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dc.contributor.advisorRay, Subharthi.
dc.creatorNdebele, Sakhile Mpilo.
dc.date.accessioned2018-10-15T12:26:19Z
dc.date.available2018-10-15T12:26:19Z
dc.date.created2017
dc.date.issued2017
dc.identifier.urihttp://hdl.handle.net/10413/15646
dc.descriptionMaster of Science in Applied Mathematics, University of KwaZulu-Natal, Westville, 2017.en_US
dc.description.abstractIn previous studies, people have shown that compact stars, like the neutron stars and quark stars, can hold a lot of charge during their formation resulting in a large mass and radius. It was also argued that when the charges leave the system due to repulsion from the self created field, these might render a secondary collapse to a charged black hole. In the present work, we have taken a particular type of charge distribution, with varying parameters, such that changing these parameters mimic the situation when the charge particles leaving the system. We have made a systematic study of each stage of the charge distributions. Our results reveal that when the charge distribution deviates slightly from the scenario where the charge density is proportional to the mass density, then the system is no longer able to retain the large mass and radius, and quickly attains a lower mass and radius.en_US
dc.language.isoen_ZAen_US
dc.subject.otherNeutron stars.en_US
dc.subject.otherGeneral relativity.en_US
dc.subject.otherEquations.en_US
dc.subject.otherStars.en_US
dc.subject.otherMatter.en_US
dc.titleCharge distribution in neutron stars.en_US
dc.typeThesisen_US


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