Search

This book is an attempt to blend an extended and cross-disciplinary research paper about an initially neglected obscure cosmic dust contamination of the early Earth into a kind of cosmic detective investigation, which should be comprehensible by the space sciences community and undergraduate students in general. The major objectives were to: [ABSTRACT FROM AUTHOR]

Surprising EMMA. The main star of this book, besides the Moon, is an obscure contamination of the young Earth that was falling from the sky. It was mostly deposited by invisible tiny cosmic dust grains that can hardly be felt between two fingers. It was neglected for a long time because its composition and the variation of its mass flux with time were not tractable. Therefore, its effects could not be predicted. [ABSTRACT FROM AUTHOR]

This section includes a heteroclite set of questions and comments of colleagues, which have still to be fully answered. Progress in science occurs not only with a few spectacular achievements that are generally cleverly advertised by funding agencies and the prestigious journals, but also by incessant questioning. They remain in the shadow for a while because you have to wait for an answer that might never come. [ABSTRACT FROM AUTHOR]

A world of "hot" spots. Until the very recent reports of Yada et al. (2004, 2005) individual tiny interstellar dust grains (stardust) were only sought in meteorites and SMMs. This is a diffcult study, which is based on the search for isotopic anomalies in tiny submicron-sized grains with ion analyzers. [ABSTRACT FROM AUTHOR]

Any study of micrometeorites involves a variety of biases, which start right away during their collection, and which have not been suffciently publicized. This section deals with the astonishing folklore of these biases. We shall question whether major differences observed between Antarctic micrometeorites and stratospheric micrometeorites could reflect kinds of complementary biases between the two collections of micrometeorites. Astonishingly, some of them would converge to enrich the SMMs collection in the most fine-grained fluffy dust particles accreted by the Earth. They might be possibly the most primitive material accreted by the Earth. But they would not give a representative sampling of the bulk micrometeorite flux, which is best obtained with the new Concordia micrometeorites collected in central Antarctica. For a change, biases developing around a small metallic plate flying at ~200m/sec in the stratosphere turned out to be quite helpful! [ABSTRACT FROM AUTHOR]

In Sect. 5.2, we quoted the excitement about tiny micrometeorites collected in the stratosphere (SMMs) with a collector plate coated with an approximately 100 μm-thick silicone oil layer, which was fixed under the wing of a stratospheric aircraft of NASA. As pointed out by Jessberger et al. (2001), "due to contamination and collection limitations most of the SMMs have been limited to the 5 to 25μm diameter range". Messenger (2000) describes these SMMs as:"diverse assemblage of materials, which are commonly very finegrained (~0.1 μm), heterogeneous and rich in volatile elements and carbon relative to all meteorite classes". [ABSTRACT FROM AUTHOR]

Colleagues still have trouble understanding how the dominant relationship between CM-type chondrites and AMMs was established. They also wonder about the meaning of this relationship in terms of solar system history, and they generally expect that it has been markedly altered upon atmospheric entry, except for the smallest particles collected in the stratosphere. They are also confused when hearing that in spite of strong similarities there are also marked differences between these two varieties of solar system materials. Consequently, some of them believe that this relationship has not been convincingly established. This section mostly relies on arguments already presented by Kurat and Maurette (1997) in a book published in French, which have only been improved recently through the analysis of the Concordia Antarctic micrometeorites (Duprat et al., 2003 and 2004). [ABSTRACT FROM AUTHOR]

The constraint of grain sizes. The discussion presented in the last section suggests that Antarctic micrometeorites would dominantly originate from comets. However, they contain refractory inclusions made of refractory oxides (Fig. 46), abbreviated as CAIs (see Sect. 6.2), which can only be formed at the highest temperatures (T ≥ 1800 K) close to the early Sun. They are at least 10 times larger than the very small inclusions of refractory oxides (sizes of about 0.1-1 μm) observed in the most fine-grained SMMs belonging to the group of the chondritic-porous aggregates (see Zinner, 2004). In contrast, micrometeorite CAIs are smaller than those observed in CM-type HCCs (Gounelle et al., 2001), which are in turn about 10 times smaller than those observed in the "dry" carbonaceous chondrites (including the CV, CO and CK types), where they can reach a size of about 1 cm. [ABSTRACT FROM AUTHOR]

A French word, "errance" (the straightforward approximate English translation is wandering) well describes the functioning of the mind when you do not know where you are going. You feel dumb just knowing that you will probably end up somewhere else. Then, you bury this shameful weakness of your neuronal system in the deepest secrecy and start again hunting for good data. However, this is an essential step of scientific inquiry, which is illustrated here below just wandering about the meaning of lunar cratering rates and the origin of comets, which are intimately interwoven with the early history of the solar system and in particular with the phenomenon of debris disk around stars. [ABSTRACT FROM AUTHOR]

The application of the accretion formula to the Earth-Moon system does not require the identification of the parent bodies of micrometeorites (i.e., asteroids or comets). However, this identification is necessary to better extrapolate this formula to other terrestrial planets, such as Mars. One would also like to understand how the invariant composition of micrometeorites constrains the nature of their parent bodies. We report on a few arguments that have not been thoroughly explored yet, and which run against the conventional view that most micrometeorites originate from the collisions and/or erosion of asteroids. The only remaining alternative is that they dominantly originate from comets. [ABSTRACT FROM AUTHOR]

In this section, EMMA is first extrapolated to the Moon, to hopefully get new clues about a confusing problem that people have failed to figure out since 1970. It deals with the so-called meteoritic contamination of the lunar crust in siderophile elements such as iridium, which was previously attributed to the crater-forming impactors and not to micrometeorites. We next move to Mars to try to check whether EMMA can account for the high sulfur and nickel contents of Martian soils measured with instruments carried by the rovers Spirit and Opportunity in 2004. Before 1999, this obscure contamination looked at first glance to be of a limited interest. Consequently, it was neglected in earlier works. We discovered recently that the true reason for this neglect was probably that the description of this contamination on the Moon and Mars requires facing an astonishing diversity of very dificult problems in planetology, in which we became bogged down. But it was too late to quit. [ABSTRACT FROM AUTHOR]

The basic time frame of EMMA is the formation time interval of the Earth, Δ(Earth) ~ 100 Myr. This value has been estimated from both the 129I- 129Xe radioactive chronometer (Pepin and Phinney, 1975; Staudacher and Allègre 1982) and modern theories about the formation of the Earth initiated by Wetherill (1994) -for a recent summary see Canup and Agnor (2000). In this scenario, the composition of the Earth's atmosphere reported in Table 1 would give the average composition of about 1000 billions of billions of billions (e.g., ~1030) of juvenile IDPs captured by the Earth after the formation of the Moon, and representing a total mass of material of ~5.1024 g. Amazingly, this composition turns to be quite similar to that of an aliquot of about 500 AMMs with sizes of around 100.200 μm, amounting to a few milligrams of material, that we used to infer the composition of a "micrometeoritic" atmosphere. [ABSTRACT FROM AUTHOR]

Ozima and Podosek (2002) clearly state: "In summary, there is still no satisfactory theory on the origin of terrestrial noble gases". This view is also supported by Porcelli and Pepin (2000), who note: "there still is no consensus on how the terrestrial noble gases originated". Two of the major problems with the distribution of noble gases on the Earth concern: [ABSTRACT FROM AUTHOR]

On the Earth, an astonishing balance between the absorption and scattering of solar radiation by the early Earth produced the remarkable benign greenhouse effect favourable to the origin and evolution of life. Indeed, the first constraint on any scenario is that the early oceans were not boiling or freezing! It is generally considered that the temperature has to be sufficiently high to prevent freezing at a time when the solar luminosity was smaller than today. But it has to be kept sufficiently low by some mysterious feedback effect, in order to protect the Earth from a runaway greenhouse effect, which led to a surface temperature of about 450 °C on Venus. In fact, the long-lasting micrometeorite thermospheric volcanism effective after the Moon-forming impact, should have ruled the post-lunar greenhouse effect that was critical for the birth of life. Indeed, this impact eradicated at once all atmospheric ingredients of the pre-lunar greenhouse effect at a time when the young Earth was already almost fully outgassed. Subsequently, micrometeorites released simultaneously greenhouse gases for heating and smoke particles for cooling. These micrometeorite ashes resided temporarily within a kind of giant thermospheric cocoon, which might have functioned as a self-regulating IR heater during the period of low solar luminosity. Indeed, it was simultaneously heated up from the inside through the aerodynamical braking of micrometeorites. [ABSTRACT FROM AUTHOR]

About 80% of the Cap-Prudhomme AMMs collected near the margin of the Antarctic ice sheets showed anomalous low sulfur contents (~0.1%) with regard to the value of ~ 3% measured in CM chondrites, to which about 95% of these AMMs are related. We thought first, like everybody, that sulfur, which is quoted as the most volatile of the moderately volatile elements, would have been lost upon frictional heating upon atmospheric entry. But then, why is it that Ca, which is the most refractory element, would have also been lost? Moreover, there was no size effect in the loss of S and Ca going from 200 μm to 30μm size grains. This runs against frictional heating, which increases with particle sizes. Therefore Kurat deduced that sulfur, Ca and Ni could have been preferentially lost during "cryogenic-Cweathering" effective in the first top meter of blue ice fields near the sea shore, involving the preferential leaching of carbonates, sulphates and sulfides (Maurette et al. 1992). [ABSTRACT FROM AUTHOR]

In this section micrometeorites are further divided in two distinct families: [ABSTRACT FROM AUTHOR]

Maurette (1998a and 1998b) gives a more detailed discussion of previous works supporting the role of unmelted micrometeorites in prebiotic chemistry. Krueger and Kissel (1987) quoted thermodynamic computations suggesting that the μm-size C-rich grains that they discovered in the tail of Halley's comet with their time-of-flight mass spectrometer on board the Vega spacecraft, when added to a prebiotic soup of organics, could trigger the formation of nucleic acids. Anders (1989) relied on the characteristics of the tiny stratospheric micrometeorites with sizes of about 5-15 μm, which amount to less than about 1% of the micrometeorite mass flux, to argue that micrometeorites played a major role in the delivery of organics to the Earth. As first quoted by Ponchelet (1989), we proposed in 1989 that much larger micrometeorites, similar to Antarctic micrometeorites, might have been functioning as individual microscopic chemical reactors on the early Earth during their interactions with gases and waters (Maurette et al., 1990, 1991b, 1998a, 1998b). Subsequently, Chyba and Sagan (1992) ceased fully supporting the role of the direct impact of comets in the delivery of such organics, and started to refer that of micrometeorites. [ABSTRACT FROM AUTHOR]

Exobiology is a multidisciplinary science that deals with the origin and early evolution of life. For the birth of life to occur, the setting of its cosmic cradle has to be right. The first step is to make early seas and to buildup a benign greenhouse effect that prevents their freezing and/or boiling. Next, an efficient prebiotic chemistry has to operate in this water to synthesize the key macromolecules that could start dividing, thus giving the first sketch of life. This synthesis requires: energy; liquid water; salts like phosphate; organic molecules such as amino acids; mineral surfaces behaving like catalysts of their reaction; etc. [ABSTRACT FROM AUTHOR]

The early Earth's atmosphere was much more massive than today. Before the condensation of water and the subsequent dissolution of CO2that precipitated into carbonates, the partial pressures of H2O and CO2were about 270 bars and 60 bars, respectively. Today, planetary exploration has revealed that the atmospheres of 8 planets and 3 of their approximately 120 satellites have a structure rather similar to that deduced from the vertical temperature profile of the contemporary Earth's atmosphere, which shows that the temperature alternately decreases and increases with height (troposphere, stratosphere, mesosphere, and thermosphere). In particular, because the giant planets and Venus are all topped by a high-temperature low-density thermosphere (Dowling, 1999), we can safely assume that the early Earth had also a thermosphere. [ABSTRACT FROM AUTHOR]

The chemical composition of the Earth's atmosphere can be defined by the Ne/N2,H2O/N2and CO2/N2ratios deduced from the total amounts of these four volatiles in the atmosphere. The same volatiles are released by hydrous-carbonaceous micrometeorites upon frictional heating as to generate a micrometeoritic model atmosphere. Its composition is inferred from the weight % contents of Ne, N2,H2O and carbon that were measured in about 500 Antarctic micrometeorites from the 100-200 μm size fraction. The composition of the micrometeoritic atmosphere was thus found to be strikingly similar to that of our blue planet. [ABSTRACT FROM AUTHOR]

According to the definition of Ozima and Podosek (2002), the Earth's atmosphere refers to all volatiles in surface reservoirs, including air, water and sedimentary rocks such as carbonates in which early CO2 is now trapped. [ABSTRACT FROM AUTHOR]

Micrometeorites and meteorites.The mass flux (number of tons, per year, for the whole Earth) of meteorites and micrometeorites can be estimated, both before and after atmospheric entry, from the works of Haliday et al. (1989), Zolensky et al. (1992), Love and Brownlee (1993), Bland et al. (1996), Hammer and Maurette (1996), Gounelle et al. (1999) and Duprat et al. (2003, 2004). [ABSTRACT FROM AUTHOR]

Archeologists only started to trace back successfully the advance of the Roman legions, trade patterns and the evolution of manufacturing techniques in Roman time, once they found an efficient scheme of classification for the fragments of amphora used to transport wine for the soldiers. Similarly, the classification of meteorites and micrometeorites is an essential step in the exploitation of these extraterrestrial debris. We recall that one of the main objectives of meteoriticists over the last 30 years was to find the most primitive objects of the solar system, which have been the least reprocessed since the formation of the early solar nebula, with the view to exploit them as reliable archivist of our distant past. This section outlines some of the methods used to classify meteorites and Antarctic micrometeorites. It also summarizes some of the key features of the surprisingly simple relationship between micrometeorites and a relatively rare group of stony meteorites, the hydrous-carbonaceous CM-type chondrites, which was only confirmed recently after the study of the Concordia micrometeorites collected in central Antarctica in January 2002. A more technical discussion of this relationship presented in Sect. 25 will allow its extension to the smaller micrometeorites collected by NASA in the stratosphere. The book of Wasson (1985) is still one of the best monographs about meteorites. [ABSTRACT FROM AUTHOR]

When they are ejected into the interplanetary medium during interasteroidal collisions, meteorites have a limited lifetime in space, which is scaled by their "cosmic-ray exposure ages" inferred from the concentrations of cosmogenic nuclides such as 3He, 21Ne and 38Ar, produced during the nuclear reactions of galactic cosmic rays with the constituent atoms of meteorites. Such ages range from about 10 to 500 Myr, with the notable exception of the shorter age of the CI- and CM-type hydrous-carbonaceous chondrites (see Sect. 22.3). Consequently, meteorites have to be constantly replenished upon interasteroidal collisions. [ABSTRACT FROM AUTHOR]

In accordance with Ozima and Podosek (2002), atmosphere will refer to all volatiles in surface reservoirs of the Earth, including air but also liquid and frozen water and sedimentary rocks, such carbonates, where early CO2is now trapped. Today, around 90% of the mass of air is found in the first six kilometers of the thick gaseous envelope of the Earth which extends to about 800 km, the altitude beyond which the magnetosphere exists. The mass of the oceans, which amount to about 97.2% of all terrestrial waters, would be equivalent to an aproxmately 2.7 km thick "film" of liquid water around the Earth (i.e., about 0.04% of the Earth's radius). For a comparison, the total mass of terrestrial living organisms would represent an equivalent thickness of around 10 cm and if the Earth was reduced to the size of an orange the oceans would represent one drop of water. [ABSTRACT FROM AUTHOR]

Many observations remind us that the Earth-Moon system has been bombarded by projectiles covering a wide size range between submicrometer particles to the giant Mars-sized body that did form the Moon during its impact with the proto-Earth. They include: [ABSTRACT FROM AUTHOR]

Planets and small bodies. Besides the Sun, which represents about 99.85% of its mass, the present day solar system include large bodies, i.e., the four terrestrial planets, the four giant planets, and Pluto, which is probably not a planet, but rather an object from the Edgeworth-Kuiper belt of comets captured by Neptune; more than 130 satellites of the planets. Jupiter, the most massive planet of the solar system, is about 320 times more massive than the Earth, which weighs about 80 lunar masses. Its orbit separates the two very distinct worlds of the inner solar system, populated by rocky bodies, from the outer solar system, which is the world of the giant gaseous planets, icy bodies and intense coldness, which starts at around 5 astronomical units (AU) from the Sun and ends up at 50,000 AU with the outer edge of the Oort cloud of comets -one AU is the average distance between the Earth and the Sun, of about 150 millions of km. [ABSTRACT FROM AUTHOR]

Prediction of iridium content. Iridium is a highly siderophile element. Accordingly to a conventional scenario (c.f., Sect. 3.5), this element was initially stored in both the planetesimals that formed the proto-Earth and the half-dozen planetary embryos (i.e., proto-planets) that subsequently merged into it. Each of these bodies, which were not fully decelerated before their impact with the Earth's surface, exploded. This led to the production of pockets of liquid silicates in which "droplets" of liquid iron nucleated. They ended up coagulating in huge metal masses that quickly sank to the core. Therefore, it can be expected that the Mars-sized Moon-forming impact, which occurred at time t1 ~ 4.44 Gyr, was scavenging any residual iridium to the core, thus preparing a new niche for the accumulation of micrometeoritic iridium. [ABSTRACT FROM AUTHOR]

It is generally assumed that oxygen appeared much later in the history of the Earth, during the (Great Oxidation Event), GOE which lasted about 150 Myr, about 2 Gyr ago. But the causes of the GOE are still debated. For a long time, it was thought that it resulted from the biogenic activity of photosynthetic early life forms, which decomposed a fraction of the atmospheric CO2to extract the carbon necessary to their growth. But Holland (2002) now argues that it might be associated with complex changes in the composition of volcanic gases! The fate of the fraction oxygen resulting from the photodissociation of micrometeoric water vapour in the early thermosphere, during the peak of the PHBomb, was not decrypted, yet. The unsolved problem is to trace back its reaction network with early materials. [ABSTRACT FROM AUTHOR]

Jupiter is a gigantic gravitational sling that can alter the orbits of small bodies while triggering their "chaotic" diffusion. This property was used to fly the spacecraft Ulysses around the solar poles. Ulysses was not fired directly to the Sun but to Jupiter, which did sling it back to the Sun, thus saving the spacecraft a lot of energy. [ABSTRACT FROM AUTHOR]

About 75% of the incoming micrometeorites are destroyed upon atmospheric entry, being either volatilized or transformed into dry cosmic spherules. In 1998, Cécile Engrand got the first strong hint that the ashes of these "dead" micrometeorites might also have contributed to exobiology. She found that the isotopic composition of the water "ash" that they released in the thermosphere gives the best fit to the standard SMOW value measured for an average of the terrestrial oceans (Sect. 9.2). Consequently, they contributed to exobiology, at least through the delivery of the basic fluid of life, water. [ABSTRACT FROM AUTHOR]