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Home , Chondrule, Meteorite fall, Ureilite

““RecoveryRecovery ofof meteoritesmeteorites inin Spain,Spain, andand thethe specialspecial meteoritemeteorite fallfall ofof 2008TC32008TC3 overover SudanSudan””

Josep M. Trigo-Rodríguez (Institute of Space Sciences, CSIC-IEEC) processing, time Heat, collisional OUTLINEOUTLINE z Protoplanetary disks and : – A test for formation theories z The properties of primeval bodies. z A multidisciplinary approach to study interplanetary matter: The Spanish Meteor & Fireball Network (SPMN) z A continuous meteor and fireball monitoring over Spain – Daylight : recoveries – Main results obtained since SPMN first operations z Asteroidal streams: recent SPMN discoveries: – How common are streams producing meteorites? – NEOs and JFCs as source of meteorites…? z Meteorites sampling MB and NEO bodies – An opportunity for planetary exploration: Puerto Lápice and 2008TC3 z Conclusions: the importance of meteorite recovery YOUNGYOUNG STELLARSTELLAR OBJECTSOBJECTS ((YSOsYSOs))

z These objects are evidence of the violent environment that surrounds star formation

z Molecular clouds are enriched by nucleosynthesis products, and dust from previous stars

z Strong (100-200 km/s) stellar winds throw part of the HST (NASA) materials continuously falling into unstable regions of the disk.

z Strong magnetic fields produce bipolar outflows that are characteristic of these objects

z The was formed in a gas-rich environment subject to strong and energetic stellar winds coming from the young Sun Snell et al. (1980) Shu et al. (2001) AA SIMPLIFIEDSIMPLIFIED BIRTHBIRTH SEQUENCESEQUENCE FORFOR THETHE SOLARSOLAR SYSTEMSYSTEM

z What was the origin of the matter falling into the protoplanetary disk? – Not all chemical and isotopic fingerprints were erased because the was not so hot as Cameron (1978) and Lewis (1980) thought. – Products of the chemical evolution of the galaxy – Primitive meteorites inherited stellar materials: • Isotopic anomalies and

z formed from the of first condensates, and preexisting materials ∼3- 5 Myr after condensation of CAIs. – Time constraints from the study of SLN – Primordial nebula collapsed ~4.57 Gyr ago

First 10Myr in SS formation PRIMITIVEPRIMITIVE METEORITES:METEORITES: DIRECTDIRECT INFORMATIONINFORMATION ONON DISKDISK COMPOSITIONCOMPOSITION

z Chondritic meteorites are coming from undifferentiated bodies: – Protoplanetary sediments – Contain , refractory inclusions, but also fine dust and organics in matrix. z Diversity of formation conditions depending of heliocentric distance: – Different abundances of chondritic materials z However, important effects of turbulence that mixed the materials and altered the simple scenario

Ameboid Inclusion (AOI) in Acfer 094 PRIMITIVEPRIMITIVE CHONDRITESCHONDRITES

z Initially they were highly porous materials: P>60% (Blum et al., 2006) z Chondrules, refractory inclusions, grains, and fine dust and organics were accreted from the nebula z Collisional evolution compacted the primordial materials

Ungrouped Acfer 094 CARBONACEOUSCARBONACEOUS CHONDRITESCHONDRITES

z Rocks from water-rich bodies containing chondrules, inclusions and fine dust materials:

– Until 10% H2O and 4% C in mass

z Some CCs experienced aqueous alteration to different degrees (McSween, 1979) – Many mineral phases are alteration products 1 cm sized SEM image of Y791198 CM2 (Zolensky & McSween, 1988): • phyllosilicates, sulfides, carbonates, and oxides

z CCs suffered secondary processes after accretion (Brearley & Jones, 1998): – Aqueous alteration – Brecciation (consequence of impacts)

z Two main scenarios for aqueous alteration: – (Zolensky & McSween, 1988) – Preaccretionary, occurred in uncompacted precursors (Metzler et al. 1992) Murchison CM2 PRESOLAR COMPONENTS RETAINED IN PRIMITIVE SOLAR SYSTEM MATERIALS

z Short-live radionuclides – They were incorporated during condensation on mineral phases in the solar nebula: CAIs, chondrules, etc – A few (e.g. noble gases) were retained in the matrix during the early accretion of planetesimals z Presolar grains z Fine-dust materials: – Carbonaceous materials with chemistry and isotopic anomalies inherited from the IM STELLARSTELLAR SOURCESSOURCES OFOF SELECTEDSELECTED RADIONUCLIDESRADIONUCLIDES z In particular short-lived nuclides (SLN) were important for planetesimals internal heating z They incorporated from the vapor phase into the minerals forming chondritic components

Parent Daughter Detected Presence Half-Life Likely stellar source(s) (106 yr)

10Be 10B CAIs (McKeegan et al., 1.5 Spallation product 2000)

26Al 26Mg CAIs (Lee et al.,1966) and 0.73 SN, massive AGBs chondrules (Galy et al. 2000)

41Ca 41K CAIs (Srinivasan et al., 0.1 AGBs 1994)

53Mn 53Cr CAIs (Birk and Allègre, 3.7 AGBs 1985), chondrules, etc 60Fe 60Ni CAIs, 1.5 SN, massive AGBs (Shukolyukov and Lugmair, 1993) 87Rb 87Sr CAIs 48,800 Massive AGBs DATINGDATING SYSTEMSSYSTEMS BASEDBASED ONON PRIMORDIALPRIMORDIAL RADIONUCLIDESRADIONUCLIDES

z Two types of isotopic system Parent Daughter(s) Half-life (yr) * are used to determine timing of events in the solar nebula 40K 40Ar or 40Ca 1.3×109 – The quantity of a stable daughter derived from 87 87 10 the decay of a proportion of an Rb Sr 4.88×10 extant long-lived radioisotope 147 143 11 gives the absolute age or time Sm Nd 1.06×10 to the present since the system became closed to isotopic 176Lu 176Hf 3.57×1010 interchange – Also the quantity of an isotope 187Re 187Os 4.56×1010 inferred to have been produced by the total decay of 232 208 4 10 a short-lived isotope yields the Th Pb + 6 He 1.4×10 period between isotopic 235 207 4 8 closure, and the time when the U Pb + 7 He 7.04×10 parent became extinct 238 206 4 9 U Pb + 8 He 4.47×10 z Both systems are cross- calibrated with precise U-Pb * T1/2=0.693/λ, being λ the decay constant ages of rapidly cooled igneous meteorites THETHE FORMATIONFORMATION SCENARIOSCENARIO OFOF FIRSTFIRST SOLARSOLAR SYSTEMSYSTEM MATERIALSMATERIALS z ≈4.6 Gyr ago the solar nebula started its collapse – Presolar grains were embedded in the dust – In the hot nebular regions the first refractory minerals formed by evaporation, recondensation and melting of presolar dust grains, and SS condensates z At ~4567 Myr: CAIs formed incorporating radionuclides from the stellar environment z At ~4566 Myr: formation begins and continues for about 1-2 Myr z Between 4565-4564 Myr the different components accrete to form the chondritic : first planetesimals z Since then: Collisional compaction, and aqueous alteration have participated in processing the rock-forming materials of minor (undifferentiated) bodies Jewitt et al. (2008) AA MASSIVEMASSIVE AGBAGB STARSTAR ININ THETHE ORIGINORIGIN OFOF THETHE SOLARSOLAR SYSTEM?SYSTEM? z We have suggested that a 6.5 M© AGB star of solar metallicity played a role in the Solar System enrichment in short-lived nuclides (SLN) z By comparing the SLN abundances in primitive meteorites with the isotopic pattern modeled for the surrounding environment of that AGB star – Our model match the abundances of 26Al, 41Ca, 60Fe, and 107Pd inferred to have been present in the solar nebula

by using a dilution factor of 1 part of Image Gabriel Pérez Diaz (IAC) AGB material per 300 parts of original solar nebula material Publication details: – Such a polluting source does not Trigo-Rodríguez J.M., D.A. García-Hernández, overproduce 53Mn, as M. Lugaro, A. I. Karakas, M. van Raai , P. models do, and only marginally affects García Lario, and A. Manchado (2009) isotopic ratios of stable elements and Planetary Science 44, 627. TYPESTYPES OFOF STELLARSTELLAR GRAINSGRAINS z Usually called “presolar” because: – These grains are suspicious to be formed in stellar outflows of late-type stars and in ejecta of stellar explosions – Their stellar origin is identified by their anomalous isotopic compositions compared to SS materials

Grain type Typical size Abundance Stellar sources Diamond 2 nm 1,000 ppm AGB?, SNe Silicon carbide 0.1-20 µm 10 ppm AGB, SNe, J-stars, novae refractory Graphite 1-20 µm 1-2 ppm RG, AGB, SNe Oxides 0.15 – 3 µm 1 ppm SNe, AGB Silicon nitride 0.3 – 1 µm ∼ 3 ppb SNe, AGB Ti-, Fe-, Zr-, Mo- 10-200 nm < 1 ppb SNe carbides Kamacite, iron ∼10-20 nm ? SNe Olivine 0.1-0.3 µm ? RGB, AGB, SNe?

compiled from: Zinner, (2003) and Lodders and Amari (2005) THETHE PATHWAYPATHWAY FROMFROM SMALLSMALL TOTO LARGELARGE THETHE REMNANTS:REMNANTS: COMETSCOMETS ANDAND ASTEROIDSASTEROIDS

1 km 433 Eros (NEAR- Tempel 1 Shoemacker/NASA) (Deep Impact/NASA) LABORATORYLABORATORY EXPERIMENTSEXPERIMENTS

z Main goal: – To learn about the expected physical properties of primeval accretionary bodies z Study of macroscopic aggregates (a,b) built from different types of grains:

– c) Spherical monodisperse SiO2 grains – d) Irregular diamonds

– e) Irregular polydisperse SiO2 z Resulting porosities of the order of 80 to 67% for the maximum compression of planetesimals (relative velocities of 50 m/s) z Tensile strengths in the range of 0.2 to 1.1 kPa

Tensile Strength Blum et al., ApJ (2006) Determination experiment POROSITYPOROSITY ANDAND DENSITYDENSITY OFOF METEORITESMETEORITES

z All meteorites arriving at Earth are compacted samples: – Materials are also biased during atmospheric transition towards the tougher objects (!) STARDUST:STARDUST: CLUESCLUES ONON KBKB COMETSCOMETS

z 81P/Wild 2 particles decelerated in SiO2 aerogel from 6 km/s – A Family Comet formed in the Kuiper Belt z In the Preliminary Examination Team we studied the , chemical and isotopic composition of the surviving particles – Incoming particles were fragile aggregates – Fine grain materials rarely survived, but large mineral grains were almost intact • About a thousand with diameters of 5 to 300µm z Physics behind excavation of tracks: Trigo-Rodríguez et al. (2008) MAPS 43, 75. CLUESCLUES ININ RECOVEREDRECOVERED GRAINSGRAINS

z The largest recovered grains are ~5-15µm in diameter. – The toughest fragments that survived the capture process – They are composed by fragile aggregates of relatively large mineral grains compacted in a fine-dust material similar to the matrix of carbonaceous chondrites – This fine-grained component is rich in organics and contains important isotopic anomalies: • Detected enrichments in 15N/14N

8 µm-size particle (FEBO) (Brownlee et al., 2006) TEM image showing 15N hotspot (PET/NASA) PROCESSEDPROCESSED SILICATESSILICATES INSIDEINSIDE AA KUIPERKUIPER BELTBELT COMET!COMET!

z Many mineral grains recovered larger that 1 µm are olivine and – Sinthesized nearby the Sun! • Confirmation of important radial turbulence in the protoplanetary disk (Bockelée- Morvan et al, 2002). – Wild 2 silicates were formed in the inner solar system: • New picture

z Can be these results extrapoled to other ? SPACECRAFTSPACECRAFT MISSIONSMISSIONS TOTO ASTEROIDSASTEROIDS THETHE MAINMAIN ASTEROIDASTEROID BELTBELT – Remnants of the bodies that were not gravitationally scattered or accreted into the • About 200.000 known in the Main Belt (~750.000 estimated) • With orbits approaching to Earth: – NEOs acronym of NEAR EARTH OBJECTs • 785 with diameter D> 1 km • 6435 in total – Potentially Hazardous Asteroids: • 145 over D>1 km • 1067 in total • About 80-90% of bodies impacting the Earth are delivered from the Main Belt

Asteroides Ida y Dactil (ESA) DYNAMICDYNAMIC RESONANCESRESONANCES

z The main belt has many unstable regions, evidenced by the called Kirkwood gaps in distribution z Those objects whose orbital periods are multiples of the periods of nearby planets (mainly Jupiter, Saturn and ) are in “resonances” z Most meter-sized reaching the Earth come from these regions THETHE ROLEROLE OFOF IMPACTSIMPACTS ININ METEORITEMETEORITE DELIVERYDELIVERY

z Impacts have been continuously excavating asteroids: – The energy released in the impact drives rocks over escape velocity

z These rocks follow distinctive orbits for millions of years: – When orbital resonances change their orbits they reach the inner solar system – Tens of millions of years after the collision, these rocks reach the Earth as meteorites

z Important biasing processes: – Subjected to collisions with other rocks in the main belt – They are broken in the terrestrial atmosphere • The most fragile rocks are rarely surviving ! Don Dixon ATMOSPHERICATMOSPHERIC INTERACTIONINTERACTION

-10 Perseid fireball, August 12, 1993 (Trigo-Rodriguez, 1994) TERMINOLOGYTERMINOLOGY

z Meteoroid – Particle orbiting the Sun

z Luminosity α Ek 2 z Ek=½ m·v

– Meteor (-4 < Mv<+6 )

– Fireball or (Mv≤-4)

– Superbolides (Mv≤-17): • Meteorites: rare surviving samples. HOWHOW ISIS AA METEORMETEOR PRODUCED?PRODUCED? z Meteoroid melting starts when collisions lead to T>1500 K – Ablation process. z Radiation regions: – Main spectra: • Origin in the HEAD • T≈ 4500 K – Second component: • COLLISION FRONT • T≈ 9500 K – The ablation column forms the METEOR. z Sinks of energy: – IR and UV radiative mechanisms still unknown. – Fragmentation and sputtering effects. FIREBALLFIREBALL NETWORKSNETWORKS’’ ROLEROLE z European Fireball Network: THE EUROPEAN FIREBALL NETWORK • Recovery of Pribram meteorite in 1959. First orbital determination. • 2002 Neuschwanstein. z Prairie Network (1964-1974): • 16 stations around . • Recovery of Lost City meteorite (H5) in 1970 . z Canadian Photogr. Network (1971-1985): • Recovery of Innisfree in 1977 (LL5). z Direct and unique orbital and spectral information (!): • Most bodies are not recovered. z Three networks under operation: • Spain (2004-present) • Australia (2006-present) • , Canada (2007-present) SPANISHSPANISH FIREBALLFIREBALL NETWORKNETWORK z First all-sky CCD + video network: – Astrometric res. ∼1.5 arcmin (Trigo-Rodriguez et al., 2004) z History: – First all-sky images 2002. – First double stations: 2004. – Present status: • 6 all-sky CCD stations • 11 video stations – + 2 new CCD + video stations planned for 2010 z Homepage: – To promote people’s participation – Popularization of this field in Spain • Creation of social, and scientific interest – Homepage: www.spmn.uji.es FIRSTFIRST AUTOMATISEDAUTOMATISED PROTOTYPEPROTOTYPE

+2 magn. North δ Aquarid, Aug. 12, 2006 Night sky Montsec Astronomical Observatory (IEEC), July 24 2006 AA CONTINUOUSCONTINUOUS MONITORINGMONITORING

z All sky CCD cameras have extraordinary sensitivity: – They can be operated under unfavorable conditions – Detection of meteors and fireballs (Mv<+3)

Image of a 2006 Perseid meteor (Full and cloudy skies) THETHE κκ CYGNIDCYGNID DISPLAYDISPLAY

z This experienced a display reported by our team in CBET 1055 z About 20 fireballs of this shower were imaged during 2007, and 50% were recorded from multiple station. z Two fireball spectra, one very detailed exhibiting chondritic composition For more details: - Trigo-Rodriguez et al. (2008) MNRAS. HIGHHIGH SENSITIVITYSENSITIVITY VIDEOVIDEO CAMERASCAMERAS

z Other type of stations based in video detectors are being setting up by the SPMN z Array of high-sensitivity CCD video cameras. – Daylight events ALSO monitored – Nocturnal cameras are also endowed with holographic diffraction gratings for obtaining meteor spectra. CCD video cameras operated from Univ. Huelva – Fast aspherical lenses (f0.8) are attached to these cameras to maximize image quality: • Limiting meteor magnitude +2/+3 without using image intensifiers. z For meteors brighter than mag. -6 the diffraction gratings attached to the video cameras allows us to record the corresponding emission spectrum: – Information about the chemical composition of the particles.

Folgueroles station near Vic () operated by AAO-CSIC NEWNEW GALICIANGALICIAN STATIONSSTATIONS z Our goal is to achieve the full monitoring of the atmosphere over the Iberian Peninsula by 2010: – Effective surface: Half a million km2 z Prof. Docobo (Univ. Santiago Compostela) efforts to study and popularize this research area has fructified in two new SPMN stations in Galice: OARMA Y LUGO.

z Both Galician stations started monitoring operations in May 2009. z The brightest event recorded from that date was the fireball SPMN010609 occurred on June 1, 2009 at 0h23m31s UTC Composite image of SPMN010609 AA RECENTRECENT IMAGEDIMAGED EVENTEVENT

SPMN020909 from z A -12 abs. magn. bolide appeared over Sevilla station on Sept. 2, 2009 at 21h39m05.1s UT z It was named SPMN020909 “Montilla” z Recorded from three stations z Its ending height was at 47km – It was probably not a meteorite-dropping event THETHE NEONEO 2002NY402002NY40 ASAS SOURCESOURCE OFOF METEORITESMETEORITES

z In 2006 three fireballs identified by the SPMN and the Finish network had a common origin: – Their orbits reveal their similitude with NEOs 2002NY40 and 2004NL8

z For the first time three bolides were linked with NEOs “Cortes de la Frontera” bolide (SPMN310806) z Trigo-Rodríguez et al. (2007) MNRAS All-sky image from La Mayora, Málaga (IAA-CSIC) USINGUSING DISSIMILARITYDISSIMILARITY FUNCTIONSFUNCTIONS TOTO IDENTIFYIDENTIFY NEONEO ANDAND JFCJFC SOURCESSOURCES z To determine the association of meteoroid orbits with their parent bodies a method involving orbital comparison via dissimilarity functions must be used. – The Southworth-Hawkins criterion (Dsh) – Plus other criteria: Jopek, Jenniskens, etc… z Backwards integration in time of the orbits of NEOs and meteoroids provides the evolution of the orbital elements, and allow

the determination of Dsh ∝ƒ(t)

2008 CG116 & AVG Stream t0 = 2455000.5 1,6

1,4

1,2

1

0,8 D (SH) 0,6

0,4

0,2

0 From Galligan (2001), MNRAS 327. -20000 -15000 -10000 -5000 0 Years

A very unlikely association shows Dsh>0.2 in few thousand years (J. Lacruz) ORBITALORBITAL EVOLUTIONEVOLUTION

SPMN310806

2002NY40 HOWHOW CANCAN BEBE ROCKSROCKS FROMFROM 2002NY402002NY40 DELIVEREDDELIVERED TOTO EARTH?EARTH?

Like the asteroid Itokawa, 2002NY40 seems to be a rubble pile: maybe some of the boulders were lifted off during a break up caused by a close approach to the Earth or Mars? 2002NY40 radar image, Roberts et al. (2007) FIREBALLFIREBALL SPECTRASPECTRA COMPAREDCOMPARED WITHWITH PARENTPARENT BODYBODY MINERALOGYMINERALOGY

z The analyses of the spectra of two bolides allowed the determination of: – Chemical ratios of both meteoroids, similar to the LL group of Ordinary Chondrites – 2002NY40 has a reflectance spectrum like LL chondrites

FN300806 bolide video spectrum (E. Lyytinen)

Reduced spectrum (Trigo-Rodríguez et al., 2007) RECOVERINGRECOVERING METEORITESMETEORITES ININ SPAINSPAIN 2004. RECOVERY OF VILLALBETO DE LA PEÑA L6 CHONDRITE

• We are compiling all possible information on meteoroids reaching the Earth over the Iberian peninsula: – Dynamic from their orbits – Chemical from meteor spectra • Meteorite recovery efforts have been successful in two previous occasions – Accurate information on the atmospheric trajectories and orbits of bolides producing meteorites is

one of our goals, only achieved in 2007. RECOVERY OF PUERTO LAPICE nine occasions until now (!) • Spain is one of the optimal locations in Europe to recover meteorites because of having scarce vegetation and plain terrains in most of its territory, particularly nearby the Mediterranean coast. SPMNSPMN STUDIESSTUDIES ONON METEORITEMETEORITE FALLSFALLS z VILLALBETO DE LA PEÑA FALL z Daylight event, casually recorded. z Daylight bolide of magnitude -18±1 z January 4, 2004 at 16h46m45s UTC z Initial meteoroid mass: 750 ± 150 kg z SPMN infrastructure allowed the bolide study and meteorite recovery For more details: Llorca et al. (2005) MAPS and Trigo-Rodríguez et al. (2006) MAPS

Composite frame sequence of the video recorded from Leon.

z Total light emission: 5.7×109 J from the analysis of the video z Energy: ~0.022 kilotons – Consistent with photometric, seismic, and infrasonic data. z Determination of the trajectory and orbit. NOCTURNNOCTURN CALIBRATIONCALIBRATION OFOF PICTURESPICTURES FORFOR TRAJECTORYTRAJECTORY DETERMINATIONDETERMINATION

z 65 calibration points were selected in every frame (right). In the 110 frames, a total of ~7,000 points were accurately measured. z Calibration images were obtained for all locations where the fireball was imaged. Astrometric reduction was made by following the procedures of Borovicka et al. (2003). z On the right is a calibration picture containing stars from constellations of Boötes, Hercules and Draco. VILLALBETOVILLALBETO FALL:FALL: SEISMICSEISMIC DATADATA

Seismic detection of the airblast during massive fragmentation at a height of 28 km. Arriondas seismic station () Data from Llorca et al. (2005) Picture taken from Las Oces (León). Fireball imaged at 47 km height, ~1 second before main fragmentation. VILLALBETOVILLALBETO OBSERVINGOBSERVING CONDITIONSCONDITIONS

z The Earth receives ~10 impacts with such energy every month: – Appeared in broad daylight when thousands of people were attending diverse festivities in the northern part of the Iberian Peninsula – Increasing availability of digital cameras makes possible for eyewitnesses to obtain valuable records of daylight fireballs VILLALBETOVILLALBETO FALL:FALL: FRAGMENTATIONFRAGMENTATION EVENTSEVENTS

Severe breakup at 28 km P = ~70 Mdyn cm-2

z Video frame at the same moment from León z Picture of the bolide in flight after fragmentation obtained from Santa Columba de Corueño (León) METEORITEMETEORITE RECOVERYRECOVERY

First recovered meteorites by our team, most are exposed in the MNCN (CSIC).

z Best documented case of a in Spain: • A video tape and two direct pictures. • Tens of images of the persistent train. • 4.6 kg of meteorites recovered. Villalbeto de la Peña . VILLALBETOVILLALBETO FALL:FALL: ORBITALORBITAL DATADATA

z Villalbeto de la Peña is the ninth meteorite z with a known heliocentric orbit.

z MAIN DATA:

z Initial velocity: 16.9 ± 0.4 km/s z Heliocentric velocity: 37.7 ± 0.5 km/s

z Orbital period: 3.5 ± 0.5 yr z Aphelion distance: 3.7 ± 0.4 AU z Eccentricity: 0.63 ±0.04 z Semimajor axis: 2.3 ± 0.2 AU z Inclination: 0.1 ± 0.2 º z Argument of perihelion: 132.3° ± 1.5° z Perihelion distance: 0.860 ± 0.007 AU z Longitude of perihelion: 56.0° ± 1.5° Orbit of Villalbeto (considering the uncertainty in the orbital elements) compared with previously determined orbits of meteorites (Trigo-Rodríguez et al., MAPS, 2006) VILLALBETOVILLALBETO’’SS ORIGINORIGIN z Using the source-region model for NEAs of Bottke et al. (2001), and taking into account the uncertainties in the orbital elements, Villalbeto de la Peña could have originated in four regions:

• The 3:1 jovian resonance,

• The ν6 resonance, • The Mars-crossing region, • The outer main belt.

However, the similar probabilities for these four regions make it difficult to determine the exact source of the meteorite PUERTOPUERTO LLÁÁPICEPICE EUCRITEEUCRITE

z Produced from a daylight bolide seen on May 10, 2007 z Fall details studied in the SPMN framework z It is the eight eucrite recovered in Europe, and the only one with reliable trajectory and orbital information z From casual pictures of the persistent train we have reconstructed the probable trajectory and range of orbital solutions z About 70 recovered fragments, most of few grams (TKW ~600 g)

For more details: One piece showing the different lithologies (basaltic - Llorca et al. (2009) MAPS 42(2), ) - Trigo-Rodriguez et al. (2009) MAPS 42(2), THETHE ORIGINORIGIN OFOF PUERTOPUERTO LLÁÁPICEPICE z The trajectory was not so accurately determined from the pictures of the train, and not video records were found z Although no velocity information exists, the trajectory data compiled allowed the determination of a range of orbital elements z It was a 30-cm sized meteoroid on a Apollo-type orbit with semimajor axis larger than 1 AU z Cosmic ray exposure age: 19±2 Myr z The original meteoroid could have been delivered from the main belt by a resonance

– The 3:1 and ν6 resonances would link the Puerto Lápice meteoroid to the Vesta family THETHE BUNBURRABUNBURRA ROCKHOLEROCKHOLE

z It is a new meteorite with orbit recovered in Australia on 2008 (Bland et al., 2009) z A basaltic meteorite that is not coming from the HED suite (Vesta) z It arrived from an Aten-type orbit

(72% probability from the ν6 resonance)

The bolide and the stone (Bland et al., 2009, Science 325, 1525) BBÉÉJARJAR SUPERBOLIDE:SUPERBOLIDE: 1111--77--20082008 z The brightest bolide recorded by our network in about one

decade (Mabs=-18) z The incoming mass was over 1.8 Tm, deepening until a height of 22 km, indicative of meteorite survival

The Bejar bolide as photographed from Torrelodones (J.P. Vallejo) DISRUPTIONDISRUPTION OFOF C/1919Q2C/1919Q2 METCALF:METCALF: AA JUPITERJUPITER FAMILYFAMILY COMETCOMET

z The orbit computed for the Béjar bolide places the origin behind Jupiter, opening a pathway for meteorites from the outer solar system (Trigo-Rodríguez et al., 2009, MNRAS 394, 569) z A continuous study of bright bolides from new CCD-video networks can provide important surprises in the next future SOMESOME NETWORKNETWORK STATISTICSSTATISTICS z About 300 fireballs are imaged every year z Below are shown the most important 2007 events, some of them representative of streams producing bolides:

Code Date Time (UTC) Abs. SPMN Stations RAD Magn. SPMN090207 Feb. 2 21h13m58±15s -6 Montseny + Folg SPO SPMN250307 Feb. 25 00h48m33.1±0.1s -13 Sevilla + C. Negro VIR SPMN100507 May 10 17h57m30±30s -16 ± 3 Cas. pictures +reports SPO Meteorite recovery SPMN140707 July 14 01h43m40±1s -6 Sevilla + C. Negro ODR SPMN160807 Aug. 16 02h25m26.5±0.1s -9 Sevilla + El Aren. KCG SPMN180807 Aug. 18 21h21m09.3±0.1s -8 Sevilla + El Aren. PER SPMN230807 Aug. 23 04h22m22.9±0.1s -13 Sevilla + C. Negro AQU SPMN211007 Oct. 21 03h29m36.7±0.1s -9 Sev. + C. Neg. + Torr ORI SPMN181107 Nov. 18 01h14m10±2s -11 Montseny + Folg LEO SPMN131207 Dec. 13 01h25m46.8±0.1s -11 Sevilla XOR METEORITESMETEORITES FROMFROM NEONEO 2008TC32008TC3 2008TC3 from Gualba Observatory (A. Sánchez) z 2008 TC3 was a 4-meter asteroid identified in direct route of collision with the Earth on Oct. 6, 2008 z After the bright bolide recorded by Meteosat satellites, produced meteorites (!) z In Dec. 2008, was recovered a fascinating in the Nubian desert in North z are ultramafic rocks of probable magmatic origin z The accurate orbit allows to link dynamically this meteoroid with F-class asteroid 152679 1998 KU2

For more details Jenniskens et al. (2009) Nature 458, 485. THETHE PRESENTPRESENT FLUXFLUX OFOF BODIESBODIES Brown et al., (2002) z In the mass range: 3 0.1≤M∞≤ 2×10 kg z Heterogeneous * Puerto Lápice composition. * Villalbeto z Main fireball groups and percentage populations: – Group 0: ?, 3% – Gr. I: Solid material from asteroidal origin (AO), 29% – Gr. II: Porous AO, 27% – Gr. III: Fluffy, probably The Earth receives one impact in the range of 2 to 10 ktons annually and one cometary, 35% impact of 0.3 ktons monthly. CONCLUSIONSCONCLUSIONS z Primitive meteorites and comets provide direct information on the nature of protoplanetary disk components • Evidence for low strength and high porosity planetesimals • Importance of turbulence and mixing in the early protoplanetary disk z Astrophysical models should explain the formation of meteorite components: • Formation conditions of CAIs, AOIs, chondrules, presolar grains, etc… z Cometary matter was probably an important source of organic material at the time life originated on the Earth: • Even today it continues raining on the Earth in appreciable amounts. z Importance of the study of meteors and fireballs: – Fireball networks: Valuable data on atmospheric interaction and survival of • Are slow cometary meteoroids efficiently delivering organics and water to the Earth? • Orbital information of meteorites: asteroidal and cometary (?) parent bodies. – Meteor spectroscopy provides new interesting information • Chemical composition of meteoroids coming from a large variety of sources • Complementary source of chemical data compared to sample-return missions