Planetology in a Laboratory

PLANETOLOGY IN A LABORATORY

A. Benuzzi-Mounaix LULI Laboratory - Ecole Polytechnique OUTLINE

ü Introduction: what is planetology in laboratory?

ü How to do planetology in a laboratory? Generation of “planetary” matter, Equation of state measurements, diagnostics .....

ü Some interesting results

ü The research program PLANETLAB (2012-2016)

ü Facilities for planetology in a laboratory, teams involved, PhD subjects Introducon PLANETARY SCIENCE

² Study of Formaon and evoluon of planets

² Study of planet interiors

FAST GROWING SCIENCE DUE TO EXOPLANETS DISCOVERY

From 1988 to today

838 planets discovered Introducon Key quesons about planets inside and outside the Solar System

•What is the nature of the iron core at the center of Earth and other terrestrial planets?

•What is the interior structure of Jupiter and the other giant planets?

•What kinds of planets exist outside our solar system? Can we characterize their structures, composions, dynamics and evoluon?

Why the Saturn luminosity is not compable with its age?

To be able to answer

We have to know the equaon of state (i.e. the relaon between ρ,P,E) of the maer exisng in the planet interiors

But …. Introducon What type of maer?

Our giant planets

The important classes of materials are:

-Hydrogen and Helium

-Simple molecular

compounds H2O, NH3, CH4

-Silicates and oxides:

(Mg,Fe)2SiO4, (Mg,Fe)SiO3, SiO2, (Mg,Fe)O

-Iron and iron alloys

Introducon At which condions? Introducon This maer is called Warm Dense Maer

Al phase diagram (ρ,T) 104 classical plasma ! = 1 0. 1 ρsolide < ρ < 100 ρsolide 103 dense ! = 10 0. 1 eV < T < 100 eV plasma 102 WDM ! = 100 Condions found not only 101 high density in planetology but also in matter Ineral Conﬁnement Fusion 100 10-4 10-2 1 102 104 Density ( g/cm3) Introducon This maer is called Warm Dense Maer

Al phase diagram (ρ,T) 104 classical plasma ! = 1

103 dense ! = 10 plasma 102 WDM is the state at the intersecon WDM ! = 100 between plasma physics and condensed 101 high maer physics. density matter WDM is correlated and degenerate 100 Correlated Γ = E / E > 1 -4 c th 10 10-2 1 102 104 Coulomb energy E Density ( g/cm3) c Thermal energy Eth Degenerate ΤF > T Perfect gas does not apply Perturbaon theory is completely invalid – no small parameters Introducon Important progresses on theorecal side: Quantum Molecular Dynamics calculaons

ü Electrons are treated by quantum mechanics through Schrödinger equaon within the so called "Kohn-Sham" theory which is exact (ab inio)

ü The ions moon is deduced from Newton equaons using quantum forces created by electrons.

ü Thermodynamical equilibrium

Electronic density of D ü Equaon of state, transport properes, opacies…. 2 @ 1g/cc and 29.000 K No use of empirical parameters No need of an a priori experimental knowledge

But to conﬁrm their predicve power Need of experimental data How do planetology in a laboratory How create this planetary maer in a laboratory?

Stac way

Diamond cell Isothermal Compression P ≈ 0 - a few Mbar Dynamic way

Chemical explosions, gas guns

(Nuclear explosions)

High power lasers Shock Compression P ≈ 0 - hundreds of Mbar How to do planetology in a laboratory What is a shock ?

An abrupt change in pressure, density, energy which moves through a medium

Pressure, Density, Energy Rankine Hugoniot relations

Shock velocity D Conservation of the Fluid velocity U mass

z momentum energy How to do planetology in a laboratory Laser driven shock

Cold target Hot Laser plasma

Shock

Ablation pressure 14 2 IL en 10 W/cm 2 P " 12(I /#) 3 λ en µm L P en Mbar

Today Pressures of several tens of Mbar

! How to do planetology in a laboratory EOS measurements using a shock

Rankine-Hugoniot

ρ0D = ρ (D-U) mass

ρ0DU = P-P0 momentum

2 ρ0D(E-E0+U /2)=PU energy

3 equations, 5 unknown parameters (D,U,P,E,ρ)

To have a point on f(P, E, ρ) = 0

ü 2 parameters - absolute measurement 2 velocities D and U → time and distance How to do planetology in a laboratory How do we measure shock parameters?

Usual diagnoscs

Velocity Interferometer System for Any Reﬂector (VISAR)

target! streak Velocities (D or U) by Doppler effect & reﬂectivity λ

λ0 τ D or U

Self-emission D & Temperature T target

streak Kirchoff law: I(T,λ) = α(λ) IP(T, λ) Planckian α (λ) = 1-R (λ) radiation T How to do planetology in a laboratory Recent developments to have microscopic informaon X-ray scaering diagnosc

X-ray scaering cross 3 contribuons: secon

Free e- Weakly bound e- Thightly bound e-

Inelasc features broadened by Elasc feature thermal moons (Rayleigh peak)

Intensity Inelastic feature Inelasc feature Elastic feature Electronic density and temperature

Elasc feature

Correlaon eﬀects, phase transions ECompton E0 Energy How to do planetology in a laboratory Recent developments to have microscopic informaon X-ray absorpon near edge spectroscopy

3s - 3p band ! F 2p 2s Absorpon X K-edge

• Probe the valence 1s electrons r • Probe the local atomic order

Powerful diagnosc to study structure changes, phase transions and to test approximaons used in theories

SOME INTERESTING RESULTS Some results Some results on water

The movaon

0.7 Metallic

0.6

Fluid 0.5 Neptune isentrope Ionic 0.4

r Main Hugoniot

0.3

Temperature T (eV) T Temperature Superionic Molecular Molecular

o 0.2

0.1 Precompressed Hugoniot Solid 0 0 0.5 1 1.5 2 2.5 3

Pressure P (Mbar) Phase diagram obtained from ab initio computations (C. Cavazzoni et al., Science 283, 1999)

Why is the magnec ﬁeld of these planets so high and asymmetric?

Is it because the mantles are constuted of « ice » layers, ﬂuid and conducng?

0.7 0.7 Metallic Metallic 0.6 0.6

Fluid

Fluid 0.5 0.5 Neptune isentrope Ionic Neptune isentrope Ionic 0.4

0.4 r

0.3

0.3 c

Temperature T (eV) T Temperature Superionic

Molecular é

Temperature T (eV) T Temperature o Superionic

0.2 Molecular

o 0.2

0.1 0.1 Solid

0 Solid 00 0.5 1 1.5 2 2.5 3 0 0.5 1 1.5 2 2.5 3 Pressure P (Mbar) Pressure P (Mbar) Phase diagram obtained from ab inio computaons (C. Cavazzoni et al., Science 283, 1999) Phase diagram obtained from ab inio computaons (C. Cavazzoni et al., Science 283, 1999) Some results Some results on water

0.7 Metallic

0.6

Fluid 0.5 Opcal properes have Neptune isentrope Ionic been measured In the phase 0.4

r Main Hugoniot diagram

0.3

Temperature T (eV) T Temperature Superionic Molecular Molecular

o 0.2 M Hugoniot has been 0.1 Precompressed Hugoniot Solid measured 0 0 0.5 1 1.5 2 2.5 3

Pressure P (Mbar) Phase diagram obtained from ab initio computations (C. Cavazzoni et al., Science 283, 1999) And Hugoniot has been

P. Celliers et al PoP 2004

0.7 0.7 Metallic Metallic 0.6 0.6

Fluid

Fluid 0.5 0.5 Neptune isentrope Ionic Neptune isentrope Ionic 0.4

0.4 r

0.3

0.3 c

Temperature T (eV) T Temperature Superionic

Molecular é

Temperature T (eV) T Temperature o Superionic

0.2 Molecular

o 0.2

0.1 0.1 Solid

Mantle ! !

Outer core ! Liquid Fe!

Inner core! solid Fe! Simultaneous Temperature/ Pressure measurements across T at Earth’s Inner-Outer core boundary melting the melting region → Tmelting P=3.3 Mbar!

Critical constraint for modeling the chemical composition and energy balance of the Earthʼs core! Huser et al., PoP, 2005 Some results Study of electronic structure changes in a large WDM domain using XANES

Test WDM theories in a well-known case (Al)

Dense plasma Atomic state ! !

...

ρ 3s - 3p 3p band ! 3s F Pre-edge onset 2p 2p (1.6 g/cc) 2s 2s

density

1s 1s r r

The onset of a metal/non metal transion has been put in evidence and conﬁrmed by calculaons.

A. Benuzzi-Mounaix et al PRL (2011); A. Levy et al. PRL (2012) PLANETLAB research program (ANR 2012-2016)

Coordinated by LUTH, Observatoire de Paris Funds 500.000 euros

ü Establish benchmarking values for the equaons of Main goals: states, melng curves and the transport properes in the Fe-Si-Mg-O-S complex system exisng inside core of giant planets and super earths ü Make super earth models

THEORETICAL APPROACH EXPERIMENTAL APPROACH (ab inio calculaons) (using stac and dynamic methods)

(LUTH Meudon, CEA Bruyères le (LULI Ecole Polytechnique, Chatel) IMPMC Paris 6) Planetlab research program (ANR 2012-2016)

Program based on calculaons for exoplanets descripon aer a careful validaon against both stac and dynamical experiments that can be performed in a limited region of the phase diagram. Concerning silica Dynamic experiment to study dissociaon around the Hugoniot (scheduled on LULI 2000) using XANES/X-ray scaering Ab inio calculaons up to 20Mbar and 50000 K: melng, EOS, …

Dynamic experiment using quasi-isentropic compression to detect melng (experiment scheduled on LIL laser at CEA)

Super-earth

Stac experiments coupled to synchrotron radiaon Laser facilies in France and around the world for planetology

High energy and long pulses

JANUS laser – LLNL - USA

PALS – Prague - Czech Republic VULCAN – RAL - UK Energy LULI2000 - Ecole Polytechnique - FRANCE GEKKO laser – Osaka University - JAPAN ORION - AWE - UK LIL - CEA - FRANCE OMEGA laser – University of Rochester - USA LMJ/PETAL laser – CEA – France NIF laser – LLNL - USA Stac measurements and facilies

Contact: [email protected]

Located in Grenoble, This is the largest synchrotron in Europe

Located close to Orsay, this french facility is smallest + in situ X-ray than ESRF but suﬃcient for measurements many type of high pressure (diﬀracon, experiments absorpon, …) Experimental Teams in Paris area

LULI laboratory : A. Benuzzi-Mounaix, M. Koenig, A. Ravasio, E. Brambrink, T. Vinci, A. Denoeud ( experiments with laser)

CEA (Bruyères le Chatel) : P. Loubeyre, S. Brygoo, G. Huser (experiments with DAC + laser)

IMPMC (Paris 6): G. Morard, G. Fiquet, F. Guyot (experiments with DAC)

Theorecal teams in Paris area

LUTH (Meudon) : S. Mazevet, R. Musella

CEA (Bruyères le Chatel) : V. Recoules, J. Bouchet Internship M2 (followed by PHD)

Experimental study for planetology using high power laser Supervisors : A. Ravasio Contact: [email protected]

LULI 2000: 1kJ at 1054 nm 0.5ns-3ns 100J at 1054 1-5 ps

Internship M2 + PHD subject (already funded)

Properes of iron alloys for planetary modeling Supervisors : J. Bouchet (CEA) V Recoules (CEA) S. Mazevet (LUTH) Contact: [email protected]

Naonality requested: French Previous ab inio results on iron

Cores are solid for planets having their

mass > 5 MT

If no liquid phase, no magnec ﬁeld -> solar winds can reach the surface -> probably no possible life on these planets

Morard et al. HEDP, 2011 Internship M2 + PHD subject (already funded) Previous ab inio results on iron

Properes of iron alloys for planetary modeling Supervisors : J. Bouchet (CEA) V Recoules (CEA) S. Mazevet (LUTH) Contact: [email protected]

The discovery of extra solar planets (exoplanets) calls for a beer understanding of the properes of iron and its alloys Fe-Si-S-O in temperature and pressure domains never studied unl now. In this thesis we will use the solid state simulaon methods as DFT to study the alloys eﬀects on iron properes as the melng temperature and more generally on the equaon of state. Then these new data will be integrated in planetary models. This project will take place in an ANR obtained by the Observatoire de Morard et al. HEDP, 2011 Paris, the CEA, the Ecole Polytechnique et the university of Paris Jussieu and will be supervised by the Observatoire Cores are solid for planets having their

de Paris et the CEA. This subject has a strong numerical mass > 5 MT part and will call for a strong background in solid state physics, numerical simulaons, geophysics and planetary If no liquid phase, no magnec ﬁeld -> modeling. solar winds can reach the surface -> probably no possible life on these Naonality requested: French planets THANK YOU FOR ATTENTION