{"id":{"repo_id":"texas-state","oai_identifier":"oai:digital.library.txst.edu:10877/19291"},"canonical_url":"https://search.dev.ndltd.org/etd/texas-state/oai:digital.library.txst.edu:10877/19291","repository":{"repo_id":"texas-state","name":"Texas State University","base_url":"https://digital.library.txst.edu/server/oai/request"},"display":{"title":"The Connection Between X-Ray Binaries and Star Clusters in the Andromeda Galaxy","abstract":"The exploration of X-ray binaries (XRBs) and their relationship with star clusters is an important aspect of astrophysics, offering insights into the processes that govern stellar evolution and the dynamical interactions within star clusters. XRBs are fascinating astronomical systems where a star orbits around a compact object, typically a neutron star or black hole. The intense gravitational pull of the compact object leads to the accretion of material from the companion star, which due to friction heats up so much that it emits high-energy X-ray photons. Previous studies have shown that most stars, including XRBs, form in star clusters. These densely populated regions are the birthplaces of countless stellar objects, playing a critical role in their early evolution. However, several processes, such as close gravitational interactions between stars (dynamical interactions) and the gradual loss of stars due to the cluster's gravitational field weakening (cluster evaporation), lead to stars leaving their birth clusters. This ejection can significantly influence the life cycle and characteristics of XRBs. Understanding these processes is crucial for comprehending the life history of XRBs and the evolutionary trajectory of their parent clusters. The Andromeda Galaxy, the closest spiral to our own (The Milky Way) provides a unique and rich field for investigating these phenomena. Its proximity and similarity to the Milky Way make it an ideal candidate for studying the formation and evolution of XRBs for this project. Studying Andromeda allows us to view the galaxy from a distance whereas in the Milky Way we are on the plane and the extinction due to dust creates and issue in measurements. Furthermore, the availability of detailed observational data from the Panchromatic Hubble Andromeda Treasury (PHAT) and the Chandra X-ray Observatory presents an unprecedented opportunity to delve into these studies with greater precision and depth than ever before. This study employs a systematic approach, focusing on the spatial distribution and properties of XRBs and their associated star clusters in the Andromeda Galaxy.","abstract_html":"The exploration of X-ray binaries (XRBs) and their relationship with star clusters is an important aspect of astrophysics, offering insights into the processes that govern stellar evolution and the dynamical interactions within star clusters. XRBs are fascinating astronomical systems where a star orbits around a compact object, typically a neutron star or black hole. The intense gravitational pull of the compact object leads to the accretion of material from the companion star, which due to friction heats up so much that it emits high-energy X-ray photons. Previous studies have shown that most stars, including XRBs, form in star clusters. These densely populated regions are the birthplaces of countless stellar objects, playing a critical role in their early evolution. However, several processes, such as close gravitational interactions between stars (dynamical interactions) and the gradual loss of stars due to the cluster's gravitational field weakening (cluster evaporation), lead to stars leaving their birth clusters. This ejection can significantly influence the life cycle and characteristics of XRBs. Understanding these processes is crucial for comprehending the life history of XRBs and the evolutionary trajectory of their parent clusters. The Andromeda Galaxy, the closest spiral to our own (The Milky Way) provides a unique and rich field for investigating these phenomena. Its proximity and similarity to the Milky Way make it an ideal candidate for studying the formation and evolution of XRBs for this project. Studying Andromeda allows us to view the galaxy from a distance whereas in the Milky Way we are on the plane and the extinction due to dust creates and issue in measurements. Furthermore, the availability of detailed observational data from the Panchromatic Hubble Andromeda Treasury (PHAT) and the Chandra X-ray Observatory presents an unprecedented opportunity to delve into these studies with greater precision and depth than ever before. This study employs a systematic approach, focusing on the spatial distribution and properties of XRBs and their associated star clusters in the Andromeda Galaxy.","abstract_has_math":false,"creators":["Guerrero, Mauro"],"institution":"Texas State University","degree_name":"Master of Science","degree_level":"Masters","degree_discipline":"Physics","degree_department":null,"school":null,"contributors":[],"advisors":["Rangelov, Blagoy"],"committee_chairs":[],"committee_members":["Mastroleo, Ricardo","Togi, Aditya"],"year":2024,"date_issued":"2024-08","date_published":"2024-08","updated_at":"2026-07-27T21:22:55Z","subjects":["physics","astrophysics","x-ray binaries","star clusters"],"languages":["en"],"rights":[],"rights_urls":[],"identifier_entries":[]},"links":{"outbound_url":"https://hdl.handle.net/10877/19291","outbound_label":"Handle","outbound_source":"dc:identifier.uri"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor.advisor","label":"Advisor","values":["Rangelov, Blagoy"]},{"key":"dc:contributor.committeemember","label":"Committee Member","values":["Mastroleo, Ricardo","Togi, Aditya"]},{"key":"dc:creator","label":"Author","values":["Guerrero, Mauro"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date.accessioned","label":"Dc Date Accessioned","values":["2024-08-12T21:06:12Z"]},{"key":"dc:date.available","label":"Dc Date Available","values":["2024-08-12T21:06:12Z"]},{"key":"dc:date.issued","label":"Date","values":["2024-08"]},{"key":"dc:type","label":"Dc Type","values":["Thesis"]},{"key":"thesis:degree_discipline","label":"Discipline","values":["Physics"]},{"key":"thesis:degree_level","label":"Degree Level","values":["Masters"]},{"key":"thesis:degree_name","label":"Degree Name","values":["Master of Science"]},{"key":"thesis:institution_name","label":"Thesis Institution Name","values":["Texas State University"]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["physics","astrophysics","x-ray binaries","star clusters"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language.iso","label":"Language (ISO)","values":["en"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier.uri","label":"Identifier URI","values":["https://hdl.handle.net/10877/19291"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["The exploration of X-ray binaries (XRBs) and their relationship with star clusters is an important aspect of astrophysics, offering insights into the processes that govern stellar evolution and the dynamical interactions within star clusters. XRBs are fascinating astronomical systems where a star orbits around a compact object, typically a neutron star or black hole. The intense gravitational pull of the compact object leads to the accretion of material from the companion star, which due to friction heats up so much that it emits high-energy X-ray photons. Previous studies have shown that most stars, including XRBs, form in star clusters. These densely populated regions are the birthplaces of countless stellar objects, playing a critical role in their early evolution. However, several processes, such as close gravitational interactions between stars (dynamical interactions) and the gradual loss of stars due to the cluster's gravitational field weakening (cluster evaporation), lead to stars leaving their birth clusters. This ejection can significantly influence the life cycle and characteristics of XRBs. Understanding these processes is crucial for comprehending the life history of XRBs and the evolutionary trajectory of their parent clusters. The Andromeda Galaxy, the closest spiral to our own (The Milky Way) provides a unique and rich field for investigating these phenomena. Its proximity and similarity to the Milky Way make it an ideal candidate for studying the formation and evolution of XRBs for this project. Studying Andromeda allows us to view the galaxy from a distance whereas in the Milky Way we are on the plane and the extinction due to dust creates and issue in measurements. Furthermore, the availability of detailed observational data from the Panchromatic Hubble Andromeda Treasury (PHAT) and the Chandra X-ray Observatory presents an unprecedented opportunity to delve into these studies with greater precision and depth than ever before. This study employs a systematic approach, focusing on the spatial distribution and properties of XRBs and their associated star clusters in the Andromeda Galaxy."]},{"key":"dc:format","label":"Dc Format","values":["Text"]},{"key":"dc:format.medium","label":"Dc Format Medium","values":["1 file (.pdf)"]},{"key":"dc:title","label":"Title","values":["The Connection Between X-Ray Binaries and Star Clusters in the Andromeda Galaxy"]}]}],"canonical_facts":{"dc:contributor.advisor":["Rangelov, Blagoy"],"dc:contributor.committeemember":["Mastroleo, Ricardo","Togi, Aditya"],"dc:creator":["Guerrero, Mauro"],"dc:date.accessioned":["2024-08-12T21:06:12Z"],"dc:date.available":["2024-08-12T21:06:12Z"],"dc:date.issued":["2024-08"],"dc:description.abstract":["The exploration of X-ray binaries (XRBs) and their relationship with star clusters is an important aspect of astrophysics, offering insights into the processes that govern stellar evolution and the dynamical interactions within star clusters. XRBs are fascinating astronomical systems where a star orbits around a compact object, typically a neutron star or black hole. The intense gravitational pull of the compact object leads to the accretion of material from the companion star, which due to friction heats up so much that it emits high-energy X-ray photons. Previous studies have shown that most stars, including XRBs, form in star clusters. These densely populated regions are the birthplaces of countless stellar objects, playing a critical role in their early evolution. However, several processes, such as close gravitational interactions between stars (dynamical interactions) and the gradual loss of stars due to the cluster's gravitational field weakening (cluster evaporation), lead to stars leaving their birth clusters. This ejection can significantly influence the life cycle and characteristics of XRBs. Understanding these processes is crucial for comprehending the life history of XRBs and the evolutionary trajectory of their parent clusters. The Andromeda Galaxy, the closest spiral to our own (The Milky Way) provides a unique and rich field for investigating these phenomena. Its proximity and similarity to the Milky Way make it an ideal candidate for studying the formation and evolution of XRBs for this project. Studying Andromeda allows us to view the galaxy from a distance whereas in the Milky Way we are on the plane and the extinction due to dust creates and issue in measurements. Furthermore, the availability of detailed observational data from the Panchromatic Hubble Andromeda Treasury (PHAT) and the Chandra X-ray Observatory presents an unprecedented opportunity to delve into these studies with greater precision and depth than ever before. This study employs a systematic approach, focusing on the spatial distribution and properties of XRBs and their associated star clusters in the Andromeda Galaxy."],"dc:format":["Text"],"dc:format.medium":["1 file (.pdf)"],"dc:identifier.uri":["https://hdl.handle.net/10877/19291"],"dc:language.iso":["en"],"dc:subject":["physics","astrophysics","x-ray binaries","star clusters"],"dc:title":["The Connection Between X-Ray Binaries and Star Clusters in the Andromeda Galaxy"],"dc:type":["Thesis"],"thesis:degree_discipline":["Physics"],"thesis:degree_level":["Masters"],"thesis:degree_name":["Master of Science"],"thesis:institution_name":["Texas State University"]},"updated_at":"2026-07-27T21:22:55Z"}