clast; they have high concentrations of SO3 (11-12 wt.%) and
contain Cl (0.6 wt.%). This suggests that the clast formed on a volatile-rich parent body,
similar to Mars. The mean oxygen isotope composition of the feldspar and tridymite in the
clast is very different from the oxygen isotope compositions of samples from the Earth or
Moon, but shows some similarity to the oxygen isotope fractionation trend for brecciated
Martian meteorites.
Effective discrimination of Apollo 12 basalts with small sample sizes
L. Alexander1,2, J. F. Snape2,3, K. H. Joy4, I. A. Crawford1,2, and H. Downes1,2.
(l.alexander@bbk.ac.uk)
1
Department of Earth and Planetary Science, Birkbeck College, University of London, UK
(l.alexander@bbk.ac.uk) 2Centre for Planetary Sciences at UCL-Birkbeck, London. 3
Department of Geosciences, Swedish Museum of Natural History, SE-104 05 Stockholm,
Sweden. 4SEAES, University of Manchester, Manchester, UK.
Introduction: Mare basalt samples provide us with information on the composition of the
Moon’s upper mantle. However, often only small amounts of material are available for
analysis, which can result in significant errors in interpretation of analyses [1]. The ability to
classify small samples using non-destructive methods is of primary importance since gramsized quantities of material are all that are likely to be returned by future robotic sample
missions [2]. This talk compares new and previously published analyses [3, 4, 5], obtained
for the Apollo 12 olivine, ilmenite, pigeonite and feldspathic lava suites with basaltic soil
samples analysed as part of a study on basaltic diversity at the Apollo 12 site, in order to
investigate how they can be distinguished.
Methods: major and minor element mineral analyses for the feldspathic basalt sample 12038,
the ilmenite basalt samples 12022 and 12063 and new data for basaltic fines from the soil
sample 12070,889 were obtained using a JEOL JXA-8100 electron microprobe wavelength
dispersive system (WDS) with an Oxford Instruments INCA energy dispersive system (EDS).
Backscattered electron images and elemental X-ray maps were used to identify mineral
phases. Trace element analyses in mineral phases were obtained by laser ablation inductively
coupled plasma mass spectrometry (LA-ICP-MS), using an Agilent 7700X ICP-MS and a
New Wave Research UP-213 laser.
Results: Olivine: Olivine is the most useful discriminator as it can be used to calculate the
equilibrium parent melt Mg# (atomic Mg/[Mg+Fe]) and hence identify the basalt type [3, 5].
This will also indicate whether the bulk chemistries of samples are likely to be representative
of their parent rocks [3, 5]. Ti/V ratios in lunar olivine have previously been shown to be
useful discriminators, providing samples have cooled rapidly and are fine-grained [3, 5, 6].
Ilmenite: It is possible to separate olivine basalts from the other A12 groups based on MgO
concentration in ilmenite. Ilmenite in pigeonite, ilmenite and feldspathic basalts have <2 wt%
MgO. Several basaltic samples studied here have higher ilmenite MgO contents than
previously analysed Apollo 12 samples. Sample 12003,308_5A is similar to ilmenite basalts
[3], but its ilmenite MgO contents (5.2–5.6 wt%) are much higher than all other ilmenite
basalts apart from the unrepresentative partial cumulate sample, 12005 [7].
Plagioclase: Variation of plagioclase An# with Mg# highlights some important differences in
crystallisation trends between different samples. It has previously been suggested [3, 5] that
samples 12023,155_4A, 155_5A and 12003,314_D were similar in terms of their bulk
chemistry, textures and major element mineral chemistries to the Apollo 12 feldspathic basalt
12038 [3, 5]. However, they show significant differences in plagioclase crystallisation trends
and chemistry [8] and it is therefore less likely that these basaltic fines originated from the
same parent lava flow.
Pyroxene: It is possible to calculate parent melt compositions by inverting trace element data
for primitive pyroxene core compositions. However, care needs to be taken to sample true
core compositions from unequilibrated samples and to use suitable distribution coefficients
for this purpose. We use the method of [9, 10] to reconstruct parent melts for basaltic samples
since this takes into account the changes in composition of the pyroxene phases. We have
tested this method by applying it to Mg-rich pyroxene cores in two ilmenite basalts (samples
12022 and 12063) and the feldspathic basalt sample 12038 and comparing the results with
published data of bulk rock compositions for those samples, which are in good agreement.
Conclusions: Olivine major and minor element chemistry has been shown to be the most
effective at discriminating between basalt types [3, 5], but where olivine is not present,
pyroxene can be used to recalculate parent melt compositions in unequilibrated samples.
Ilmenite and plagioclase chemistries can also help to indicate differences in parent melt as
well as to identify cumulate samples.
References: [1] Neal, C.R. et al., (1994) Meteoritics 29, 334-348. [2] Zolensky, M.E. et al., (2000) Meteoritics
& Planet. Sci., 35, 9-29 [3] Snape, J.F. et al., (2014) Meteoritics & Planet. Sci., 49, 842-871. [4] Keil, K., et al.,
(1971) LPSC Vol 2, 319 [5] Alexander, L. et al. (2014) Meteoritics & Planet. Sci., 49, 1288-1304. [6] Fagan,
A.L. et al., (2013) GCA, 106, 429-445. [7] Dungan, M.A., and Brown, R.W. (1977) LPSC Vol 8, 1339-1381.
[8] Alexander, L. (2015) PhD Thesis. [9] Sun, C., and Liang, Y., (2012) Contrib. Mineral. Petrol. 163: 807–
823. [10] Sun, C., and Liang, Y., (2013) GCA, 119, 340-358
Predicting Liquid-Vapour Phase Diagram of MgSiO3 by First-Principles Molecular
Dynamics Simulation
Bing Xiao, Lars Stixrude
(b.xiao@ucl.ac.uk)
Department of Earth Sciences, UCL
Many crucial details about vaporization of MgSiO3 at high temperature are not well
investigated both in experiments and theoretical aspect. The liquid-gas phase diagram of
MgSiO3 can be a very valuable piece of information to have better understanding the
chemical compositions of hot gas in the big impact or even those atmospheres of exoplanets.
Here, we use first principles molecular dynamics (FPMD) simulation to predict the vapourliquid phase diagram of MgSiO3. The phase boundary is calculated by using Gibbs dividing
surface method. It is found that the critical temperature of such vapour-liquid binary system
is situated between 6000 K and 7000 K. The chemical compositions of vapour below 6000 K
can be recognized using bond lengths and coordination numbers as the criteria. We
discovered small molecules such as SiO, O2, [O] and [Si] are the dominant species in vapour
below 5000 K. Mg related species are rare below the same temperature. Meanwhile, above
5000 K, MgO, [Mg] and atomic clusters such like SiO2, SiO3, MgSiO3 and MgSiO2 are
formed in the gas. Our current results are compared to a calculation using thermodynamic
model implemented in MAGMA code [B. Fegley Jr and A.G.W. Cameron, 1987] for
MgSiO3.
What you need to know to use the ExoMol Line Lists for Studying
Exoplanetary Atmospheres
Dr Laura McKemmish
(l.mckemmish@ucl.ac.uk)
Department of Physics and Astronomy, UCL
ExoMol has made a name in producing high quality, complete high-temperature line lists for
a wide variety of astrophysically relevant molecules, including biomarkers. These line lists
(specifying the frequency and intensity of absorption lines in molecules) are used in complex
atmospheric models to predict absorption based on temperature, pressure, atmospheric
composition and other factors. But what if your observed spectrum doesn’t match your
model? Have you used the wrong input parameters? Is the atmospheric model wrong? Or is
the underlying line list wrong?
As a producer of line lists in the ExoMol group, I can help you answer the last question. I will
tell you how we produce these line lists and, most importantly, where we expect errors to
occur and where they will not occur (as well as tell you about what sort of errors and their
magnitude). For example, if you are looking at water absorption around 3000 cm-1, then the
line lists will be near perfect. Looking at VO at 17,000 cm-1 (in the visible) - not so much.
Why? I will tell you what molecules, parameters and spectral regions are easy for us to study,
and which are difficult, and why this is the case. I will explain where experimental data is
critical, the accuracy with which different input parameters can be calculated by ab initio
theory, and how experiment and theory can be used together to build a more complete picture
of the spectroscopy of molecules.
And, if nothing else, you should come to my talk to hear why the ExoMol group talks (and
thinks) in cm-1.
Modelling the Compressibility of Saturn's Magnetosphere
N. Achilleos (1,2), C. S. Arridge (6), P. Guio (1,2), N. M. Pilkington (1,2), A. Masters (4), N.
Sergis (5), A. J. Coates (3,2), M. K. Dougherty (4)
(nicholas.achilleos@ucl.ac.uk)
(1) Department of Physics and Astronomy, University College London, Gower St., London, WC1E 6BT, (2)The
Centre for Planetary Sciences at UCL/Birkbeck, Gower St., London, WC1E 6BT, (3) Mullard Space Science
Laboratory, Department of Space and Climate Physics, University College London, Dorking, UK, (4) Blackett
Laboratory, Imperial College London, London, UK. (5) Academy of Athens, Office of Space Research &
Technology, Athens, Greece. (6) Department of Physics, Lancaster University, Lancaster, UK
Work presented by Pilkington et al. (e.g. AGU 2014) shows observational evidence that
Saturn's magnetopause may be significantly affected by variations in the beta parameter of
the outer magnetospheric plasma, as well as by variations in solar wind dynamic pressure. In
order to model the influence of these two physical parameters on magnetospheric
compressibility, we construct magnetostatic models of the dayside magnetosphere of the
planet using the UCL Magnetodisc Model in 'Saturn mode'. For different values of hot
plasma beta, which span the observed range at Saturn, we construct a model power law
expressing the relation between magnetopause standoff distance and solar wind dynamic
pressure (assumed to be equal to total magnetic plus plasma pressure at the model's outer
boundary). We comment on the behaviour of the magnetospheric compressibility and scale
according to: (1) The response of the magnetopause location to changes in solar wind
dynamic pressure at fixed plasma beta; and (2) The response of the system which ensues
when plasma beta varies at fixed solar dynamic wind pressure.
Quantitative spectral analysis of hydrothermal deposits in Nili Patera,
Mars
Harris, J.K.1,2, Crawford, I.A.1,2, Cousins, C.R.3
(jennifer.harris@bbk.ac.uk)
1
UCL/Birkbeck Centre for Planetary Sciences, 2 Birkbeck University of London, Department
of Earth and Planetary Sciences, 3 University of St Andrews, Department of Geography and
Geoscience
There is evidence that throughout the history of Mars various regions were temporarily
habitable (Cousins and Crawford, 2011; Martinez-Frias et al., 2006; Schulte et al., 2006;
Ulrich et al., 2012; Westall et al., 2013). In these cases habitability is defined as the
availability of liquid water and an energy source to sustain metabolism. Hydrothermal
systems provide both of these conditions and are also likely to preserve any biofabrics that
may form opening up the possibility of detecting past life (Summons et al., 2011). Evidence
for the existence of extinct hydrothermal systems has been found by both orbital and groundbased campaigns across the martian surface. This evidence has been both structural and
mineralogical. The Nili Patera caldera in the Syrtis Major Planum region of Mars contains a
number of bright patches that have been identified as rich in hydrated silica (Skok et al.,
2010) from Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) hyperspectral
images and interpreted as hydrothermal alteration deposits. To date the mineralogical studies
of this region have been purely qualitative. Spectral Mixture Analysis (SMA) is a field of
techniques that enable quantitative data to be extracted from hyperspectral images. The
optimal combination of SMA algorithms were identified and applied to regions in the Nili
Patera previously identified as containing hydrothermal deposits.
References
Cousins, C.R., Crawford, I.A., 2011. Volcano-ice interaction as a microbial habitat on Earth and Mars.
Astrobiology 11, 695–710.
Martinez-Frias, J., Amaral, G., Vázquez, L., 2006. Astrobiological significance of minerals on Mars surface
environment. Rev. Environ. Sci. Bio/Technology 5, 219–231.
Schulte, M., Blake, D., Hoehler, T., McCollom, T., 2006. Serpentinization and its implications for life on the
early Earth and Mars. Astrobiology 6, 364–76.
Skok, J.R., Mustard, J.F., Ehlmann, B.L., Milliken, R.E., Murchie, S.L., 2010. Silica deposits in the Nili Patera
caldera on the Syrtis Major volcanic complex on Mars. Nat. Geosci. 3, 838–841.
Summons, R.E., Amend, J.P., Bish, D., Buick, R., Cody, G.D., Des Marais, D.J., Dromart, G., Eigenbrode, J.L.,
Knoll, A.H., Sumner, D.Y., 2011. Preservation of martian organic and environmental records: final report of the
Mars biosignature working group. Astrobiology 11, 157–181.
Ulrich, M., Wagner, D., Hauber, E., de Vera, J.-P., Schirrmeister, L., 2012. Habitable periglacial landscapes in
martian mid-latitudes. Icarus 219, 345–357.
Westall, F., Loizeau, D., Foucher, F., Bost, N., Betrand, M., Vago, J., Kminek, G., 2013. Habitability on Mars
from a microbial point of view. Astrobiology 13, 887–97.
A Model for the Electronic conductivity of SiO2 at extreme conditions
R . Scipioni and L. Stixrude
(r.scipioni@ucl.ac.uk)
Department of Earth Sciences, UCL
The electrical conductivity of liquid Silica SiO2 at extreme temperatures and pressures is
investigated with ab initio Molecular dynamics. The conductivity exhibits a maximum at T <
15000 K also observed with the Mott - Ziman formulation. At high pressures structural and
conductivity properties follow the analogous isoelectronic element Ne, at lower temperatures
O-Si charge ordering appears that results in shifts of pseudogaps and Fermi energies. It is
their relative positions that determine the conductivity. Although structural changes occur, no
dissociation is obtained at high temperatures rather a continuous shell/charge reordering
confirmed by a monotonic decrease in heat capacities.
Directly-detected electron beams near Enceladus
G. H. Jones (1,2) and the Cassini CAPS Team
(g.h.jones@ucl.ac.uk)
(1) Mullard Space Science Laboratory, University College London
(2) The Centre for Planetary Science at UCL/Birkbeck
Similarities between Enceladus – an active moon of Saturn with a significant plume
ionosphere – and moons such as Io in the Jupiter system, where a strong electrodynamic
interaction between it and the Jovian magnetosphere was both predicted and subsequently
observed, a similar interaction region was expected to couple Enceladus and the Kronian
magnetosphere. Magnetometer observations reveal the presence and directions of fieldaligned currents, with the northern and southern Alfvén wing’s field-aligned current sheets
crossed. The Cassini spacecraft’s encounters with Enceladus when the Cassini Plasma
Spectrometer, CAPS, was operating, has allowed the direct detection of electron beams in the
moon’s vicinity. Pryor, Rymer, et al. (2011) reported the detection of interaction-associated
particles during the E4 encounter of August 2008: CAPS observed magnetic field-aligned
electrons, whilst the Magnetospheric Imaging Instrument, MIMI, similarly observed ion
beams. In the same work, a corresponding weak, variable auroral spot in Saturn’s ionosphere
at UV wavelengths was reported. Here, we report on the field-aligned electron beams
observed by the CAPS instrument in addition to the first one discovered, and present
interpretations of these beams’ nature that should assist in building a more complete
understanding of this fascinating moon-magnetosphere interaction.
Iron silicides in the Solar System
Prof. Hilary Downes (h.downes@ucl.ac.uk)
UCL/Birkbeck Centre for Planetary Sciences, and Department of Earth and Planetary
Sciences, Birkbeck, Malet Street, London, WC1E 7HX, UK
Abstract not available.
(Prof. Downes has kindly stepped in for Dr Rai - abstract retained below for informationwho unfortunately had to withdraw from the meeting)
Constraints from geochemistry on the provenance of material forming terrestrial
planets: Case study of ureilite meteorites
Nachiketa Rai1,2, Hilary Downes1,2, Caroline L. Smith2 UK
(n.rai@ucl.ac.uk)
1
Centre for Planetary Sciences, Birkbeck-UCL, University of London, Malet Street, London,
WC1E 7HX, UK
2
Natural History Museum, Cromwell Rd, London SW7 5BD, UK
Using oxygen isotope signatures to constrain the building blocks of terrestrial planets has
been a standard approach [1,2]. Ureilite meteorites are ultramafic achondritic meteorites
composed largely of olivine and pyroxenes, that are thought to have been derived as residues
of partial melting within the mantle of a carbon-rich asteroid [3]. These meteorites display a
wide range of oxygen isotope signatures that distinguishes ureilites from other planetary
bodies such as the Earth, Moon and Mars.
We have undertaken modelling to constrain the possible building blocks of the ureilite parent
body (UPB), based on combinations of chondritic meteorites that are considered to be the
building blocks of all terrestrial planetary bodies. We ran simulations trying to find matches
consisting of three and two member combinations from various chondritic meteorite types
that could simultaneously satisfy the oxygen isotope characteristics (D17O, d17O and d18O)
from UPB compositions. Our preliminary results indicate that the oxygen isotope signatures
of the UPB can be reproduced based on chondritic materials as possible building blocks but
this leads to numerous non-unique solutions, which appear equally feasible. We have
improved the model by including elemental ratios (Mg/Si, Al/Si, Fe/Si, Fe/Al), but found that
our models could not reproduce the Fe/Si and Fe/Al ratios unless we take into account a
missing Fe-rich core component. We find that our models also require inclusion of Fe-poor
and Fe-rich chondrules as essential building blocks for the UPB.
References: [1] Lodders & Fegley (1997), Icarus 126 (2), 373-394 [2] Sanloup et al. (1999) Physics of the Earth
and Planetary Interiors 112, 43–54 [3] Mittlefehldt et al. (1998) Mineralogical Society of America. Rev.
Mineral. 36. p. 195.
SMILE: Solar wind Magnetosphere Ionosphere Link Explorer
G. Branduardi-Raymont and the SMILE team
(g.branduardi-raymont@ucl.ac.uk)
Mullard Space Science Laboratory
SMILE is a space mission dedicated to study the interaction of the solar wind with the Earth’s
magnetic field.
SMILE will investigate the dynamic response of the Earth's magnetosphere to the impact of
the solar wind in a unique manner, never attempted before: it will combine soft X-ray
imaging of the Earth's magnetic boundaries and magnetospheric cusps with simultaneous UV
imaging of the Northern aurora. For the first time we will be able to trace and link the
processes of solar wind injection in the magnetosphere with those acting on the charged
particles precipitating into the cusps and eventually the aurora. This is not only a matter of
scientific curiosity; solar-terrestrial interactions have profound practical consequences on our
ever more complex technological infrastructures, in space and on the ground, on human
health and life, and drive what we have come to know as ‘space weather’. Exploring, and
reaching an understanding of what drives space weather, will eventually lead to forecast and
mitigate its effects.
Out of 13 missions originally proposed, SMILE is the one selected by the European Space
Agency (ESA) and the Chinese Academy of Sciences (CAS) for an initial study phase during
this summer, with a final decision for implementation due in Nov. 2015. The mission is
sponsored by both ESA and CAS and the payload is the joint responsibility of European,
Canadian and Chinese institutions, with science support from the USA. The launch is
expected for the end of 2021 and the mission duration is baselined at three years.
Searching for Co-Seismic Displacement on Mars through Sub-Pixel Image
Co-Registration and Correlation
Peter M. Grindrod1, Pieter Vermeesch2, James Hollingsworth3, Francois Ayoub4
(p.grindrod@ucl.ac.uk)
1
Department of Earth and Planetary Sciences, Birkbeck, University of London, UK,
Department of Earth Sciences, UCL, UK, 3Arup, UK, 4Division of GPS, California Institute
of Technology, USA.
2
One of the primary science goals of the InSight mission to Mars is to measure the magnitude,
rate and geographical distribution of internal seismic activity, through the Seismic
Experiment for Interior Structure (SEIS) instrument [1]. Although current seismic levels are
unknown, one of the best candidate regions for ongoing activity is the Cerberus Fossae fault
system, due to the young surface age [e.g. 2] and possible recent Marsquake-triggered
boulder avalanches [3]. Recent advances in optical image correlation through the software
package COSI-Corr have allowed aerial and orbital images to be orthorectified and coregistered with a 1/50 pixel accuracy, allowing the identification of sub-pixel displacements
[4]. This approach has been validated for use with several different geological feature types
and processes, including terrestrial glacier flow [5] and co-seismic displacement [6] as well
as dune and ripple migration on Earth [7] and Mars [8]. Here we report on our preliminary
attempts in searching for co-seismic displacements in the Cerberus Fossae region of Mars,
using Mars Reconnaissance Orbiter HiRISE and CTX images and COSI-Corr. For each study
site, at least three images are required, which represent two different time periods: one stereo
pair taken with little time between images to allow production of a Digital Terrain Model
(DTM), and one temporally-distinct image, taken a long time before or after the stereo pair.
We present our initial results at different resolutions, with recommendations for ongoing and
future studies, particularly potential long baseline methods fusing existing data with stereo
images expected from the CaSSIS instrument [9] onboard the ExoMars 2016 Trace Gas
Orbiter.
References. [1] Dandonneau, P.-A. et al. (2013), LPSC 44, #2006. [2] Keszthelyi, L.P., et al.
(2007), Geophys. Res. Lett., 34, L21206. [3] Roberts et al. (2012), J. Geophys. Res., 117,
E02009. [4] Leprince, S., et al. (2007), IEEE Trans. Geosci. Remote Sens., 45, 1529-1558. [5]
Scherler, D., et al. (2008), Remote Sens. Env., 112, 3806-3819. [6] Hollingsworth, J., et al.
(2012), J. Geophys. Res., 117, B11407. [7] Vermeesch, P., and S. Leprince (2012), Geophys.
Res. Lett., 39, L14401. [8] Bridges, N.N., et al. (2012), Nature, 485, 339-342. [9] Thomas,
N., et al. (2014), 8th Int. Conf. Mars, #1067.
The Properties of Fe-S-Si and its Implications for Mercury’s Core
1
2
1
1
A. Edgington , O. T. Lord , L. Vocadlo , L. Stixrude & I. G. Wood
(a.edgington.12@ucl.ac.uk)
1
1
Department of Earth Sciences, University College London, Gower St., London, WC1E 6BT
and The Centre for Planetary Sciences at UCL/Birkbeck, Gower St., London, WC1E 6BT,
2
School of Earth Sciences, University of Bristol, Bristol.
The structure and composition of the innermost planet remains an elusive puzzle. The
existence of Mercury’s magnetic field, and the observed internal liquid layer [1] suggests a
partially molten core; however, the very high uncompressed density additionally implies a
body highly enriched in metallic iron. Previous studies have considered the addition of
sulphur to the pure iron system, as this has the ability to significantly depress the melting
curve of iron, and possibly allow Mercury’s core to remain molten to the present day [2]. The
presence of sulphur has significant implications for the evolution and dynamics of the
planet’s core, and may result in the existence of iron snow [3]. Recent measurements from
the MESSENGER spacecraft have placed important constraints on the abundance of iron on
Mercury’s surface to be ~ 4 wt% [4]. This suggests that Mercury formed in reduced
conditions, such that sulphur may not be the only light element present, as significant
amounts of silicon could have also dissolved into the core [5]. It follows, then, that to
continue investigating the composition of Mercury’s core, we must next consider a Fe-S-Si
alloy.
In this study we have used a combination of experimental and computational techniques to
study Fe-S-Si with the relative weight percentages 80:10:10, as a possible candidate for the
composition of the interior of Mercury. This composition is consistent with surface
composition measurements [6] as well as lying outside of the measured immiscibility gap for
the Fe-S-Si ternary system [7, 8]. Laser-heated diamond-anvil-cell techniques have been used
to measure the melting curve of Fe-S-Si (at% ratio 80:10:10), extending previous studies of
the Fe-S-Si ternary system [e.g. 7, 8] to Mercury’s central core pressures and beyond up to
~50 GPa. To complement these experiments, ab–initio molecular dynamics calculations are
being performed to determine of the material’s thermodynamic properties up to 4000 K and
40 GPa. These two studies reveal the slope of the melting curve and its adiabatic gradient
respectively, which together may allow insight into the evolution of Mercury’s core.
[1] Margot, J. L. et al. (2007) Science, 316: 710-714
[2] Schubert, G. et al. (1988) in ‘Mercury’ 429-460
[3] Chen, B et al. (2008) Geophys. Res. Lett., 35, L07201
[4] Nittler, L. R. et al. (2011) Science, 333, 1847-1850.
[5] Malavergne, V. et al. (2010) Icarus, 206:199-209
[6] Chabot, N. L. et al. (2014) EPSL, 390:199-208.
[7] Morard, G. & Katsura, T. (2010) Geochim. Cosmochim. Acta, 74:3659-3667.
[8] Sanloup, C. & Fei, Y. (2004) Phys. Earth Planet. Mat., 147: 57-65.
Heavy negative ions observed during Cassini’s Titan T16 flyby using the
CAPS Electron Spectrometer (ELS)
A. Wellbrock1,2, A.J. Coates1,2, G.H. Jones1,2, J.H. Waite3
(a.wellbrock@ucl.ac.uk)
1
Mullard Space Science Laboratory, University College London, UK,
Centre for Planetary Sciences at UCL/Birkbeck, UK
3
Southwest Research Institute, USA
2
One of the unexpected and significant results of the Cassini mission was the discovery of
heavy organic negative ions in Titan’s ionosphere by the CAPS Electron Spectrometer (ELS)
(Coates et al, 2007, Waite et al., 2007). These are observed during every encounter when the
instrument points in the ram direction at altitudes between 950 and 1400 km. The heaviest
ions observed so far have masses up to 13,800 amu/q (Coates et al., 2009). This indicates that
complex hydrocarbon and nitrile chemical processes take place in Titan’s upper atmosphere.
Studying the effects of different controlling parameters on the densities of different negative
ion mass groups helps constrain the chemical formation and destruction processes (Wellbrock
et al., 2013). The highest masses were observed during the T16 flyby. In this paper we
present CAPS-ELS negative ion observations during T16 and discuss possible reasons for the
particularly high masses observed during this encounter, which may include polar and
seasonal effects.
The science case for Lunar Mission One
Prof. Ian Crawford (i.crawford@ucl.ac.uk)
Department of Earth and Planetary Sciences, Birkbeck
Lunar Mission One (LM1) is an innovative proposal for a robotic mission to the South Pole
of the Moon (for background see http://lunarmissionone.com/). In December 2014 the project
successfully secured funding of approximately 1 million USD from a total of 7297 private
and corporate backers, and the project has now moved into a detailed planning phase.
In this talk I will outline the key science drivers for LM1. A key component of the LM1
science case is the proposal to drill to a depth of 20-100m below the lunar surface, something
that has never been attempted before. By emplacing scientific instruments at an as yet
unexplored location, and extracting and analyzing samples from deep below the surface, LM1
will address a number of high-priority lunar science questions. These are focused mainly on
the search for, and characterization of, volatiles at the lunar poles, and on the geology of the
giant South Pole-Aitken impact basin. There may also be opportunities to conduct lowfrequency radio astronomy from the lunar surface.
If successful, LM1 will help pave the way for future human and robotic exploration of the
Moon, while at the same time demonstrating an innovative funding model for future space
exploration.
ExoMars 2018 Rover Candidate Landing Sites: The Aram Dorsum inverted channel
and Hypanis Vallis deltaic system
Elliot Sefton-Nash1, M. Balme2, S. Gupta3, P. Grindrod1, P. Fawdon2, J. Davis4, P.
Sidiropoulos5, V. Yershov5 & J-P. Muller5 (e.sefton-nash@ucl.ac.uk)
1. Dept. of Earth and Planetary Sciences, Birkbeck, University of London, UK.
2. Dept. of Physical Sciences, The Open University, Milton Keynes, UK.
3. Dept. of Earth Science & Engineering, Imperial College, London, UK.
4. Dept. of Earth Sciences, University College London, UK.
5. Mullard Space Science Laboratory, University College London, UK.
The search for life on Mars is a cornerstone of international solar system exploration. In
2018, the European Space Agency will launch the ExoMars Rover to further this. The key
science objectives of the ExoMars Rover are to: 1) search for signs of past and present life on
Mars; 2) investigate the water/geochemical environment as a function of depth in the shallow
subsurface; and 3) to characterise the surface environment. ExoMars will drill into the subsurface to look for indicators of past life using a variety of complementary techniques,
including assessment of morphology (potential fossil organisms), mineralogy (past
environments) and a search for organic molecules and their chirality (biomarkers). The
choice of landing site is vital if the objectives are to be met.
Our UK consortium led proposals for two of the four high priority sites that remain under
consideration, Aram Dorsum and the Hypanis Vallis delta. The Aram Dorsum site in western
Arabia Terra is situated about half way between Meridiani Planum and Mars’ dichotomy
boundary, where Arabia Terra meets the northern lowlands. Aram Dorsum itself is a flattopped, branching, sinuous ridge-like feature that we interpret to be a former fluvial channel
system that has been preserved in positive relief by differential erosion. The Hypanis fluvial
deltaic system lies in northern Xanthe Terra, also on Mars’ dichotomy boundary. Our
Hypanis study area includes fluvio-deltaic deposits at the termini of Hypanis Vallis and
Sabrina Vallis. At Hypanis, fine-scale layering and multiple depositional lobes imply longterm delta activity producing continual or recurring low-energy depositional environments.
Broadly, we assess our candidate landing sites by maximizing potential rover science return
while adhering to strict engineering constraints. We analyse hyperspectral data to infer
mineralogy, crater size frequency distributions to infer surface age and visible, thermal and
topographic data to perform geologic mapping. For both sites, there is geomorphological and
mineralogical evidence for sustained or recurring aqueous activity. Low-energy deposition in
delta or channel marginal units may have concentrated any potential biosignatures
transported from upstream fluvial systems. Crater size frequency distributions indicate
ancient origins, but recent surface exposure ages, which implies long-term protection of
potential science targets from the surface environment for much of Mars’ history.
Consequently, we interpret both sites to have a high preservation potential for any biomarkers
emplaced in potentially habitable depositional settings. This presentation will focus on the
most recent results and conclusions from our work. Detailed analysis of both sites by the UK
consortium will support their science and engineering cases to be presented at the Third
Landing Site Selection Workshop, currently scheduled for October 2015.
POSTER ABSTRACTS
Characterisation of a potential landing site in the lunar South Pole region
H. Irfan1,2, I. A. Crawford1,2, P. M. Grindrod1,2, D. De Rosa3 and J. D. Carpenter3
(huma.irfan.09@ucl.ac.uk)
1
Department of Earth and Planetary Sciences, Birkbeck, University of London, Malet Street,
London, WC1E 7HX, UK 2Centre for Planetary Sciences, UCL/Birkbeck, London, WC1E
6BT, UK. 3European Space Agency, Estec, Keplerlaan 1, 2200 AG, Noordwijk ZH, The
Netherlands.
Figure 1. Lunar South Polar region, potential landing site of interest.
Introduction: The objective of this study is the detailed investigation and characterisation of
a potential landing site of interest in the lunar South Pole, which is being conducted in
collaboration with the European Space Agency (ESA). A prospective region of ~30 x 40 km,
centred at 82.7°S, 33.5°W (Fig. 1) is being examined for these studies, which is located on
the western limb of the Scott crater in the lunar South Pole, this location has been highlighted
previously as an example of a possible site of interest in light of the Russian Luna-Resurs
mission. The aim is to investigate and characterise smaller sub-sites of ~3 x 3 km within this
locality that satisfy the criteria for the landing site selection, which take into account a risk
assessment perspective and proximity to the scientifically interesting features that include:
favourable illumination conditions, safe topography, technical constraints for spacecraft
landing precision, and a proximity to the scientifically significant features which hint of a
possible presence of volatiles and/or water ice and any latent scientifically interesting
mineralogy.
The lunar South Pole is a scientifically interesting region for future landing missions, within
which, cold regions containing crater cold-traps have been suggested by the Diviner Lunar
Radiometer Experiment data surface-temperature observations, where the temperatures can
reach as low as 38 K in the permanently shadowed regions. It is thought that within these
crater cold-traps, cryogenically trapped water ice and/or volatiles of a primitive origin may
have been derived from impacts and believed to have been preserved for billions of years.
Suitable temperatures for volatile stability may also be found in the subsurface in some
illuminated areas. In the light of these observations and assumptions, the site considered for
this study presents interesting possibilities which are being investigated in detail in this study.
Datasets and Methodology: For a comprehensive analysis of this region and the sub-sites
within it, various lunar remote sensing datasets have been utilised to ascertain the merit of the
potential landing site based on the aforementioned criteria. NASA’s Moon Mineralogy
Mapper (M3) hyperspectral data aboard the Chandrayaan I are used to investigate the
scientifically important volatiles and mineralogy in the region using the Envi software. The
Lunar Orbiter Laser Altimeter (LOLA) datasets, Lunar Reconnaissance Orbiter Camera
(LROC) Narrow Angle Camera (NAC) images, USGS Integrated Software for Imagers and
Spectrometers (ISIS), ArcGIS and The NASA Ames Stereo Pipeline (ASP) software are used
to process datasets and generate Digital Terrain Models (DTMs). Hazard maps including
crater and boulder size-frequency distributions, slope and roughness maps are also generated
using the ArcGIS software.
Characteristics of Jupiter’s auroral acceleration region
L. C. Ray, J. Gustin, D. Grodent
(licia.ray@ucl.ac.uk)
Department of Physics and Astronomy, UCL
Jupiter’s dynamic auroral region is the signature of magnetosphere-ionosphere coupling. The
magnetospheric drivers of the emission are relatively well understood, yet the high-latitude
characteristics of the interaction have not been measure in-situ. Ahead of Juno’s arrival next
summer, we use HST STIS observations of Jupiter’s auroral emission to infer the location of
Jupiter’s auroral acceleration region and the properties of the precipitating auroral electrons.
We analyze two images of Jupiter’s northern emission, determining the precipitating electron
energy and incident energy flux for the main aurora, Io spot, Ganymede footprint, and flare
regions. The resulting relationships between energy flux and electron precipitation energy for
the main auroral emission are compared to the theoretical relationship derived by Lundin &
Sandahl [1978] for a range of auroral region locations, and temperatures and densities
appropriate for the jovian system.
Jupiter’s thermospheric winds and energy budget
L.C. Ray, N. A. Achilleos, S. Miller
(licia.ray@ucl.ac.uk)
Department of Physics and Astronomy, UCL
When the Galileo probe entered Jupiter’s equatorial atmosphere, it confirmed high
thermospheric exobase temperatures of ~900 K, about 700 K higher than what was expected
from solar EUV heating. A prime candidate to explain the high temperatures is the transport
of auroral energy equatorwards from high latitudes. However, the combination of strong
Coriolis forces from the rapid planetary rotation rate, coupled with ion drag from
magnetosphere-ionosphere coupling, results in an ‘ion drag fridge’ effect (Smith et al., 2007),
which acts to transport auroral energy poleward, rather than equatorward. This additional
energy input from the magnetosphere-ionosphere-thermosphere coupling inflates the polar
thermosphere. One of the mechanisms that balances this heating is cooling via H3+ infrared
emission. We use the UCL JASMIN model (Jovian Axisymmetric Simulator with
Magnetosphere, Ionosphere, and Neutrals), which includes the effects of auroral precipitation
heating, H3+ cooling, ion drag, Joule heating and the transport of energy via thermal winds in
order to characterize the global energy budget of the jovian thermosphere.
Photoelectrons at Enceladus
S. A. Taylor1,2; A. J. Coates1,2, G. H. Jones1,2, A. Wellbrock1,2
(s.taylor.14@ucl.ac.uk)
1
Mullard Space Science Laboratory, University College London, UK
2
Centre for Planetary Sciences at UCL/Birkbeck, UK
The Electron Spectrometer (ELS) of the Cassini Plasma Spectrometer (CAPS) measures
electrons in the energy range 0.6-28,000 eV with an energy resolution of 16.7%. ELS has
observed photo- electrons produced in the plume of Enceladus. These photoelectrons are
found during Enceladus encounters in the energetic particle shadow where the spacecraft is
shielded from penetrating radiation by the moon [Coates et al., 2013]. Observable is a
population of photoelectrons at _ 20-30 eV, which are seen at other bodies in the solar system
and are usually associated with ionisation by the strong solar He II (30.4 nm) line. We have
identified secondary peaks detected by ELS which are also interpreted as a warmer
population of photoelectrons created through the ionisation of neutrals in the E-Ring. We
have noted differences in the relative intensities of these peaks dependent on the geometry of
the encounter and whether the spacecraft passes through the plume. We have begun
comparing the observations with models of photoelectron production spectra to try and
explain how the plume materials may directly contribute to these photoelectron populations.
References
Coates, A. J., A. Wellbrock, G. H. Jones, J. H. Waite, P. Schippers, M. F. Thomsen, C. S.
Arridge, and R. L. Tokar (2013), Photoelectrons in the Enceladus plume, Journal of
Geophysical Research (Space Physics), 118, 5099{5108, doi:10.1002/jgra.50495.
Photoelectrons at Titan near the terminator
A. Wellbrock1,2, A.J. Coates1,2, G.H. Jones1,2, J.H. Waite3
(a.wellbrock@ucl.ac.uk)
(1) Mullard Space Science Laboratory, University College London, UK
(2) Centre for Planetary Sciences at UCL/Birkbeck, UK
(3) Southwest Research Institute, USA
Cassini’s CAPS Electron Spectrometer (ELS) has observed discrete energy peaks at 24.1 eV
in the electron spectra in Titan's ionosphere. These electrons are believed to be
photoelectrons generated due to the ionisation of N2 by the strong solar He II (30.4nm) line.
They are generally observed in Titan's dayside ionosphere, because this is where neutral N2
particles can be ionised by solar radiation. Coates et al. (2007) discuss initial observations of
these photoelectrons in Titan's distant tail during the Titan encounter 'T9'. Wellbrock et al.
(2012) describe three other case studies where these photoelectrons were observed at large
distances from Titan. The photoelectrons are unlikely to have originated at these locations
because of low neutral N2 densities. The most likely explanation for their existence at these
locations is that they travelled along magnetic field lines to the observation sites from the
dayside ionosphere, where they were created. Hybrid modelling results support this idea
(Wellbrock et al., 2012). We continue the study of photoelectron energy peaks at Titan here
and present first results from a statistical overview of observations in Titan's ionosphere and
exosphere. We start by investigating how local photoelectron production is affected by the
extinction of UV flux through the atmosphere near the terminator.
Negative ion observations at Titan: Mass spectra evolution and density
profiles from T39-T43
A. Wellbrock1,2, A.J. Coates1,2, G.H. Jones1,2, J.H. Waite3
(a.wellbrock@ucl.ac.uk)
(1) Mullard Space Science Laboratory, University College London, UK
(2) Centre for Planetary Sciences at UCL/Birkbeck, UK
(3) Southwest Research Institute, USA
One of the most unexpected results of the Cassini mission was the discovery of heavy organic
negative ions in Titan’s ionosphere by the CAPS Electron Spectrometer (ELS) (Coates et al,
2007, Waite et al., 2007). These are observed during every encounter when the instrument
points in the ram direction at altitudes between 950 and 1400 km. The heaviest ions observed
so far have masses up to 13 800 amu/q (Coates et al., 2009). This indicates that complex
hydrocarbon and nitrile chemical processes take place in Titan’s upper atmosphere. Studying
the effects of different controlling parameters on the densities of different negative ion mass
groups helps constrain the chemical formation and destruction processes (Wellbrock et al.,
2013).
In this paper we discuss the evolution of negative ion mass spectra during the T40 flyby. We
also investigate density trends from flybys T39-T43; this was a group of encounters where
flyby parameters and external conditions were similar.
Future activities organised by the
UCL/Birkbeck Centre for Planetary Sciences
2 – 4 September 2015: ASB6: The Origin, Distribution & Detection of Life in
the Universe.
The Astrobiology Society of Great Britain’s 6th biennial meeting is hosted, this year, by the
CPS at UCL. Further details, registration and abstract submission can be found at:
https://www.ucl.ac.uk/cps/asb6
Accommodation at Ramsay Halls for three nights available to students for a total cost of
£30, thanks to generous support from the UKSA, and to non-students for £100 –
Limited places, so book early! Please advertise to your colleagues.
June 2016: 6th Summer Meeting of the CPS
Astrobiology and Planetary Exploration (APEX) Seminars:
Weekly during term time. Programme here:
http://www.homepages.ucl.ac.uk/~ucfbiac/APEX.htm
http://www.ucl.ac.uk/cps