Bonal, Lydie (1980-....).
Overview
| Works: | 5 works in 7 publications in 1 language and 7 library holdings |
|---|---|
| Roles: | Opponent, Author, Thesis advisor, Other |
Publication Timeline
.
Most widely held works by
Lydie Bonal
Matière organique et métamorphisme thermique dans les chondrites primitives by
Lydie Bonal(
)
3 editions published in 2006 in French and held by 2 WorldCat member libraries worldwide
The Organic Matter of primitive chondrites is inherited from the presolar cloud, but the chondritic OM have suffered from secondary processes inside the proto-solar nebula and on their asteroidal parent body (Aqueous Alteration, Thermal Metamorphism), that may erase or transform the initial characteristics. The TM has been approached here from OM, which is irreversibly transformed by TM. More than 30 chondrites (CV3, CO3, UOC) have been studied : structure of the OM has been quantified by Raman spectroscopy, the texture by HRTEM. Petrographic studies have also been done on each chondrite. A new interclass metamorphic tracer is defined : consistent with other ones available in the litterature, independant from the AA and sensitive to the Peak Metamorphic Temperature. For the most metamorphosed chondrites, the PMT is evaluated from the structural grade of the OM : 330°C (Allende), consistent with other available thermometers. The limitations of the commonly defined petrographic scale are shown and a new one based on a Raman spectral parameter is defined. A precise evaluation of the metamorphic grade of the chondrites allows to discriminate the nebular from the asteroidal effects induced on the petrography. This work gives also some constraints to the models of formation of the chondritic OM. It shows that the organic precursor from ordinary and carbonaceous chondrites are chemically and structurally closed and that the understanding of the isotopic characteristics from the OM (D, 15N) requires to take into account the effects induced by the secondary processes. This work favors an interstellar origin of the precursor of the chondritic OM
3 editions published in 2006 in French and held by 2 WorldCat member libraries worldwide
The Organic Matter of primitive chondrites is inherited from the presolar cloud, but the chondritic OM have suffered from secondary processes inside the proto-solar nebula and on their asteroidal parent body (Aqueous Alteration, Thermal Metamorphism), that may erase or transform the initial characteristics. The TM has been approached here from OM, which is irreversibly transformed by TM. More than 30 chondrites (CV3, CO3, UOC) have been studied : structure of the OM has been quantified by Raman spectroscopy, the texture by HRTEM. Petrographic studies have also been done on each chondrite. A new interclass metamorphic tracer is defined : consistent with other ones available in the litterature, independant from the AA and sensitive to the Peak Metamorphic Temperature. For the most metamorphosed chondrites, the PMT is evaluated from the structural grade of the OM : 330°C (Allende), consistent with other available thermometers. The limitations of the commonly defined petrographic scale are shown and a new one based on a Raman spectral parameter is defined. A precise evaluation of the metamorphic grade of the chondrites allows to discriminate the nebular from the asteroidal effects induced on the petrography. This work gives also some constraints to the models of formation of the chondritic OM. It shows that the organic precursor from ordinary and carbonaceous chondrites are chemically and structurally closed and that the understanding of the isotopic characteristics from the OM (D, 15N) requires to take into account the effects induced by the secondary processes. This work favors an interstellar origin of the precursor of the chondritic OM
Etude d'une série de micrométéorites antarctiques : caractérisation multi-analytique et comparaison à des chondrites
carbonées by
Manon Battandier(
)
1 edition published in 2018 in French and held by 2 WorldCat member libraries worldwide
L'étude des petits corps de système solaire (astéroïdes et comètes), qui se sont formés il y a 4.567 milliards d'années, nous renseigne sur les matériaux initialement présents dans la nébuleuse solaire et sur les processus opérants dans le système solaire primitif. Cette étude peut être notamment menée par l'analyse de cosmomatériaux dits primitifs, telles que des météorites (principalement les chondrites), des poussières interplanétaires (IDPs) ou encore des micrométéorites.Ce travail de thèse consiste en une multi-analyse d'une série de 58 micrométéorites antarctiques (AMMs) provenant de la collection CONCORDIA 2006 et 2016. Parmi elles, différents types texturaux reflétant les différents degrés de chauffage subi durant l'entrée atmosphérique sont représentés: 40 particules non fondues à grains fins (Fgs), 12 particules intermédiaires partiellement fondues (Fg-Scs), 1 particule partiellement fondue scoriacée (Sc) et 5 sphérules cosmiques complètement fondues (CSs). Les échantillons ont été étudiés par différentes méthodes analytiques: i) par spectroscopie Raman, permettant ici d'étudier la structure de la matière organique polyaromatique; ii) par spectroscopie IR, permettant ici d'étudier la matière organique essentiellement aliphatique ainsi que l'état d'hydratation et la minéralogie des échantillons; et 3) par spectrométrie de masse à ionisation secondaire (NanoSIMS), utilisée ici pour mesurer la composition isotopique du carbone et de l'azote de la matière organique contenue dans les AMMs. Dans le but de contraindre la diversité des corps parents échantillonnés par les cosmomatériaux, des chondrites carbonées de types 1 et 2 CM, CR et CI sont également étudiées.La combinaison des caractérisations Raman et IR a permi de mettre en évidence des différences entre les AMMs, en terme d'abondance, de structure et de composition chimique de la matière organique, de minéralogie et d'état d'hydratation. En particulier, 7 Fgs se distinguent des autres AMMs de part: i) une minéralogie hydratée avec phyllosilicates, ii) une richesse en matière organique polyaromatique et aliphatique, iii) une structure de la matière organique polyaromatique différente. Des expériences de chauffage, mises en place dans le présent travail, sur des grains de matrice de chondrites carbonées CM, CR, CI montrent que la traversée atmosphérique peut induire: la déshydratation des échantillons, une diminution de l'abondance en matière organique et une modification structurale de la matière organique polyaromatique. L'identification de 17 Fgs non hydratées montre que malgré une texture à grains fins, certaines Fgs peuvent avoir subi un chauffage significatif durant l'entrée atmosphérique. Les 7 Fgs identifiées apparaissent alors comme celles ayant été le moins modifiées par la traversée atmosphérique et sont donc les plus primitives de notre série. De plus, cette étude montre que l'état d'hydratation, la minéralogie et la matière organique sont des traceurs encore plus sensibles au chauffage subi lors de la traversée atmosphérique que la texture des micrométéorites.Des différences propres, ne s'expliquant pas par le chauffage atmosphérique, sont révélées entre les 7 Fgs hydratées et les chondrites carbonées CM, CR, CI étudiées. Ces différences sont: i) une signature spectrale spécifique des silicates en IR, ii) une richesse en matière organique aliphatique et iii) des caractérisques différentes de la matière organique aliphatique. De plus, l'analyse des compositions isotopiques du carbone et de l'azote montre une grande variabilité des rapports isotopiques parmi les AMMs contrairement aux observations dans les chondrites carbonées. Ces différences propres sont ici interprétées par l'échantillonnage de corps parents différents entre AMMs et chondrites carbonées
1 edition published in 2018 in French and held by 2 WorldCat member libraries worldwide
L'étude des petits corps de système solaire (astéroïdes et comètes), qui se sont formés il y a 4.567 milliards d'années, nous renseigne sur les matériaux initialement présents dans la nébuleuse solaire et sur les processus opérants dans le système solaire primitif. Cette étude peut être notamment menée par l'analyse de cosmomatériaux dits primitifs, telles que des météorites (principalement les chondrites), des poussières interplanétaires (IDPs) ou encore des micrométéorites.Ce travail de thèse consiste en une multi-analyse d'une série de 58 micrométéorites antarctiques (AMMs) provenant de la collection CONCORDIA 2006 et 2016. Parmi elles, différents types texturaux reflétant les différents degrés de chauffage subi durant l'entrée atmosphérique sont représentés: 40 particules non fondues à grains fins (Fgs), 12 particules intermédiaires partiellement fondues (Fg-Scs), 1 particule partiellement fondue scoriacée (Sc) et 5 sphérules cosmiques complètement fondues (CSs). Les échantillons ont été étudiés par différentes méthodes analytiques: i) par spectroscopie Raman, permettant ici d'étudier la structure de la matière organique polyaromatique; ii) par spectroscopie IR, permettant ici d'étudier la matière organique essentiellement aliphatique ainsi que l'état d'hydratation et la minéralogie des échantillons; et 3) par spectrométrie de masse à ionisation secondaire (NanoSIMS), utilisée ici pour mesurer la composition isotopique du carbone et de l'azote de la matière organique contenue dans les AMMs. Dans le but de contraindre la diversité des corps parents échantillonnés par les cosmomatériaux, des chondrites carbonées de types 1 et 2 CM, CR et CI sont également étudiées.La combinaison des caractérisations Raman et IR a permi de mettre en évidence des différences entre les AMMs, en terme d'abondance, de structure et de composition chimique de la matière organique, de minéralogie et d'état d'hydratation. En particulier, 7 Fgs se distinguent des autres AMMs de part: i) une minéralogie hydratée avec phyllosilicates, ii) une richesse en matière organique polyaromatique et aliphatique, iii) une structure de la matière organique polyaromatique différente. Des expériences de chauffage, mises en place dans le présent travail, sur des grains de matrice de chondrites carbonées CM, CR, CI montrent que la traversée atmosphérique peut induire: la déshydratation des échantillons, une diminution de l'abondance en matière organique et une modification structurale de la matière organique polyaromatique. L'identification de 17 Fgs non hydratées montre que malgré une texture à grains fins, certaines Fgs peuvent avoir subi un chauffage significatif durant l'entrée atmosphérique. Les 7 Fgs identifiées apparaissent alors comme celles ayant été le moins modifiées par la traversée atmosphérique et sont donc les plus primitives de notre série. De plus, cette étude montre que l'état d'hydratation, la minéralogie et la matière organique sont des traceurs encore plus sensibles au chauffage subi lors de la traversée atmosphérique que la texture des micrométéorites.Des différences propres, ne s'expliquant pas par le chauffage atmosphérique, sont révélées entre les 7 Fgs hydratées et les chondrites carbonées CM, CR, CI étudiées. Ces différences sont: i) une signature spectrale spécifique des silicates en IR, ii) une richesse en matière organique aliphatique et iii) des caractérisques différentes de la matière organique aliphatique. De plus, l'analyse des compositions isotopiques du carbone et de l'azote montre une grande variabilité des rapports isotopiques parmi les AMMs contrairement aux observations dans les chondrites carbonées. Ces différences propres sont ici interprétées par l'échantillonnage de corps parents différents entre AMMs et chondrites carbonées
Minéralogie et composition isotopique des phases d'altération des premières roches du Système Solaire by
Dan Lévy(
)
1 edition published in 2019 in French and held by 1 WorldCat member library worldwide
1 edition published in 2019 in French and held by 1 WorldCat member library worldwide
Origine des éléments volatils et chronologie de leur accrétion au sein du Système Solaire interne : Apport de l'analyse
in-situ des achondrites by
Cécile Deligny(
)
1 edition published in 2021 in French and held by 1 WorldCat member library worldwide
Volatile elements such as hydrogen and nitrogen control the evolution of planetary bodies and their atmospheres, and are essential elements for the development of life on Earth. Nevertheless, the origin of volatile elements and the timing of their accretion by terrestrial planets formed in the inner solar system remains a subject of debate and controversy in planetary science. To answer these questions, the isotopic ratios of hydrogen (D/H) and nitrogen (15N/14N) are powerful tools to trace the origin (solar, chondritic or cometary) of volatile elements trapped in planetary bodies. Therefore, to constrain the source(s) of volatile elements trapped in rocky planets, we analyzed hydrogen and nitrogen contents and isotopic compositions by ion microprobe (LGSIMS) in achondrites that originate from asteroids or from planets that are assumed to have formed in the inner solar system. These meteorites preserve a record of the initial stages of the formation of their parent bodies and can constrain the early evolution of planetary volatile elements. In-situ analysis by SIMS is a quasi-non-destructive technique, which permits to measure the abundance and the isotopic composition of volatile elements of different phases in terrestrial, extraterrestrial and synthetic samples. The recent development of the protocol of nitrogen analysis in silicate samples by ion probe allows us to target tens of micron- sized objects (i.e., glassy melt inclusions). Volatile elements were measured in melt inclusions trapped in minerals and in interstitial glasses. Although the analysis of nitrogen in aubrites was unsuccessful, the analysis performed on Martian meteorites and angrites revealed the presence of a large amount of water and nitrogen within these meteorites. In particular, the study of angrites and more precisely the meteorite D'Orbigny allowed us to highlight the presence of water and nitrogen having isotopic composition similar to those of the primitive meteorites formed in the outer solar system (i.e., CM-like carbonaceous chondrites). These results imply that these volatile elements must have been present in the inner solar system within the first ~4 Ma after CAI formation (i.e., the first solids to form in the solar system) and may have been trapped by the terrestrial planets during their formation. Furthermore, the analysis of Martian meteorites and more particularly of Chassigny revealed the presence of nitrogen with an isotopic composition enriched in 15N compared to enstatite chondrites and terrestrial diamonds which are believed to record the most primitive value of nitrogen on Earth
1 edition published in 2021 in French and held by 1 WorldCat member library worldwide
Volatile elements such as hydrogen and nitrogen control the evolution of planetary bodies and their atmospheres, and are essential elements for the development of life on Earth. Nevertheless, the origin of volatile elements and the timing of their accretion by terrestrial planets formed in the inner solar system remains a subject of debate and controversy in planetary science. To answer these questions, the isotopic ratios of hydrogen (D/H) and nitrogen (15N/14N) are powerful tools to trace the origin (solar, chondritic or cometary) of volatile elements trapped in planetary bodies. Therefore, to constrain the source(s) of volatile elements trapped in rocky planets, we analyzed hydrogen and nitrogen contents and isotopic compositions by ion microprobe (LGSIMS) in achondrites that originate from asteroids or from planets that are assumed to have formed in the inner solar system. These meteorites preserve a record of the initial stages of the formation of their parent bodies and can constrain the early evolution of planetary volatile elements. In-situ analysis by SIMS is a quasi-non-destructive technique, which permits to measure the abundance and the isotopic composition of volatile elements of different phases in terrestrial, extraterrestrial and synthetic samples. The recent development of the protocol of nitrogen analysis in silicate samples by ion probe allows us to target tens of micron- sized objects (i.e., glassy melt inclusions). Volatile elements were measured in melt inclusions trapped in minerals and in interstitial glasses. Although the analysis of nitrogen in aubrites was unsuccessful, the analysis performed on Martian meteorites and angrites revealed the presence of a large amount of water and nitrogen within these meteorites. In particular, the study of angrites and more precisely the meteorite D'Orbigny allowed us to highlight the presence of water and nitrogen having isotopic composition similar to those of the primitive meteorites formed in the outer solar system (i.e., CM-like carbonaceous chondrites). These results imply that these volatile elements must have been present in the inner solar system within the first ~4 Ma after CAI formation (i.e., the first solids to form in the solar system) and may have been trapped by the terrestrial planets during their formation. Furthermore, the analysis of Martian meteorites and more particularly of Chassigny revealed the presence of nitrogen with an isotopic composition enriched in 15N compared to enstatite chondrites and terrestrial diamonds which are believed to record the most primitive value of nitrogen on Earth
Composition isotopique des éléments légers dans les micrométéorites ultracarbonées par spectrométrie de masse à émission
ionique secondaire à haute résolution en masse, contribution à la connaissance des surfaces cométaires by
Noémie Bardin(
)
1 edition published in 2015 in French and held by 1 WorldCat member library worldwide
This thesis covers the isotopic analysis of carbon-rich interplanetary dust (ultracarbonaceous micrometeorites), in order to better understand the isotopic fractionation process of light elements (hydrogen and nitrogen) observed in the organic phases of primitive extraterrestrial matter. It is possible, within a collection of micrometeorites coming from the central regions of the Antarctic continent, to identify ultra-carbonaceous micrometeorites (UCAMMs - for Ultra-Carbonaceous Antarctic MicroMeteorites) which contain about ten times more carbon than the primitive meteorites. These particles are extremely rare and open the possibility to study in laboratory cometary particles of large sizes (100-200 microns). This thesis focuses on the isotopic analyses of UCAMMs, in order to understand the isotopic fractionation processes of light elements (hydrogen and nitrogen) observed in the organic matter of the primitive solar system. Mineralogical, chemical and structural analyses on two fragments of ultra-carbonaceous micrometeorites were performed in the framework of collaborations using techniques of scanning electron microscopy, electron microprobe, infrared microspectroscopy (SOLEIL synchrotron). The main work of this thesis concerns the isotopic analysis of two UCAMMs by Secondary Ion Mass Spectrometry (SIMS) using the NanoSIMS ion microprobe. The instrumental developments performed in collaboration between the CSNSM and the Curie Institute teams allow to resolve molecular interferences with a mass resolving power higher than 20 000 retaining a sensibility compatible with the measurements considered here. So, it has been possible to measure for the first time the hydrogen isotopic composition with the polyatomic ions 12C2D- and 12C2H- and to compare its spatial distribution with that of the nitrogen (12C15N-/12C14N-) obtained on the same surface with the same magnetic field. A protocol for producing a series of standard samples was developed from polymers isotopically enriched in deuterium in order to determine the instrumental fractionation of the NanoSIMS showing the possibility to perform precise measurements of the hydrogen isotopic composition in the organic matter with polyatomic ions (CD-/CH- and C2D-/C2H- ratios). The isotopic maps at high spatial resolution (200 nm) in C2D/C2H and C15N/C14N show a very heterogeneous distribution in deuterium with extreme values going up to 20 times the terrestrial ocean value, whereas the 15N/14N ratios remain globally close (within 20%) to the terrestrial atmosphere value. Measurements of N/C ratios in ion imaging performed at the NanoSIMS confirm the values measured by electron microprobe and show that the organic matter of UCAMMs is rich in nitrogen. Comparisons between isotopic images with each other and with the images obtained by the other techniques show that the organic matter of ultracarbonaceous micrometeorites is constituted of different components. The main component doesn't exhibit a correlation between the D and 15N excesses. A minor component of the analyzed surface exhibits correlated excesses in D and in 15N, without neither the elemental or structural composition of this component significantly differs from the rest of the grain. Finally, a minor component showing moderate enrichments in D and 15N/14N ratios lower than the terrestrial atmosphere value could have been identified.All the data can be explained assuming that the ultracarbonaceous micrometeorites come from the surface of transneptunian icy objects. The elemental and isotopic characteristics observed in the organic matter of UCAMMs might result from the mixing of different strata of the parent body having undergone irradiation by the galactic cosmic radiation at large heliocentric distances
1 edition published in 2015 in French and held by 1 WorldCat member library worldwide
This thesis covers the isotopic analysis of carbon-rich interplanetary dust (ultracarbonaceous micrometeorites), in order to better understand the isotopic fractionation process of light elements (hydrogen and nitrogen) observed in the organic phases of primitive extraterrestrial matter. It is possible, within a collection of micrometeorites coming from the central regions of the Antarctic continent, to identify ultra-carbonaceous micrometeorites (UCAMMs - for Ultra-Carbonaceous Antarctic MicroMeteorites) which contain about ten times more carbon than the primitive meteorites. These particles are extremely rare and open the possibility to study in laboratory cometary particles of large sizes (100-200 microns). This thesis focuses on the isotopic analyses of UCAMMs, in order to understand the isotopic fractionation processes of light elements (hydrogen and nitrogen) observed in the organic matter of the primitive solar system. Mineralogical, chemical and structural analyses on two fragments of ultra-carbonaceous micrometeorites were performed in the framework of collaborations using techniques of scanning electron microscopy, electron microprobe, infrared microspectroscopy (SOLEIL synchrotron). The main work of this thesis concerns the isotopic analysis of two UCAMMs by Secondary Ion Mass Spectrometry (SIMS) using the NanoSIMS ion microprobe. The instrumental developments performed in collaboration between the CSNSM and the Curie Institute teams allow to resolve molecular interferences with a mass resolving power higher than 20 000 retaining a sensibility compatible with the measurements considered here. So, it has been possible to measure for the first time the hydrogen isotopic composition with the polyatomic ions 12C2D- and 12C2H- and to compare its spatial distribution with that of the nitrogen (12C15N-/12C14N-) obtained on the same surface with the same magnetic field. A protocol for producing a series of standard samples was developed from polymers isotopically enriched in deuterium in order to determine the instrumental fractionation of the NanoSIMS showing the possibility to perform precise measurements of the hydrogen isotopic composition in the organic matter with polyatomic ions (CD-/CH- and C2D-/C2H- ratios). The isotopic maps at high spatial resolution (200 nm) in C2D/C2H and C15N/C14N show a very heterogeneous distribution in deuterium with extreme values going up to 20 times the terrestrial ocean value, whereas the 15N/14N ratios remain globally close (within 20%) to the terrestrial atmosphere value. Measurements of N/C ratios in ion imaging performed at the NanoSIMS confirm the values measured by electron microprobe and show that the organic matter of UCAMMs is rich in nitrogen. Comparisons between isotopic images with each other and with the images obtained by the other techniques show that the organic matter of ultracarbonaceous micrometeorites is constituted of different components. The main component doesn't exhibit a correlation between the D and 15N excesses. A minor component of the analyzed surface exhibits correlated excesses in D and in 15N, without neither the elemental or structural composition of this component significantly differs from the rest of the grain. Finally, a minor component showing moderate enrichments in D and 15N/14N ratios lower than the terrestrial atmosphere value could have been identified.All the data can be explained assuming that the ultracarbonaceous micrometeorites come from the surface of transneptunian icy objects. The elemental and isotopic characteristics observed in the organic matter of UCAMMs might result from the mixing of different strata of the parent body having undergone irradiation by the galactic cosmic radiation at large heliocentric distances
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Related Identities
- Aléon, Jérôme Other Thesis advisor
- Remusat, Laurent Opponent
- Beck, Pierre (1980-....). Thesis advisor
- Engrand, Cécile Opponent
- École doctorale terre, univers, environnement (Grenoble) Other
- Battandier, Manon (1992-....). Author
- Institut de planétologie et d'astrophysique de Grenoble Other
- Deloule, Etienne (19..-....). Other Opponent Thesis advisor
- Djouadi, Zahia Other
- Communauté d'universités et d'établissements Université Grenoble Alpes Degree grantor