Star Formation: Modelling the Collapse of a Dense Core

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dc.contributor.authorFranklin, Daniel
dc.date.accessioned2021-10-22T15:52:53Z
dc.date.available2021-10-22T15:52:53Z
dc.date.created2021
dc.description2021 Celebration of Student Research and Creativity presentationen_US
dc.description.abstract"Stars begin their life in molecular clouds: areas of dense gas in the interstellar medium that are threaded by magnetic fields. Within these molecular clouds, the gas is distributed unevenly resulting in denser regions known as cores. Star formation is thought to begin when a core loses support from its magnetic field and material from the core begins to “fall in” making the core even denser. Once this over dense region of gas has formed, collapse is inevitable and a young star is formed. Using a classic partial differential equation model of this process as a starting point, we explore how the relationship between a core’s pressure and density influences the timeline of the core’s collapse."en_US
dc.description.urihttps://youtu.be/43jhkegjStAen_US
dc.identifier.urihttp://hdl.handle.net/11216/4027
dc.language.isoen_USen_US
dc.publisherNorthern Kentucky Universityen_US
dc.relation.ispartofseriesCelebration of Student Research and Creativity;2021
dc.subjectStars Formationen_US
dc.subjectStars Densityen_US
dc.subjectStars Magnetic fieldsen_US
dc.titleStar Formation: Modelling the Collapse of a Dense Coreen_US
dc.typePresentationen_US

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Student Research and Creativity