Detection de nanoparticules dans le milieu interplanétaire
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1 Detection de nanoparticules dans le milieu interplanétaire 1 Nicole Meyer-Vernet LESIA, Observatoire de Paris avec: M.Maksimovic 1, A.Lecacheux 1, K.Issautier 1, G.Le Chat 1, A. Czechowski 2, I. Mann 3, I. Zouganelis 7, K. Goetz 4, M.L. Kaiser 5, O.C. St. Cyr 5, S.D. Bale 6 2 Space Research Centre, Polish Academy of Sciences, Warsaw 3 School of Science and Engineering, Kindai University Kowakae, Osaka 4 School of Physics and Astronomy, University of Minnesota 5 NASA-GSFC 6 Space Sciences Laboratory, University of California 7 LPP, UPMC, Ecole Polytechnique nicole.meyer@obspm.fr 1 Meyer-Vernet- Seminaire 2009
2 Nanoparticules OUTLINE Particles, particles, particles... Nano-poussières dans l'héliosphère Principe de détection avec un instrument "ondes" plasma micro dust nano dust Solar Orbiter Detections Perspectives 2 Meyer-Vernet- Seminaire 2009
3 Red blood cells: 7µ Flu virus 100nm DNA ~ 2 nm wide C nm PAH: C 24 H nm nanoparticles 1 nm bulk matter 0.1 µ Interplanetary medium at 1 AU: F EM /F G ~ /a 2 nm Lorentz force dominates Lorentz force interaction with plasma, magnetic negligible fields, solar wind ions 10 A molecules ions, electrons PLASMAS Lorentz force dominates 3 Meyer-Vernet- Seminaire 2009
4 surface/mass electric charge 1/size size Lorentz force : F EM = q V X B chemical reactivity large surface-to-mass ratio large charge-to-mass ratio a (particle size) Gravitational force : F G = mm G/d 2 a 3 (for 3-D particles) Interplanetary medium at 1 AU: F EM /F G ~ /a 2 nm > 1 Radiative force : F R = a 2 QL /d 2 a 3 for a < since Q a < F G Lorentz force dominant interaction with magnetic field interaction with solar wind ions 4 Meyer-Vernet- Seminaire 2009
5 Further consequences of small size: quantum effects p r h change optical, magnetic & electrical properties Small heat capacity energy of 1 photon h ~ c T stochastic heating [Draine & Li 2001] 5 Meyer-Vernet- Seminaire 2009
6 NGC 7023 (Iris Nebula) Interstellar nanoparticles IR emission from nanoparticles far UV extinction (Weingartner & Draine 2001) a< /2 ~10 nm Dust scattering starlight IR emission (Sellgren 1984; Léger & Puget 1982, Draine & Li 2001) due to stochastic heating? PAH? Nanodiamonds [Jones & d'hendecourt 2000, Chang et al. 2006]? Nanosilicon [Li 2004]? Indirect: photoelectric heating [Weingartner & Draine 2001] 6 Meyer-Vernet- Seminaire 2009
7 Nanoparticules Nano-poussières dans l'héliosphère Principe de détection avec un instrument "ondes" plasma micro dust nano dust Detections Perspectives 7 Meyer-Vernet- Seminaire 2009
8 Scale of heliosphere: L ~ 200 AU (1 AU = m) electric charge q Interstellar medium V SUN V Heliosphere Gyroradius in magnetic field B: mv/qb << L B Interstellar nanodust cannot enter into heliosphere [Kimura & Mann 1999] except included within larger grains 8 Meyer-Vernet- Seminaire 2009
9 Detection zodiacal light (scattered sunlight) a> near the Sun: "F-corona" Fraunhofer lines IR thermal emission m Meteor trails - optical, radar - > 100 m ~ kg/year/on Earth S. Brunier Lunar micro craters m Marine isotope records ~ kg/year/on Earth [Peucher-Ehrenbrink 1996] 9 Meyer-Vernet- Seminaire 2009
10 10 Meyer-Vernet- Seminaire 2009
11 In situ collection near Earth LDEF (NASA) m ~ kg/year/on Earth [Love & Brownlee 1993; refs in Mann & al.ssrev 2010] not calibrated for nanoparticles ~100 tons/day In situ dust analysers on interplanetary probes penetration impact ionisation m Cassini- CDA [Srama 2004] 11 Meyer-Vernet- Seminaire 2009
12 cloud SUN EARTH Cumulative interplanetary flux based on data at 1 AU (Wehry and Mann, 1999) Ulysses Dust 65 millions years 1 A 10 nm 1 m 5 km Itokawa Small bodies N. Meyer-Vernet 2007 (Basics of the Solar Wind, Cambridge U. P.) /year on Earth if ~ 2.5 g/cm 3 12 Meyer-Vernet- Seminaire 2009
13 SUN EARTH Cumulative interplanetary flux based on data at 1 AU Collisional fragmentation 1 A 10 nm 1 m 5 km N. Meyer-Vernet 2007 (Basics of the Solar Wind, Cambridge U. P.) equilibrium [Dohnanyi 1969] Total mass crushed in mass log interval independent on mass steeper slope less large particles yields less small particles decreases slope smaller slope... the reverse Note:distribution of fragments a Meyer-Vernet- Seminaire 2009
14 Cumulative interplanetary flux data at 1 AU Ulysses Serendipitous discovery A 10 nm 1 m 5 km if ~ 2.5 g/cm 3 Meyer-Vernet et al. 2009] 14 Meyer-Vernet- Seminaire 2009
15 SUN EARTH First detection not surprising since: agrees with collisional fragmentation equilibrium predicted from collisional fragmentation in interplanetary dust cloud and dynamics [Mann & al. 2007] detected near comets Halley [Utterback & Kissel 1990] PAH's in sample returned by Stardust to comet 81P/Wild2 [Sanford & al. 2006] and in Tempel2 ejecta? [Lisse et al 2006] detected near planets Loki on Io Jupiter [Zook & al. 1996, Krüger & al. 2006] Saturn [Kempf et al. 2005] 15 Meyer-Vernet- Seminaire 2009
16 Nanoparticules Nano-poussières dans l'héliosphère Principe de détection avec un instrument "ondes" Detection plasma Detection micro Detection nano rapides Detections Perspectives 16 Meyer-Vernet- Seminaire 2009
17 Preliminary interpretation of STEREO dust [Kaiser et al. 2008] Observed dust flux exceeds model by factor of 10000!! SOLUTION Same signal with smaller mass IF PARTICLES ARE FAST 17 Meyer-Vernet- Seminaire 2009
18 Interplanetary nano dust: large charge-to-mass ratio Dust grain potential balance of currents determined by on uncharged grain: j ph >> j e >> j p plasma electrons - secondary electrons j e + + protons >0 j p photoelectrons + j ph - - ionising photons charges until binds photoelectrons sufficiently to yield j ph ~ j e photoelectron energy ~ a few ev ~ V Dust grain of radius a carries electric charge q ~ 4 For a ~10 nm, q ~ 70 e charge-to-mass ratio q/m~10-5 e/m p a -2 m -2/3 0 a 18 Meyer-Vernet- Seminaire 2009
19 (Mann et al. 2007) Lorentz force: F L = q(v SW - v dust )X B SW >> gravitational force F G Larmor frequency: L= qb SW /m >> Kepler frequency: G= (M G/d 3 ) 1/2 For a ~10 nm: F L /F G ~ 200 d AU L/ G ~ 20 at 1 AU Dust speed Nano dust grains accelerated to ~ V SW if released farther than ~ 0.15 AU Czechowski et al. 2009, in preparation Distance 19 Meyer-Vernet- Seminaire 2009
20 1) The importance of being fast 2) Measuring fast dust grains with a wave instrument 20 Meyer-Vernet- Seminaire 2009
21 Measuring fast dust grains with a wave instrument Ultrasensitive radio receivers developed for space missions ISEE1, 2, 3 (ICE), Ulysses, Cluster, Wind, Cassini, STEREO, Bepi-Columbo,... STEREO 2006 Earth orbit ISEE 3/ICE 1978 sensitivity: a few nv/hz 1/2 Cassini 1997 Saturn Wind 1994 Earth orbit/l1 L1/ L2/ comet Ulysses AU/ out of ecliptic Ulysses/URAP <1990 STEREO 2005 Bepi-Colombo/SORBET cm 21 Meyer-Vernet- Seminaire 2009
22 Measuring fast dust grains with a wave instrument Radio receivers on space missions designed to measure: radioemissions (EM waves) plasma waves in situ plasma measurement via spectroscopy of plasma quasi-thermal noise [Meyer-Vernet & Perche 1989, Meyer-Vernet et al. 1998] equivalent cross-section of detector >> physical cross-section plasma electron Spacecraft plasma electron ~ V plasma electron great sensitivity & accuracy (calibrates other devices) only device capable of measuring density & temperature of cold plasmas (comets, rings..) 22 Meyer-Vernet- Seminaire 2009
23 Example: solar wind electron measurements in routine on Ulysses/URAP Data points and best fit with 6 plasma parameters (electron density & core temperature, speed, suprathermal electron density & temperature) Temperature f p Density TIME 23 Meyer-Vernet- Seminaire 2009
24 BRUIT QUASI-THERMIQUE DU PLASMA TIME [Issautier & al. 1998] Vent solaire pole à pole (Ulysse) 2001 [Issautier & al. 2001] 1992 [Meyer-Vernet & al. 1992] 1998 Magnétosphère de Saturne (Cassini) 2004 [Moncuquet & al. 2005] 24 Meyer-Vernet- Seminaire 2009
25 PLASMA QUASI-THERMAL NOISE Jupiter B [Meyer-Vernet & al. 1992] Measure: electron density electron temperature magnetic field B Saturn B [Moncuquet & al. 2005] 25 Meyer-Vernet- Seminaire 2009
26
27 Measuring fast dust grains with a wave instrument Impact ionisation Amplitude: Extrapolation of laboratory measurements: Detected electric charge upon impact: increases fast with speed Q m v 3.5 grain mass grain speed Nanoparticle: radius r ~ 10 nm, mass m ~10-20 kg, speed v ~ 400 km/s yields same Q as: submicron particle: radius r ~ 0.3 m, mass m ~10-15 kg, speed v ~ 20 km/s Nanoparticles produce large electric signals 27 Meyer-Vernet- Seminaire 2009
28
29 Measuring fast dust grains with a wave instrument Impact ionisation Time scale: Waveform (time domain sampler) Voltage Voltage rise Measurement: and/or decay time t Instrumental filtering time t Voltage power spectrum Power spectral density (frequency receiver) 1/ decay (adapted from Meyer-Vernet 1985) 1/f 2 1/f 4 1/ rise frequency f Frequency of observation -2/3 ~ 1/(2 ~ 5 khz d AU 29 Meyer-Vernet- Seminaire 2009
30
31 Nanoparticules Nano-poussières dans l'héliosphère Principe de détection avec un instrument "ondes" Detection plasma Detection micro Detection nano rapides Detections Perspectives 31 Meyer-Vernet- Seminaire 2009
32 Measuring fast dust grains with a wave instrument First (serendipitous) dust detection with wave instruments Voyager in Saturn G ring (micro-dust) Dust impacts produce voltage pulses on plasma wave instrument (Gurnett et al 1983) and Voltage power spectrum (Aubier et al. 1983) dipole antenna Voyager 2 / Saturn G ring monopole antenna PWS: PRA: Gurnett & al Aubier & al Tsintikidis & al Meyer-Vernet & al Voyager at Saturn, Uranus, Neptune monopole antenna: measures spacecraft potential dipole antenna: (measures potential between two booms) Signal on monopole much greater than signal on dipole and better calibrated Signal on dipole depends on dust via dissymetries of antennas 32 Meyer-Vernet- Seminaire 2009
33 Voyager in Uranus & Neptune rings detects micro dust Voyager/PRA (Planetary Radioastronomy instrument) Uranus Voyager at Saturn, Uranus, Neptune Meyer-Vernet et al Pedersen et al Meyer-Vernet- Seminaire 2009
34 Cassini in solar wind near Jupiter detects nano dust Io ejects nano dust Nano dust is ejected by Jupiter corotation electric field Nanodust is accelerated by solar wind Dust analyser not calibrated for nanodust But detected small signals explained by fast nano dust 34 Meyer-Vernet- Seminaire 2009
35 Cassini in solar wind near Jupiter detects nano dust Io ejects nano dust Nano dust is ejected by Jupiter corotation electric field Nanodust is accelerated by solar wind RPWS TIME Antennas 35 Meyer-Vernet- Seminaire 2009
36 RPWS Cassini in solar wind near Jupiter detects nano dust f -2 Jupiter stream quasithermal noise Meyer-Vernet, Lecacheux & al., Geophys. Res. Lett. 36, L03103 (2009) Same signal on the 3 monopoles Signal on dipole is much smaller Flux of nanodust deduced from wave instrument similar to simultaneous measurement with conventional dust detector 36 Meyer-Vernet- Seminaire 2009
37 STEREO in solar wind at 1 AU detects nano dust 37 Meyer-Vernet- Seminaire 2009
38 STEREO in solar wind at 1 AU detects nano dust WAVES Voltage power spectrum waveform Meyer-Vernet et al., Solar Phys. 256, 463 (2009) 38 Meyer-Vernet- Seminaire 2009
39 STEREO in solar wind at 1 AU detects nano dust V 2 f 4 hf voltage power spectrum: V 2 ~ 2 2 <SF( V/ ) 2 > / receiver gain surface of 2 target ~R MAX Flux from v(m) (dust dynamics) 4 2 f <..> = average during receiver acquisition time ~0.15 sec data at 1 AU 10 nm from Meyer-Vernet et al Meyer-Vernet- Seminaire 2009
40 Nanoparticules Nano-poussières dans l'héliosphère Principe de détection avec un instrument "ondes" Detection plasma Detection micro Detection nano rapides Detections Perspectives 40 Meyer-Vernet- Seminaire 2009
41 Detailed analysis of STEREO data 3 years Fig. K. Issautier & M. Maksimovic Detailed analysis of Cassini data Fig. A. Lecacheux 41 Meyer-Vernet- Seminaire 2009
42 Detection method simulation of impact plasma & electric signal [Pantellini & Landi in progress] response of wave receiver Origin of particles interplanetary dust cloud planets,... Composition, shape... Interaction with solar wind electric charge of nanodust (transition dust/molecules) dynamics [Czechowski et al. in progress] size limit? (Coulomb explosion? since q>0 not limited by field emission) effects on solar wind ("inner source"...) ISSI international team Nano Dust in the Solar System: Formation, Interactions & Detection 42 Meyer-Vernet- Seminaire 2009
43 Other detections Via radiation? Reanalysis of past detections (impacts from fast nano possibly misinterpreted as bigger & slower grains?) Wave detection of nanodust on future space missions dipole antennas: quasi-thermal plasma noise electron density & temperature monopole antennas: fast nano dust Complementary to conventional dust detectors large collecting area (whole spacecraft) not reliant on specific spacecraft attitude requires few resources (by-product of wave instrument) V 2 Hz f dust plasma QT noise 1 10 Solar Orbiter RPW f -4 f(khz) 43 Meyer-Vernet- Seminaire 2009
Detection de nanoparticules dans le milieu interplanétaire
Detection de nanoparticules dans le milieu interplanétaire 1 Nicole Meyer-Vernet LESIA, Observatoire de Paris avec: M.Maksimovic 1, A.Lecacheux 1, K.Issautier 1, G.Le Chat 1, A. Czechowski 2, I. Mann 3,
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