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- W2567188867 abstract "Over the past decades star formation has been a very attractive field because knowledgeof star formation leads to a better understanding of the formation of planets andthus of our solar system but also of the evolution of galaxies. Conditions leading to theformation of high-mass stars are still under investigation but an evolutionary scenario hasbeen proposed: As a cold pre-stellar core collapses under gravitational force, the mediumwarms up until it reaches a temperature of 100 K and enters the hot molecular core (HMC)phase. The forming central proto-star accretes materials, increasing its mass and luminosityand eventually it becomes sufficiently evolved to emit UV photons which irradiatethe surrounding environment forming a hyper compact (HC) and then a ultracompact(UC) HII region. At this stage, a very dense and very thin internal photon-dominatedregion (PDR) forms between the HII region and the molecular core.Information on the chemistry allows to trace the physical processes occurring in thesedifferent phases of star formation. Formation and destruction routes of molecules areinfluenced by the environment as reaction rates depend on the temperature and radiationfield. Therefore, chemistry also allows the determination of the evolutionary stage ofastrophysical objects through the use of chemical models including the time evolution ofthe temperature and radiation field.Because HMCs host a very rich chemistry with high abundances of complex organicmolecules (COMs), several astrochemical models have been developed to study the gasphase chemistry as well as grain chemistry in these regions. In addition to HMCs models,models of PDRs have also been developed to study in particular photo-chemistry. So far,few studies have investigated internal PDRs and only in the presence of outflows cavities.Thus, these unique regions around HC/UCHII regions remain to be examined thoroughly.My PhD thesis focuses on the spatio-temporal chemical evolution in HC/UC HIIregions with internal PDRs as well as in HMCs. The purpose of this study is first tounderstand the impact and effects of the radiation field, usually very strong in theseregions, on the chemistry. Secondly, the goal is to study the emission of various tracersof HC/UCHII regions and compare it with HMCs models, where the UV radiation fielddoes not impact the region as it is immediately attenuated by the medium. Ultimately wewant to determine the age of a given region using chemistry in combination with radiativetransfer." @default.
- W2567188867 created "2017-01-06" @default.
- W2567188867 creator A5003969718 @default.
- W2567188867 date "2016-12-14" @default.
- W2567188867 modified "2023-09-27" @default.
- W2567188867 title "Modeling chemistry in massive star forming regions with internal PDRs" @default.
- W2567188867 hasPublicationYear "2016" @default.
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