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dc.contributor.advisorJardine, Moira
dc.contributor.authorLehmann, Lisa Theres
dc.coverage.spatialxxix, 185 p.en_US
dc.date.accessioned2020-07-28T15:57:59Z
dc.date.available2020-07-28T15:57:59Z
dc.date.issued2020-07-27
dc.identifier.urihttp://hdl.handle.net/10023/20354
dc.description.abstractGood knowledge about cool star magnetic activity, topology and cycles is crucial to find a second solar system and to better understand ours. The Zeeman-Doppler-Imaging (ZDI) surveys, which unveil the stellar magnetic field topology, have now run for long enough to detect solar-like activity cycles. This is a good point to review what ZDI detects robustly and how to interpret the resulting ZDI maps. As ZDI only detects the large-scale magnetic field an important question to answer is: What can we learn from the large-scale field topology about the small-scale field for solar-like stars? I connect 3D non-potential flux transport simulations based on the Sun with the observational ZDI technique. First, I decomposed the magnetic field topology of the simulations into different length-scales. I discovered that the large-scale field reflects global properties of the small-scale field emergence for slowly-rotating solar-like stars. Second, I used synthetic line profiles modelled from the simulations as input for ZDI. I showed that ZDI can recover the hints of the small-scale flux emergence in the observable large-scale field for slow rotators but recovers approximately one order of magnitude lower magnetic energy. The maximum entropy regularisation used in ZDI prevents the correct reconstruction of the magnetic energy distribution but ZDI can recover the fractions of the different field components reasonably well. To examine if ZDI can recover solar-like cycles, I applied ZDI to non-potential flux transport simulations modelling the solar magnetic field over 15 years. I discovered that the axisymmetric poloidal fraction and the axi- and non-axisymmetric energy are the best parameters to track solar-like activity cycles while the averaged large-scale field or the total energy show no or misleading trends.en_US
dc.description.sponsorship"I acknowledge support from the Scottish Universities Physics Alliance (SUPA) prize studentship and the University of St Andrews Higgs studentship. Further, I received supplementary founding for travelling from SUPA and the European Southern Observatory (ESO) for a 8-weeks short term visit at the ESO Headquarters in 2017 and the ESO for supporting a second visit (1-month) in 2018. Further, I received a travel grant to visit the Cool Stars 20 Conference in Boston to present the work displayed in Chapter 4 from the Royal Astronomical Society (RAS)." -- Fundingen
dc.language.isoenen_US
dc.publisherUniversity of St Andrews
dc.relationConnecting simulations and observations for solar-like stars (thesis data) Lehmann, L.T., University of St Andrews, 2019. DOI: https://doi.org/10.17630/ae078167-03ea-4af6-9055-c3147e13c286en
dc.relation.urihttps://doi.org/10.17630/ae078167-03ea-4af6-9055-c3147e13c286
dc.rightsCreative Commons Attribution-NonCommercial-NoDerivatives 4.0 International*
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/4.0/*
dc.subjectMagnetic fieldsen_US
dc.subjectStarsen_US
dc.subjectSunen_US
dc.subjectZeeman-Doppler-imagingen_US
dc.subjectSpectropolarimetryen_US
dc.subject.lccQB843.C6L4
dc.subject.lcshCool starsen
dc.subject.lcshStars--Magnetic fields--Computer simulationsen
dc.subject.lcshStars--Magnetic fields--Observationsen
dc.subject.lcshSunen
dc.titleCool star magnetic field topologies : connecting simulations and observations for solar-like starsen_US
dc.typeThesisen_US
dc.contributor.sponsorScottish Universities Physics Alliance (SUPA)en_US
dc.contributor.sponsorUniversity of St Andrewsen_US
dc.type.qualificationlevelDoctoralen_US
dc.type.qualificationnamePhD Doctor of Philosophyen_US
dc.publisher.institutionThe University of St Andrewsen_US
dc.rights.embargodate2022-06-02
dc.rights.embargoreasonThesis restricted in accordance with University regulations. Electronic copy of Chapter 5 restricted until 2nd June 2022en


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    Except where otherwise noted within the work, this item's license for re-use is described as Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International