Chemistry in externally FUV illuminated protoplanetary disks in the Orion Nebula Cluster
| dc.contributor.advisor | Guzmán Veloso, Viviana | |
| dc.contributor.author | Díaz Berríos, Javiera Katalina | |
| dc.contributor.other | Pontificia Universidad Católica de Chile. Facultad de Física | |
| dc.date.accessioned | 2022-11-18T15:11:51Z | |
| dc.date.available | 2022-11-18T15:11:51Z | |
| dc.date.issued | 2022 | |
| dc.date.updated | 2022-11-18T10:09:20Z | |
| dc.description | Tesis (Master in Astrophysics)--Pontificia Universidad Católica de Chile, 2022 | |
| dc.description.abstract | Understanding the chemical composition and distribution of the birthplaces of planets (protoplanetary disks) is key to constraining the initial conditions of planet formation and planetary atmospheres. Most protoplanetary disks are born in stellar clusters and can therefore be affected by the radiation of nearby massive stars. However, little is known about the potential differences or similarities in the chemistry of isolated versus externally irradiated disks. Motivated by this question, we present ALMA Band 6 observations of two protoplanetary disks in the outskirts of the Orion Nebula Cluster (ONC) to explore the chemical composition of disks exposed to (external) FUV radiation fields: the large 216–0939 disk and the binary system 253–1536A/B. We successfully detect lines from CO isotopologues, HCN, H2CO, and C2H toward both protoplanetary disks. Undetected molecular lines include DCN and C3H2. Based on the observed disk–integrated line fluxes and flux, we do not find significant differences between isolated and irradiated disks. This suggests that these sources are far enough from the ONC so that their chemistry is not affected by the external radiation field or that we are observing the region from the disk that survives the external radiation; Indeed, these disks are massive and could, therefore self–shield from the radiation field. However, we expect CN emission to be brighter in irradiated disks than in isolated ones, which can be tested with future ALMA observations. We also expect stronger differences for disks that are closer to the ONC. | |
| dc.format.extent | 74 páginas | |
| dc.fuente.origen | Autoarchivo | |
| dc.identifier.doi | 10.7764/tesisUC/FIS/65600 | |
| dc.identifier.uri | https://doi.org/10.7764/tesisUC/FIS/65600 | |
| dc.identifier.uri | https://repositorio.uc.cl/handle/11534/65600 | |
| dc.information.autoruc | Facultad de física ; Guzmán Veloso, Viviana ; 0000-0003-4784-3040 ; 1083356 | |
| dc.information.autoruc | Facultad de física ; Díaz Berríos, Javiera Katalina ; S/I ; 232205 | |
| dc.language.iso | en | |
| dc.nota.acceso | Contenido completo | |
| dc.rights | acceso abierto | |
| dc.subject.ddc | 520 | |
| dc.subject.dewey | Astronomía | es_ES |
| dc.title | Chemistry in externally FUV illuminated protoplanetary disks in the Orion Nebula Cluster | es_ES |
| dc.type | tesis de maestría | |
| sipa.codpersvinculados | 1083356 | |
| sipa.codpersvinculados | 232205 |