On the structure of quasi-Keplerian accretion discs surrounding millisecond X-ray pulsars
dc.contributor.author | Isaac, Habumugisha | |
dc.contributor.author | Solomon, B. Tessema | |
dc.contributor.author | Edward, Jurua | |
dc.contributor.author | Simon, K. Anguma | |
dc.date.accessioned | 2020-11-17T16:39:15Z | |
dc.date.available | 2020-11-17T16:39:15Z | |
dc.date.issued | 2020 | |
dc.description.abstract | In this study, we investigated the time-independent dynamics (disc structure, forces and torques) of a quasi-Keplerian disc around a millisecond pulsar (MSP) with an internal dynamo. We considered the disc around a MSP to be divided into the inner, middle and outer regions. By assuming that the disc matter flows in a quasi-Keplerian motion, we derived analytical equations for a complete structure (temperature, pressure, surface density, optical depth and magnetic field) of a quasi-Keplerian thin accretion disc, and the pressure gradient force (PGF). In our model, the MSP-disc interaction results into magnetic and material torques, such that for a given dynamo ( ) and quasi-Keplerian (n) parameter, we obtained enhanced spin-up and spin-down torques for a chosen star spin period. Results obtained reveal that PGF results into episodic torque reversals that contribute to spinning-up or spinning-down of a neutron star, mainly from the inner region. The possibility of a quasi-Keplerian disc is seen and these results can explain the observed spin variations in MSPs like SAX J1808.4-3658 and XTE J1814-338. | en_US |
dc.description.sponsorship | Kabale University | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12493/463 | |
dc.language.iso | en_US | en_US |
dc.publisher | Indian Academy of Sciences | en_US |
dc.subject | 97.80.Jp X-ray binaries—97.60.Gb pulsars—97.10.Gz accretion and accretion discs | en_US |
dc.title | On the structure of quasi-Keplerian accretion discs surrounding millisecond X-ray pulsars | en_US |
dc.type | Article | en_US |
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