cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.21954/ou.rd.27458367
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" -<b>4/4: warped disc movies</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.21954/ou.rd.27458367.v1
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" -<b>4/4: warped disc movies</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.17037/data.00004413
title: Data for: "Understanding end-user preferences for hand hygiene enabling technologies: a mixed-methods study in peri-urban Lusaka"

description: This dataset contains information collected as part of the quantitative component of a mixed-methods study to investigate end-user preferences for hand hygiene enabling technologies in peri-urban Lusaka, Zambia. Data was collected from 81 individuals who participated in focus group discussions (FGD) held in two communities during Jan-Feb 2024. 

The dataset is comprised of 11 tables, the name of which indicates the topic of assessment. Variables include the handwashing facility or attribute being ranked, the grade assigned, and participant information. Participant information covers ID value, participant group, FGD location, and whether they participated in phase 1 (qualitative component).
description: In focus group discussions, participants were firstly asked to individually rank eight handwashing facilities from best to worst against eight attributes: appearance, convenience, ease of use, hygienic use, maintenance, vulnerability, water disposal, water management. Ties were permitted. Participants were then asked to rank each HWF by their overall preference from most to lease desirable. Estimated retail prices (based on cost price from manufacturer or distributor as well as shipping for HWFS manufactured outside Zambia) were then shared and participants were asked to again rank by overall preference. Finally, participants were asked to rank each of the attributes from most to least important.
DOI: 10.21954/ou.rd.27376764
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" -<b>3/4: sph view 3d</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.21954/ou.rd.27376764.v1
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" -<b>3/4: sph view 3d</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.6084/m9.figshare.26779969
title: CAS-Canglong model and data

description: SST model with data
DOI: 10.6084/m9.figshare.26779969.v1
title: CAS-Canglong SST data

description: SST prediction
DOI: 10.21954/ou.rd.27376290
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" -<b> 2/4: 3d movies</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.21954/ou.rd.27376290.v1
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" -<b> 2/4: 3d movies</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.21954/ou.rd.27374499
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" - <b>1/4: </b><b>2d movies</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.21954/ou.rd.27374499.v1
title: Supplementary material for PhD thesis "SPH simulations of X-ray binary systems" - <b>1/4: </b><b>2d movies</b>

description: <i>This dataset</i><i> </i><i>comprises</i><i> </i><i>the files contained on a CD-ROM which was attached to the thesis when it was</i><i> </i><i>submitted</i><i> </i><i>in</i><i> </i><i>2006</i><i>. It was uploaded to ORDO in 2024 for preservation purposes.</i><i> </i><i>For more information, please refer to the thes</i><i>is </i><i>SPH simulations of X-ray binary systems </i><i>via ORO.</i>Thesis abstractIn low mass X-ray binaries a neutron star or a black hole accretes from a low mass companion star via an accretion disc. The physics of accretion discs in these systems is currently an area of vigorous international research activity. In particular the advent of supercomputing has allowed quantitative numerical work on the dynamics of such systems. The numerical simulations are becoming increasingly able to reproduce observed phenomena, and the interplay between simulation and observation is refining the picture derived from analytical work on these systems. Consequently this PhD exploits the synergy between observation and simulation. We present two/three-dimensional smoothed particle hydrodynamics (SPH) simulations of a number of binary systems, such as XTE J1118+480, and reveal complex accretion discs that are continuously varying in shape, kinematics and dissipation. The stream-disc impact region and disc spiral density waves are prominent sources of energy dissipation. For extreme mass ratios the dissipated energy is modulated on the superhump period. We generate synthetic trailed spectrograms that reveal two distinct `S-wave' features, produced by the stream gas and the disc gas at the stream-disc impact shock. These S-waves are non-sinusoidal, and evolve with disc precession phase. We also describe three-dimensional SPH calculations of warped accretion discs in X-ray binary systems. Geometrically thin, optically thick accretion discs are illuminated by a central radiation source. This illumination exerts a non-axisymmetric radiation pressure on the surface of the disc resulting in a torque that acts on the disc to induce a twist or warp. Initially planar discs are shown to be unstable to warping driven by the radiation torque and in general the warps also precess in a retrograde direction relative to the orbital flow. We simulate a number of X-ray binary systems which have different mass ratios using a number of different luminosities for each. Models for X-ray binary systems such as Her X-1 and SS 433 are able to reproduce their observed long period photometric modulations.
DOI: 10.15468/dl.sbu33e
title: Occurrence Download

description: A dataset containing 1766 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Cymbopogon caesius (Hook. & Arn.) Stapf",
 "Continent is Africa"
 ]
}

 The dataset includes 1766 records from 62 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0017607-241024112534372/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.15468/dl.3ukuv8
title: Occurrence Download

description: A dataset containing 1073893 species occurrences available in GBIF matching the query:
{
 "DatasetKey" : [
 "is ArtenFinder"
 ]
}

 The dataset includes 1073893 records from 1 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0017597-241024112534372/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.