{"id":{"repo_id":"york","oai_identifier":"oai:yorkspace.library.yorku.ca:10315/41892"},"canonical_url":"https://search.dev.ndltd.org/etd/york/oai:yorkspace.library.yorku.ca:10315/41892","repository":{"repo_id":"york","name":"York University","base_url":"https://yorkspace.library.yorku.ca/oai/request"},"display":{"title":"Structure and Local Properties of Dark Matter Halos","abstract":"The structure and local properties of dark matter (DM) are important input variables for both direct and indirect detection experiments. Common assumptions about DM, such as, its particle nature being cold and collisionless–CDM–and its distribution in halos being isothermal and spherical, and well-modeled by an isotopic Maxwell-Boltzmann velocity distribution–the Standard Halo Model (SHM)–prove to be at odds with astrophysical observations. In this thesis I present work towards elucidating two areas of refinement to the above-mentioned assumptions regarding DM: 1) allowing moderate self-interactions between DM particles (SIDM), extending the semi-analytic Jeans modeling technique for SIDM halos to multiple dimensions and including baryons and nonspherical effects to study the resulting change in the DM halo structure; 2) quantifying the departure from the SHM by analyzing hydrodynamical simulations of Milky Way (MW) like halos to characterize the impact on local properties of DM induced by satellite galaxies like the Large Magellanic Cloud (LMC) and their implications for direct detection experiments.","abstract_html":"The structure and local properties of dark matter (DM) are important input variables for both direct and indirect detection experiments. Common assumptions about DM, such as, its particle nature being cold and collisionless–CDM–and its distribution in halos being isothermal and spherical, and well-modeled by an isotopic Maxwell-Boltzmann velocity distribution–the Standard Halo Model (SHM)–prove to be at odds with astrophysical observations. In this thesis I present work towards elucidating two areas of refinement to the above-mentioned assumptions regarding DM: 1) allowing moderate self-interactions between DM particles (SIDM), extending the semi-analytic Jeans modeling technique for SIDM halos to multiple dimensions and including baryons and nonspherical effects to study the resulting change in the DM halo structure; 2) quantifying the departure from the SHM by analyzing hydrodynamical simulations of Milky Way (MW) like halos to characterize the impact on local properties of DM induced by satellite galaxies like the Large Magellanic Cloud (LMC) and their implications for direct detection experiments.","abstract_has_math":false,"creators":["Smith-Orlik, Adam Jacob Ross"],"institution":null,"degree_name":null,"degree_level":null,"degree_discipline":null,"degree_department":null,"school":null,"contributors":[],"advisors":["Tulin, Sean","Bozorgnia, Nassim"],"committee_chairs":[],"committee_members":[],"year":2024,"date_issued":"2024-03-16","date_published":"2024-03-16","updated_at":"2026-07-24T06:33:40Z","subjects":["Astrophysics"],"languages":["en"],"rights":["Author owns copyright, except where explicitly noted. Please contact the author directly with licensing requests."],"rights_urls":[],"identifier_entries":[]},"links":{"outbound_url":"https://hdl.handle.net/10315/41892","outbound_label":"Handle","outbound_source":"dc:identifier.uri"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor.advisor","label":"Advisor","values":["Tulin, Sean","Bozorgnia, Nassim"]},{"key":"dc:creator","label":"Author","values":["Smith-Orlik, Adam Jacob Ross"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date.accessioned","label":"Dc Date Accessioned","values":["2024-03-18T18:01:22Z"]},{"key":"dc:date.available","label":"Dc Date Available","values":["2024-03-18T18:01:22Z"]},{"key":"dc:date.issued","label":"Date","values":["2024-03-16"]},{"key":"dc:type","label":"Dc Type","values":["Electronic Thesis or Dissertation"]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["Astrophysics"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language","label":"Dc Language","values":["en"]},{"key":"dc:rights","label":"Dc Rights","values":["Author owns copyright, except where explicitly noted. Please contact the author directly with licensing requests."]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier.uri","label":"Identifier URI","values":["https://hdl.handle.net/10315/41892"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["The structure and local properties of dark matter (DM) are important input variables for both direct and indirect detection experiments. Common assumptions about DM, such as, its particle nature being cold and collisionless–CDM–and its distribution in halos being isothermal and spherical, and well-modeled by an isotopic Maxwell-Boltzmann velocity distribution–the Standard Halo Model (SHM)–prove to be at odds with astrophysical observations. In this thesis I present work towards elucidating two areas of refinement to the above-mentioned assumptions regarding DM: 1) allowing moderate self-interactions between DM particles (SIDM), extending the semi-analytic Jeans modeling technique for SIDM halos to multiple dimensions and including baryons and nonspherical effects to study the resulting change in the DM halo structure; 2) quantifying the departure from the SHM by analyzing hydrodynamical simulations of Milky Way (MW) like halos to characterize the impact on local properties of DM induced by satellite galaxies like the Large Magellanic Cloud (LMC) and their implications for direct detection experiments."]},{"key":"dc:title","label":"Title","values":["Structure and Local Properties of Dark Matter Halos"]}]}],"canonical_facts":{"dc:contributor.advisor":["Tulin, Sean","Bozorgnia, Nassim"],"dc:creator":["Smith-Orlik, Adam Jacob Ross"],"dc:date.accessioned":["2024-03-18T18:01:22Z"],"dc:date.available":["2024-03-18T18:01:22Z"],"dc:date.issued":["2024-03-16"],"dc:description.abstract":["The structure and local properties of dark matter (DM) are important input variables for both direct and indirect detection experiments. Common assumptions about DM, such as, its particle nature being cold and collisionless–CDM–and its distribution in halos being isothermal and spherical, and well-modeled by an isotopic Maxwell-Boltzmann velocity distribution–the Standard Halo Model (SHM)–prove to be at odds with astrophysical observations. In this thesis I present work towards elucidating two areas of refinement to the above-mentioned assumptions regarding DM: 1) allowing moderate self-interactions between DM particles (SIDM), extending the semi-analytic Jeans modeling technique for SIDM halos to multiple dimensions and including baryons and nonspherical effects to study the resulting change in the DM halo structure; 2) quantifying the departure from the SHM by analyzing hydrodynamical simulations of Milky Way (MW) like halos to characterize the impact on local properties of DM induced by satellite galaxies like the Large Magellanic Cloud (LMC) and their implications for direct detection experiments."],"dc:identifier.uri":["https://hdl.handle.net/10315/41892"],"dc:language":["en"],"dc:rights":["Author owns copyright, except where explicitly noted. Please contact the author directly with licensing requests."],"dc:subject":["Astrophysics"],"dc:title":["Structure and Local Properties of Dark Matter Halos"],"dc:type":["Electronic Thesis or Dissertation"]},"updated_at":"2026-07-24T06:33:40Z"}