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. Durant-cette-thèse, aí etudié les effets des RCs sur l'ionisation de la phase gazeuse dans les nuages moléculaires. Notamment, les RCs ionisent H 2 et initient une série de réactions chimiques entre des ions moléculaires et des espèces neutres dans le nuage, Parce qu'ils augmentent l'abondance desélectronsdesélectrons, les RCs contrôlent aussi les processus de recombinaisonélectroniquerecombinaisonélectronique et donc les abondances des ions moléculaires

. Ainsi, les RCs contrôlent l'abondance de certaines espèces caractéristiques, appelées traceurs de l'ionisation

. Ceccarelli, traceurs de l'ionisation dans les nuages moléculaires proches de trois rémanents de supernova : W28, W51C et W44 Pour chacun de ces rémanents, des preuves observationnelles complémentaires de la présence de gaz choqué, ainsi que la détection d'´ emission gamma en provenance du nuage ? probablement induite par des protons relativistes ? démontrent l'existence d'une interaction avec le nuagè a proximité Dans la région du SNR W51C, des observationsàobservationsà haute résolution spatiale avec l'interféromètre du Plateau de Bure (IRAM) ont apporté la confirmation d'un fort taux d'ionisation, comme proposé par Elles ontégalementontégalement permis la détection d'´ emission compacte de SiO, qui révèle probablement le passage de l'onde de choc du SNR dans le gaz. Ces observations donnent ainsi une image cohérente d'une forte ionisation dans la région, dûè a la présence de RCs de bassé energie en aval du choc. Des observations complémentaires avec le télescope de 30m de l'IRAM ont permis d'une part de fournir les observations manquantesàmanquantesà courte base, et d'autre part de cartographier une zone autour de la position W51C-E,paralì element au choc. Il serait profitable d'obtenirégalementobtenirégalement une carte perpendiculaire au choc. En effet, nos observations de SiO suggèrent qu'il pourrait y avoir davantage de régions d'´ emission compacte le long de l'axe de propagation du choc. Une carte obtenue avec le 30m nous permettrait alors de définir d'autres régionsrégionsà explorer avec NOEMA. Dans la région du SNR W28, j'ai détectédétectéà l'aide du télescope de 30m de l'IRAM plusieurs lignes de visée proches de l'onde de choc avec des taux d'ionisation par les RCs au moins 100 fois supérieurssupérieursà la valeur standard. J'aí egalement identifié une position dans la région Sud, loin du choc, o` u l'ionisation est standard. Ces observations apportent la preuve de l'existence d'un très fort taux d'ionisation dans un nuage densè a proximité d'un SNR, qui peutêtrepeutêtre expliqué par la présence de RCs accélérés dans l'enveloppe du SNR. Elles apportentégalementapportentégalement des contraintes inédites sur les propriétés de diffusion des RCs, dans un domaine d'´ energie inaccessible aux autres techniques d'observation. Dans cetté etude, j'ai utilisé le rapport d'abondances DCO + /HCO + et identifié les limites de cette méthodè a haute ionisation. ` A cause de ces limites, il serait nécessaire d'identifier des traceurs de l'ionisation alternatifs. J'ai alors mené des observations complémentaires dans la région de W28 pour tenter d'identifier de tels traceurs. En m'appuyant sur une grille de modèles chimiques, Alors, enétudiantenétudiant ces traceurs, il est possible de donner des contraintes sur la valeur du taux d'ionisation par les RCs ?. La valeur considérée comme standard dans les nuages moléculaires est ? = 1 × 10 ?17 s ?1 . En associant observations et modélisation, j'aí etudié les abondances chimiques des, 2011.

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