Characterization of molecular gas substructures in the protoplanetary disk HD 163296 using ALMA interferometric data

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dc.catalogadorpva
dc.contributor.advisorGuzmán Veloso, Viviana
dc.contributor.authorMaluenda Berna, Michel Yan Luis
dc.contributor.otherPontificia Universidad Católica de Chile. Instituto de Astrofísica
dc.date.accessioned2024-01-31T13:12:57Z
dc.date.available2024-01-31T13:12:57Z
dc.date.issued2024
dc.date.updated2024-01-26T19:24:49Z
dc.descriptionTesis (Master of Science in Astrophysics)--Pontificia Universidad Católica de Chile, 2024
dc.description.abstractThis thesis conducts an extensive examination of molecular gas substructures, specifically HCN and C2H, within the protoplanetary disk surrounding HD 163296. Utilizing ALMA interferometric data in two rotational transitions, the study resolves structures down to 10 au scales, focusing on characterizing gas substructures and comparing them with millimeter dust in the disk. The methodology involves parameterizing relative abundance, incorporating Gaussian functions, and employing MCMC analysis to model observed bright ring substructures. The study reveals three bright line emission rings for both HCN and C2H, indicating a high abundance within 150 au of the central star. Interestingly, no universal connection is found between dust and molecular substructures, suggesting complex dynamics. The inner disk (<150 au) exhibits a peak relative abundance of ∼6.8 × 10−11 for HCN and ∼5.0 × 10−11 for C2H, implying active organic chemistry or hidden molecular emissions. Furthermore, a significant overlap between dust and chemical substructures within 150 au is observed, diminishing in the outer disk. The outermost bright rings at approximately 309 and 385 au for HCN and C2H respectively lack correlation with CO substructures, challenging conventional understanding of protoplanetary disk composition and dynamics. Chemical conversion of CO into other species is proposed as a partial explanation for observed vertical substructures and high C/O ratios influencing C2H and HCN abundance. This research enhances our understanding of complex dynamics and chemical processes in protoplanetary disks, providing valuable insights for future planet formation studies.
dc.fechaingreso.objetodigital2024-01-26
dc.format.extent91 páginas
dc.fuente.origenAutoarchivo
dc.identifier.doi10.7764/tesisUC/AST/81108
dc.identifier.urihttps://do.org/10.7764/tesisUC/AST/81108
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/81108
dc.information.autorucInstituto de Astrofísica; Guzmán Veloso, Viviana; 0000-0003-4784-3040; 1083356
dc.information.autorucInstituto de Astrofísica; Maluenda Berna, Michel Yan Luis; S/I; 1092424
dc.language.isoen
dc.nota.accesoContenido completo
dc.rightsacceso abierto
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.titleCharacterization of molecular gas substructures in the protoplanetary disk HD 163296 using ALMA interferometric dataes_ES
dc.typetesis de maestría
sipa.codpersvinculados1083356
sipa.codpersvinculados1092424
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