{"id":{"repo_id":"uiuc","oai_identifier":"oai:www.ideals.illinois.edu:2142/23573"},"canonical_url":"https://search.dev.ndltd.org/etd/uiuc/oai:www.ideals.illinois.edu:2142/23573","repository":{"repo_id":"uiuc","name":"University of Illinois - Urbana-Champaign","base_url":"https://www.ideals.illinois.edu/oai-pmh"},"display":{"title":"Rapid mass transfer in binary systems","abstract":"This thesis investigates the conditions for rapid mass transfer in binary stars. Previous theoretical calculations and observations of binaries imply the existence of several different timescales for mass transfer: nuclear, thermal, or dynamical. Since the mass transfer rates differ by several orders of magnitude, it is important to know which timescales are relevant to different systems. Dynamical timescale mass transfer is thought to cause substantial decreases in the orbital period through mass and angular momentum losses. Thermal timescale mass transfer is thought to transform the appearance of the binary as mass exchange occurs in a short time. Binaries currently transferring mass are doing so on the longest, nuclear, timescale.","abstract_html":"This thesis investigates the conditions for rapid mass transfer in binary stars. Previous theoretical calculations and observations of binaries imply the existence of several different timescales for mass transfer: nuclear, thermal, or dynamical. Since the mass transfer rates differ by several orders of magnitude, it is important to know which timescales are relevant to different systems. Dynamical timescale mass transfer is thought to cause substantial decreases in the orbital period through mass and angular momentum losses. Thermal timescale mass transfer is thought to transform the appearance of the binary as mass exchange occurs in a short time. Binaries currently transferring mass are doing so on the longest, nuclear, timescale.","abstract_has_math":false,"creators":["Hjellming, Michael Scott"],"institution":"University of Illinois at Urbana-Champaign","degree_name":"Ph.D.","degree_level":"Dissertation","degree_discipline":"Physics, Astronomy and Astrophysics","degree_department":null,"school":null,"contributors":[],"advisors":[],"committee_chairs":[],"committee_members":[],"year":2011,"date_issued":"2011-05-07T14:19:10Z","date_published":"2011-05-07T14:19:10Z","updated_at":"2026-07-22T22:25:22Z","subjects":["Physics, Astronomy and Astrophysics"],"languages":["eng"],"rights":["Copyright 1989 Hjellming, Michael Scott"],"rights_urls":[],"identifier_entries":[{"key":"dc:identifier","label":"Identifier","values":["AAI9010885","(UMI)AAI9010885"],"render_values":[{"text":"AAI9010885","href":null,"code":true},{"text":"(UMI)AAI9010885","href":null,"code":true}]}]},"links":{"outbound_url":"http://hdl.handle.net/2142/23573","outbound_label":"Handle","outbound_source":"dc:identifier"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:creator","label":"Author","values":["Hjellming, Michael Scott"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date","label":"Dc Date","values":["2011-05-07T14:19:10Z","10000-01-01","1989"]},{"key":"dc:type","label":"Dc Type","values":["text"]},{"key":"thesis:degree_discipline","label":"Discipline","values":["Physics, Astronomy and Astrophysics"]},{"key":"thesis:degree_level","label":"Degree Level","values":["Dissertation"]},{"key":"thesis:degree_name","label":"Degree Name","values":["Ph.D."]},{"key":"thesis:institution_name","label":"Thesis Institution Name","values":["University of Illinois at Urbana-Champaign"]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["Physics, Astronomy and Astrophysics"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language","label":"Dc Language","values":["eng"]},{"key":"dc:rights","label":"Dc Rights","values":["Copyright 1989 Hjellming, Michael Scott"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier","label":"Identifier","values":["AAI9010885","(UMI)AAI9010885","http://hdl.handle.net/2142/23573"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description","label":"Description","values":["This thesis investigates the conditions for rapid mass transfer in binary stars. Previous theoretical calculations and observations of binaries imply the existence of several different timescales for mass transfer: nuclear, thermal, or dynamical. Since the mass transfer rates differ by several orders of magnitude, it is important to know which timescales are relevant to different systems. Dynamical timescale mass transfer is thought to cause substantial decreases in the orbital period through mass and angular momentum losses. Thermal timescale mass transfer is thought to transform the appearance of the binary as mass exchange occurs in a short time. Binaries currently transferring mass are doing so on the longest, nuclear, timescale.","The characteristics of binaries which divide the three timescales are estimated by calculating the response of potential mass donors in two idealized limits: an adiabatic response, where the entropy profile does not change with mass loss, and a thermal response, where thermal relaxation is allowed but nuclear burning is not. A comparison of the changing surface radius, $\\zeta$ = dlnR/dlnM, to the Roche lobe radius implies the critical mass ratios for dynamically and thermally unstable mass transfer. These calculations are performed here for donors between 0.25 and 20 M$\\sb\\odot$ which would fill their Roche lobes before helium burning.","The adiabatic mass-loss calculations have provided a clear relation between $\\zeta\\sb{\\rm ad}$ and the donor's convective envelope mass fraction (f$\\sb{\\rm ce}$), with a smaller dependence on the state of the interior. Low-mass ZAMS donors and models near the base of the giant branch have $\\zeta\\sb{\\rm ad} \\gg 1$ change to $\\zeta\\sb{\\rm ad} \\sim 0$ between $0.05 $ 1.5 M$\\sb\\odot$, much larger changes occur: $\\zeta\\sb{\\rm th} = 0.60$, for the ZAMS models, to $\\zeta\\sb{\\rm th} \\ll -1$, for models within the Hertzsprung gap. At the base of the giant branch, $\\zeta\\sb{\\rm th}$ increases back to $-$0.2. The current distributions of cataclysmic variables and Algol binaries are discussed in consideration of these results.","Made available in DSpace on 2011-05-07T14:19:10Z (GMT). No. of bitstreams: 2 license.txt: 4922 bytes, checksum: 910b249b4beec47e7ab768910c8f966f (MD5) 9010885.pdf: 6228844 bytes, checksum: 05b78d72b01e32e6a898df500f59a2b2 (MD5) Previous issue date: 1989","Item marked as restricted to the 'UIUC Users [automated]' Group (id=2) by Howard Ding (hding2@illinois.edu) on 2011-05-07T15:05:23Z Item is restricted indefinitely.","Restriction data tranferred 2014-07-01T11:31:19-05:00 Original Data Group with Access UIUC Users [automated] Release Date: none Reason: ETDs are only available to UIUC Users without author permission","ETDs are only available to UIUC Users without author permission","U of I Only"]},{"key":"dc:title","label":"Title","values":["Rapid mass transfer in binary systems"]}]}],"canonical_facts":{"dc:creator":["Hjellming, Michael Scott"],"dc:date":["2011-05-07T14:19:10Z","10000-01-01","1989"],"dc:description":["This thesis investigates the conditions for rapid mass transfer in binary stars. Previous theoretical calculations and observations of binaries imply the existence of several different timescales for mass transfer: nuclear, thermal, or dynamical. Since the mass transfer rates differ by several orders of magnitude, it is important to know which timescales are relevant to different systems. Dynamical timescale mass transfer is thought to cause substantial decreases in the orbital period through mass and angular momentum losses. Thermal timescale mass transfer is thought to transform the appearance of the binary as mass exchange occurs in a short time. Binaries currently transferring mass are doing so on the longest, nuclear, timescale.","The characteristics of binaries which divide the three timescales are estimated by calculating the response of potential mass donors in two idealized limits: an adiabatic response, where the entropy profile does not change with mass loss, and a thermal response, where thermal relaxation is allowed but nuclear burning is not. A comparison of the changing surface radius, $\\zeta$ = dlnR/dlnM, to the Roche lobe radius implies the critical mass ratios for dynamically and thermally unstable mass transfer. These calculations are performed here for donors between 0.25 and 20 M$\\sb\\odot$ which would fill their Roche lobes before helium burning.","The adiabatic mass-loss calculations have provided a clear relation between $\\zeta\\sb{\\rm ad}$ and the donor's convective envelope mass fraction (f$\\sb{\\rm ce}$), with a smaller dependence on the state of the interior. Low-mass ZAMS donors and models near the base of the giant branch have $\\zeta\\sb{\\rm ad} \\gg 1$ change to $\\zeta\\sb{\\rm ad} \\sim 0$ between $0.05 $ 1.5 M$\\sb\\odot$, much larger changes occur: $\\zeta\\sb{\\rm th} = 0.60$, for the ZAMS models, to $\\zeta\\sb{\\rm th} \\ll -1$, for models within the Hertzsprung gap. At the base of the giant branch, $\\zeta\\sb{\\rm th}$ increases back to $-$0.2. The current distributions of cataclysmic variables and Algol binaries are discussed in consideration of these results.","Made available in DSpace on 2011-05-07T14:19:10Z (GMT). No. of bitstreams: 2 license.txt: 4922 bytes, checksum: 910b249b4beec47e7ab768910c8f966f (MD5) 9010885.pdf: 6228844 bytes, checksum: 05b78d72b01e32e6a898df500f59a2b2 (MD5) Previous issue date: 1989","Item marked as restricted to the 'UIUC Users [automated]' Group (id=2) by Howard Ding (hding2@illinois.edu) on 2011-05-07T15:05:23Z Item is restricted indefinitely.","Restriction data tranferred 2014-07-01T11:31:19-05:00 Original Data Group with Access UIUC Users [automated] Release Date: none Reason: ETDs are only available to UIUC Users without author permission","ETDs are only available to UIUC Users without author permission","U of I Only"],"dc:identifier":["AAI9010885","(UMI)AAI9010885","http://hdl.handle.net/2142/23573"],"dc:language":["eng"],"dc:rights":["Copyright 1989 Hjellming, Michael Scott"],"dc:subject":["Physics, Astronomy and Astrophysics"],"dc:title":["Rapid mass transfer in binary systems"],"dc:type":["text"],"thesis:degree_discipline":["Physics, Astronomy and Astrophysics"],"thesis:degree_level":["Dissertation"],"thesis:degree_name":["Ph.D."],"thesis:institution_name":["University of Illinois at Urbana-Champaign"]},"updated_at":"2026-07-22T22:25:22Z"}