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THE LARGE-SCALE MAGNETIC FIELDS of PLANET-HOSTING SOLAR-TYPE STARS a Thesis Submitted by Matthew W. Mengel, M.Phil., G.D.Inf.Tec

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THE LARGE-SCALE MAGNETIC FIELDS OF PLANET-HOSTING SOLAR-TYPE STARS A Thesis Submitted by Matthew W. Mengel, M.Phil., G.D.Inf.Tech, B.Inf.Tech. For the Award of Doctor of Philosophy 2017 Abstract Stellar magnetic fields and their associated phenomena influence stellar be- haviour and evolution, and potentially have significant impacts on any surrounding planetary system. However, the nature of star-planet interactions is unclear, especially the potential impact on a star of a closely orbiting massive planet with a powerful mag- netic field. This thesis presents a spectropolarimetric survey of the large-scale magnetic fields of planet-hosting solar-type stars. While little evidence is found for a systematic dif- ference in the magnetic field characteristics of planet-hosting stars compared with the population of solar-type stars, a small positive correlation is indicated between the magnitude of the tidal effects of the planet on the star and the magnetic field strength. Nevertheless, further spectropolarimetric observations of hot Jupiter hosting systems are required to confirm this tentative relationship. For the particular case of a moderately active star with a thin convective zone and a closely orbiting hot Jupiter (τ Boötis) presented here, a remarkably rapid magnetic cycle with a period of ∼ 240 d is discovered. For stars with shallow convective en- velopes, this is an unusual occurrence and suggests a possible role for planetary tidal or magnetic interaction with the star’s convective zone and magnetic dynamo. More observations are required to verify this possible star-planet interaction and to extend the work to other similar systems as they come to light from exoplanet surveys. i Certification of Thesis This Thesis is the work of Matthew W. Mengel except where otherwise ac- knowledged, with the majority of the authorship of the papers presented as a Thesis by Publication undertaken by the Student. The work is original and has not previously been submitted for any other award, except where ac- knowledged. Student and supervisors signatures of endorsement are held at USQ. Associate Professor Stephen C. Marsden Principal Supervisor Professor Bradley D. Carter Associate Supervisor Doctor Rim Fares Associate Supervisor ii List of Contributions from Publication Co-authors This section details contributions by the various authors for each of the papers pre- sented in this thesis by publication. Chapter 2, Mengel et al. (2017b): Mengel, M. W., Marsden, S. C., Carter, B. D., Horner, J., King, R., Fares, R., Jeffers, S. V., Petit, P., Vidotto, A. A., & Morin, J. (2017b). A BCool survey of the magnetic fields of planet-hosting solar-type stars. MNRAS, 465(3), 2734–2747 Author Percent Tasks Performed Contribution M. W. Mengel 85 Performed target selection, analysis, interpretation, wrote all drafts of paper, conception of project. 9 S. C. Marsden > > B. D. Carter > > R. Fares > > Conception of BCool project, steering committee of J. Horner >=> BCool collaboration long term observing project, sug- R. King 15 > gested edits to manuscript, conception of project, con- P. Petit > > fidence intervals in statistical analysis S. V. Jeffers > > A. A. Vidotto > > J. Morin ; iii Chapter 3, Mengel et al. (2016): Mengel, M. W., Fares, R., Marsden, S. C., Carter, B. D., Jeffers, S. V., Petit, P., Do- nati, J.-F., & Folsom, C. P. (2016). The evolving magnetic topology of τ Boötis. MN- RAS, 459(4), 4325–4342 Author Percent Tasks Performed Contribution M. W. Mengel 80 Performed analysis, interpretation, wrote all drafts of paper. 9 R. Fares > > S. C. Marsden > > Conception of BCool project, steering committee of B. D. Carter >=> BCool collaboration long term observing project, sug- S. V. Jeffers 20 > gested edits to manuscript, conception of project, pro- P. Petit > > vided access to code J.-F. Donati > > C. Folsom ; Chapter 4, Mengel et al. (2017a): Mengel, M. W., Jeffers, S. V., Moutou, C., Marsden, S. C., Fares, R., & Carter, B. D. (2017a). A rapid magnetic cycle on τ Boötis. in preparation Author Percent Tasks Performed Contribution M. W. Mengel 85 Conception of project, performed analysis, interpreta- tion, wrote all drafts of paper. 9 S. V. Jeffers > > C. Moutou >=> Conception of project, data acquisition, interpretation, S. C. Marsden 15 > suggested edits to manuscript R. Fares > > B. D. Carter ; iv The following papers to which co-author contributions were made by M. W. Mengel during the period of Candidacy, but not germane to the main thesis and narrative are presented in Appendices A-C. Nicholson, B. A., Vidotto, A. A., Mengel, M., Brookshaw, L., Carter, B., Petit, P., Marsden, S. C., Jeffers, S. V., & Fares, R. (2016). Temporal variability of the wind from the star τ Boötis. MNRAS, 459(2), 1907–1915 Wittenmyer, R. A., Johnson, J. A., Butler, R. P., Horner, J., Wang, L., Robertson, P., Jones, M. I., Jenkins, J. S., Brahm, R., Tinney, C. G., Mengel, M. W.,& Clark, J. (2016). The Pan-Pacific Planet Search. IV.Two Super-Jupiters in a 3:5 Resonance Orbiting the Giant Star HD 33844. Ap. J., 818, 35 Wittenmyer, R. A., Horner, J., Mengel, M. W., Butler, R. P., Wright, D. J., Tinney, C. G., Carter, B. D., Jones, H. R. A., Anglada-Escudé, G., Bailey, J., & O’Toole, S. J. (2017). The Anglo-Australian Planet Search. XXV. A Candidate Massive Saturn Ana- log Orbiting HD 30177. A. J., 153, 167 v Acknowledgments I would like to offer my sincere thanks and acknowledgements to many people and organizations for allowing me to complete this thesis. Firstly, I would like to acknowledge the Australian Department of Educa- tion for the financial support provided via the Australian Postgraduate Awards scheme. Additional funding was made available by the University of South- ern Queensland via a Strategic Research Fund provided to the Astrophysics Group for the STARWINDS project. This research was also supported by an Australian Government Research Training Program (RTP) Scholarship. Data for the project was provided by the BCool Collaboration, Dr. Rim Fares, Dr. Sandra Jeffers, and Dr. Claire Moutou. This data was collected us- ing the HARPS South instrument at the European Southern Observatory, La Silla, Chile; the NARVAL instrument located at the Teléscope Bernard Lyot (TBL) at the Observatoire Midi-Pyrenees, France; and the ESPaDOnS instru- ment at the Canada-France-Hawaii Telescope (CFHT) located at the Mauna Kea Observatory in Hawaii. TBL/NARVAL are operated by the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France. CFHT/ESPaDOnS is operated by the National Re- search Council of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the Univer- vi sity of Hawaii. Thanks to the co-authors and colleagues on my papers who provided com- ments, feedback, access to computer code: Dr. Jonathan Horner, Dr. Rachel King, Dr. Carolyn Brown, Dr. Ian Waite, Dr. Sandra Jeffers, Dr. Pascal Pe- tit, Dr. Aline Vidotto, Dr. Julien Morin, Dr. Jean-Francois Donati and Dr. Colin Folsom. Additional thanks to fellow students Belinda Nicholson, Dr. Victor See and Jack Soutter for their comments and assistance. Special thanks, of course to my team of supervisors, mentors and co-authors - Associate Professor Stephen Marsden, Professor Brad Carter and Dr. Rim Fares. I could not have completed this journey without their guidance and support. Finally, my enduring thanks to my family and friends in supporting me throughout my study. I left a career of twenty years to pursue this work, and everyone has been nothing but supportive. Thank you all for making this possible. vii Contents Abstract i Certification of Thesis ii List of Contributions from Publication Co-authors iii Acknowledgments vi Table of Contents viii List of Figures xii List of Tables xiv 1 Introduction 1 1.1 The Solar Magnetic Field . 3 1.1.1 The Solar Dynamo . 5 1.1.1.1 Differential Rotation: the ω Effect . 7 1.1.1.2 Convection and Coriolis: the α Effect . 7 1.1.2 Solar Cycles . 8 1.2 Stellar Magnetic Fields . 10 viii 1.3 Detecting and Modelling Stellar Magnetic Fields . 11 1.3.1 Detecting Magnetic Fields . 11 1.3.2 Observational Procedure for Generating Stokes Param- eters . 15 1.3.3 Zeeman Doppler Imaging . 16 1.3.3.1 Radiative Transfer in the Presence of a Mag- netic Field . 21 1.3.3.2 Limitations of ZDI . 25 1.3.4 Differential Rotation . 26 1.4 Stellar Magnetic Fields and Exoplanets . 27 1.5 Longitudinal Magnetic Field . 29 1.6 Chromospheric Activity Cycles . 30 1.7 The Magnetic Fields of Solar-Type Stars . 31 1.7.1 Magnetic Cycles . 32 1.7.2 Star-Planet Interaction . 33 1.8 Research Questions . 35 1.8.1 To what extent does the presence of a planetary sys- tem systematically affect the large-scale magnetic fields of their host solar-type stars, if at all? . 35 1.8.2 How does the presence of the hot Jupiter τ Boötis b affect the large-scale magnetic field of the host star in the particular case of τ Boötis? . 36 2 A BCool Survey of the Magnetic Fields of Planet Hosting Stars 37 2.1 Mengel et al. (2017b) “A BCool Survey of the magnetic fields of planet-hosting solar-type stars” . 38 2.2 Summary of Results . 53 ix 3 The Evolving Magnetic Field of the Planet-Hosting Solar-Type Star τ Boö tis 54 3.1 Mengel et al. (2016) “The evolving magnetic topology of τ Boötis” . 55 3.2 Summary of Results . 74 4 A Rapid Large-Scale Magnetic Cycle on τ Boö tis 75 4.1 Mengel et al. (2017a) “A rapid large-scale magnetic cycle on τ Boötis” . 76 4.2 Observations of τ Boötis January and February 2017 .
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    A&A 615, A175 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832711 & c ESO 2018 Astrophysics Exploring the realm of scaled solar system analogues with HARPS?;?? D. Barbato1,2, A. Sozzetti2, S. Desidera3, M. Damasso2, A. S. Bonomo2, P. Giacobbe2, L. S. Colombo4, C. Lazzoni4,3 , R. Claudi3, R. Gratton3, G. LoCurto5, F. Marzari4, and C. Mordasini6 1 Dipartimento di Fisica, Università degli Studi di Torino, via Pietro Giuria 1, 10125, Torino, Italy e-mail: [email protected] 2 INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025, Pino Torinese, Italy 3 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122, Padova, Italy 4 Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova, Vicolo dell’Osservatorio 3, 35122, Padova, Italy 5 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile 6 Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland Received 8 February 2018 / Accepted 21 April 2018 ABSTRACT Context. The assessment of the frequency of planetary systems reproducing the solar system’s architecture is still an open problem in exoplanetary science. Detailed study of multiplicity and architecture is generally hampered by limitations in quality, temporal extension and observing strategy, causing difficulties in detecting low-mass inner planets in the presence of outer giant planets. Aims. We present the results of high-cadence and high-precision HARPS observations on 20 solar-type stars known to host a single long-period giant planet in order to search for additional inner companions and estimate the occurence rate fp of scaled solar system analogues – in other words, systems featuring lower-mass inner planets in the presence of long-period giant planets.
  • SILICON and OXYGEN ABUNDANCES in PLANET-HOST STARS Erik Brugamyer, Sarah E

    SILICON and OXYGEN ABUNDANCES in PLANET-HOST STARS Erik Brugamyer, Sarah E

    The Astrophysical Journal, 738:97 (11pp), 2011 September 1 doi:10.1088/0004-637X/738/1/97 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. SILICON AND OXYGEN ABUNDANCES IN PLANET-HOST STARS Erik Brugamyer, Sarah E. Dodson-Robinson, William D. Cochran, and Christopher Sneden Department of Astronomy and McDonald Observatory, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712, USA; [email protected] Received 2011 February 4; accepted 2011 June 22; published 2011 August 16 ABSTRACT The positive correlation between planet detection rate and host star iron abundance lends strong support to the core accretion theory of planet formation. However, iron is not the most significant mass contributor to the cores of giant planets. Since giant planet cores are thought to grow from silicate grains with icy mantles, the likelihood of gas giant formation should depend heavily on the oxygen and silicon abundance of the planet formation environment. Here we compare the silicon and oxygen abundances of a set of 76 planet hosts and a control sample of 80 metal-rich stars without any known giant planets. Our new, independent analysis was conducted using high resolution, high signal-to-noise data obtained at McDonald Observatory. Because we do not wish to simply reproduce the known planet–metallicity correlation, we have devised a statistical method for matching the underlying [Fe/H] distributions of our two sets of stars. We find a 99% probability that planet detection rate depends on the silicon abundance of the host star, over and above the observed planet–metallicity correlation.