Magnétisme, activité et interactions magnétosphériques dans les systèmes étoile/planète géante proche

Les planètes extrasolaires en orbite proche (Jupiter chauds ou Pégasides) sont soumises à de fortes interactions avec leur étoile: rayonnement, effets gravitationnels, flot de particules, champ magnétique. La planète, baignée dans le champ magnétique de son étoile tout au long de son orbite, peut déclencher des réactions en retour sur son étoile, qui se manifesteraient par exemple par une activité photosphérique induite ou une influence sur le champ magnétique stellaire par interactions de marée. Au cours de cette thèse, le suivi en spectropolarimétrie d'un échantillon d'étoiles hôtes de Jupiter chaud m'a permis d'étudier la structure et l'évolution de leur champ magnétique par imagerie Zeeman-Doppler. Les étoiles étudiées montrent des caractéristiques magnétiques similaires celles des étoiles froides sans Jupiter chaud. Mais pour la première fois, un cycle magnétique a été observé pour une autre étoile que le Soleil. Comparé au cycle magnétique solaire, ce cycle est accéléré, suggérant que la planète pourrait influencer l'étoile. J'ai également exploré un deuxième moyen d'étude de l'influence planétaire sur l'étoile: l'activité stellaire. En plus de ce travail observationnel, j'ai étudié le champ magnétique dans la couronne stellaire, par extrapolation des magnétogrammes de surface. J'ai pu calculer ainsi le budget énergétique au niveau de la planète, un ingrédient essentiel dans la prédiction de l'émission radio exoplanétaire effectué pendant cette thèse.Extrasolar planets at small orbital distances (hot Jupiters)interact with their hosting star in several ways: irradiation, gravitation, flow of particles and magnetic fields. The planet, embedded in the large-scale stellar magnetic field throughout its orbit, can influence the star in the form of induced photospheric activity, or by influencing the stellar magnetic field via tidal interactions. Over the course of this PhD, spectropolarimetric observations of a sample of stars with a hot Jupiter allowed me to study their magnetic structure and evolution via Zeeman-Doppler Imaging. These stars show similar magnetic properties to other cool stars without Hot Jupiter. But, for the first time, a magnetic cycle on a star other than the Sun was observed. Compared to the solar cycle, this cycle is accelerated, suggesting that the planet may influence the stellar magnetic field. I have also used a second method to study the planet's influence on the star : the stellar activity. In addition to this observational study, I have examined the coronal magnetic field by extrapolating the surface magnetograms. I was thus able to calculate the magnetic budget at the planet's orbit, an important ingredient for my estimations of the planetary radio flux

A small survey of the magnetic fields of planet-host stars

Using spectropolarimetry, we investigate the large-scale magnetic topologies of stars hosting close-in exoplanets. A small survey of ten stars has been done with the twin instruments TBL/NARVAL and CFHT/ESPaDOnS between 2006 and 2011. Each target consists of circular-polarization observations covering 7 to 22 days. For each of the 7 targets in which a magnetic field was detected, we reconstructed the magnetic field topology using Zeeman-Doppler imaging. Otherwise, a detection limit has been estimated. Three new epochs of observations of Tau Boo are presented, which confirm magnetic polarity reversal. We estimate that the cycle period is 2 years, but recall that a shorter period of 240 days can not still be ruled out. The result of our survey is compared to the global picture of stellar magnetic field properties in the mass-rotation diagram. The comparison shows that these giant planet-host stars tend to have similar magnetic field topologies to stars without detected hot-Jupiters. This needs to be confirmed with a larger sample of stars.Comment: Accepted for publication in Monthly Notices of The Royal Astronomical Societ

Star-Planet Interactions

Much effort has been invested in recent years, both observationally and theoretically, to understand the interacting processes taking place in planetary systems consisting of a hot Jupiter orbiting its star within 10 stellar radii. Several independent studies have converged on the same scenario: that a short-period planet can induce activity on the photosphere and upper atmosphere of its host star. The growing body of evidence for such magnetic star-planet interactions includes a diverse array of photometric, spectroscopic and spectropolarimetric studies. The nature of which is modeled to be strongly affected by both the stellar and planetary magnetic fields, possibly influencing the magnetic activity of both bodies, as well as affecting irradiation and non-thermal and dynamical processes. Tidal interactions are responsible for the circularization of the planet orbit, for the synchronization of the planet rotation with the orbital period, and may also synchronize the outer convective envelope of the star with the planet. Studying such star-planet interactions (SPI) aids our understanding of the formation, migration and evolution of hot Jupiters.Comment: 8 pages, proceedings of Cool Stars 15, St. Andrews, July 2008, to be published in the Conference Proceedings Series of the American Institute of Physics - "Star-planet interactions" splinter session summar

The Sun as a planet-host star : proxies from SDO images for HARPS radial-velocity variations

RDH gratefully acknowledges STFC studentship grant number ST/J500744/1, and a grant from the John Templeton Foundation. ACC and RF acknowledge support from STFC consolidated grants numbers ST/J001651/1 and ST/M001296/1. JL acknowledges support from NASA Origins of the Solar System grant No. NNX13AH79G and from STFC grant ST/M001296/1.The Sun is the only star whose surface can be directly resolved at high resolution, and therefore constitutes an excellent test case to explore the physical origin of stellar radial-velocity (RV) variability. We present HARPS observations of sunlight scattered off the bright asteroid 4/Vesta, from which we deduced the Sun's activity-driven RV variations. In parallel, the Helioseismic and Magnetic Imager instrument on board the Solar Dynamics Observatory provided us with simultaneous high spatial resolution magnetograms, Dopplergrams and continuum images of the Sun in the Fe i 6173 Å line. We determine the RV modulation arising from the suppression of granular blueshift in magnetized regions and the flux imbalance induced by dark spots and bright faculae. The rms velocity amplitudes of these contributions are 2.40 and 0.41 m s−1, respectively, which confirms that the inhibition of convection is the dominant source of activity-induced RV variations at play, in accordance with previous studies. We find the Doppler imbalances of spot and plage regions to be only weakly anticorrelated. Light curves can thus only give incomplete predictions of convective blueshift suppression. We must instead seek proxies that track the plage coverage on the visible stellar hemisphere directly. The chromospheric flux index R′HK derived from the HARPS spectra performs poorly in this respect, possibly because of the differences in limb brightening/darkening in the chromosphere and photosphere. We also find that the activity-driven RV variations of the Sun are strongly correlated with its full-disc magnetic flux density, which may become a useful proxy for activity-related RV noise.PostprintPeer reviewe

Magnetic activity and hot Jupiters of young Suns : the weak-line T Tauri stars V819 Tau and V830 Tau

SGG acknowledges support from the Science & Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship [ST/J003255/1]. SHPA acknowledges financial support from CNPq, CAPES and Fapemig. AAV acknowledges support from the Swiss National Science Foundation (SNSF) via the allocation of an Ambizione Followship. Date of Acceptance: 06/08/2015We report results of a spectropolarimetric and photometric monitoring of the weak-line T Tauri stars (wTTSs) V819 Tau and V830 Tau within the MaTYSSE (Magnetic Topologies of Young Stars and the Survival of close-ingiant Exoplanets) programme, involving the ESPaDOnS spectropolarimeter at the Canada-France-Hawaii Telescope. At ≃3 Myr, both stars dissipated their discs recently and are interesting objects for probing star and planet formation. Profile distortions and Zeeman signatures are detected in the unpolarized and circularly polarized lines, whose rotational modulation we modelled using tomographic imaging, yielding brightness and magnetic maps for both stars. We find that the large-scale magnetic fields of V819 Tau and V830 Tau are mostly poloidal and can be approximated at large radii by 350-400 G dipoles tilted at≃30° to the rotation axis. They are significantly weaker than the field of GQ Lup, an accreting classical T Tauri star (cTTS) with similar mass and age which can be used to compare the magnetic properties of wTTSs and cTTSs. The reconstructed brightness maps of both stars include cool spots and warm plages. Surface differential rotation is small, typically ≃4.4 times smaller than on the Sun, in agreement with previous results on wTTSs. Using our Doppler images to model the activity jitter and filter it out from the radial velocity(RV) curves, we obtain RV residuals with dispersions of 0.033 and 0.104km s-1 for V819 Tau and V830 Tau, respectively. RV residuals suggest that a hot Jupiter may be orbiting V830 Tau, though additional data are needed to confirm this preliminary result. We find no evidence for close-in giant planet around V819 Tau.Publisher PDFPeer reviewe

A spectro-polarimetric study of the planet-hosting G dwarf, HD 147513

The results from a spectro-polarimetric study of the planet-hosting Sun-like star, HD 147513 (G5V), are presented here. Robust detections of Zeeman signatures at all observed epochs indicate a surface magnetic field, with longitudinal magnetic field strengths varying between 1.0–3.2 G. Radial velocity variations from night to night modulate on a similar timescale to the longitudinal magnetic field measurements. These variations are therefore likely due to the rotational modulation of stellar active regions rather than the much longer timescale of the planetary orbit (Porb = 528 d). Both the longitudinal magnetic field measurements and radial velocity variations are consistent with a rotation period of 10 ± 2 days, which are also consistent with the measured chromospheric activity level of the star (′log R′HK = -4.64). Together, these quantities indicate a low inclination angle, i ~ 18°. We present preliminary magnetic field maps of the star based on the above period and find a simple poloidal large-scale field. Chemical analyses of the star have revealed that it is likely to have undergone a barium-enrichment phase in its evolution because of a higher mass companion. Despite this, our study reveals that the star has a fairly typical activity level for its rotation period and spectral type. Future studies will enable us to explore the long-term evolution of the field, as well as to measure the stellar rotation period, with greater accuracy.Publisher PDFPeer reviewe

Estimating magnetic filling factors from Zeeman–Doppler magnetograms

V.S., S.P.M., and A.J.F.acknowledge funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (grant agreement No. 682393 AWESoMeStars). S.B.S. acknowledges funding via the Austrian Space Application Programme (ASAP) of the Austrian Research Promotion Agency (FFG) within ASAP11, the FWF NFN project S11601-N16 and the sub-project S11604-N16. A. A.V. acknowledges funding received from the Irish Research Council Laureate Awards 2017/2018.Low-mass stars are known to have magnetic fields that are believed to be of dynamo origin. Two complementary techniques are principally used to characterize them. Zeeman–Doppler imaging (ZDI) can determine the geometry of the large-scale magnetic field while Zeeman broadening can assess the total unsigned flux including that associated with small-scale structures such as spots. In this work, we study a sample of stars that have been previously mapped with ZDI. We show that the average unsigned magnetic flux follows an activity-rotation relation separating into saturated and unsaturated regimes. We also compare the average photospheric magnetic flux recovered by ZDI, BV, with that recovered by Zeeman broadening studies, BI. In line with previous studies, BV ranges from a few % to ~20% of BI. We show that a power-law relationship between BV and BI exists and that ZDI recovers a larger fraction of the magnetic flux in more active stars. Using this relation, we improve on previous attempts to estimate filling factors, i.e., the fraction of the stellar surface covered with magnetic field, for stars mapped only with ZDI. Our estimated filling factors follow the well-known activity-rotation relation, which is in agreement with filling factors obtained directly from Zeeman broadening studies. We discuss the possible implications of these results for flux tube expansion above the stellar surface and stellar wind models.Publisher PDFPeer reviewe

Hur mogen är marknaden för klimatsmart betong och dess aktörer?

Carbon dioxide emissions have long proven to be one of the greenhouse gases that affect our planet's climate and environment. With the upcoming EU targets and Sweden's own net zero targets, the construction and real estate sector is required to work with climate-smart materials to construct the buildings of the future. The net zero target for year 2045 requires a joint pool of power from all companies to find innovative solutions to reduce carbon dioxide emissions. The purpose of this study was to investigate how conscious and active the construction and real estate sector is for climate-smart concrete through a survey and comparison of different typ of concretes EPDs. The work aims to investigate how far the development has taken place and to investigate how the market has adopted the new products that are available. The purpose was also to investigate which alternative additives are most common and the advantages and disadvantages of the climate-smart concrete. Climate smart is a term for concrete that contains a lower percentage of Portland cement clinker than the traditional concrete. A questionnaire was created to answer the purpose of the study. The survey sent out involved questions about how companies view the new environmental target for year 2045. As well as investigating how the construction and real estate sector works together to achieve the goal of reducing carbon dioxide emissions by 85% less than in year 1990. A comparison was made between three different EPDs of climate-smart concrete and two reference concrete with ordinary Portland cement clinker. Reference concrete one is a standard value derived from previous studies made and reference concrete two is an EPD value. This was done to investigate the amount of carbon dioxide they emit at the production stage. A reference building was used to calculate the amount of concrete. The result shows that the comparison between reference concrete one with the standard value and the three climate-smart concrete from Svensk Betong, Betongindustrin and Swerock gives a carbon dioxide reduction of 29.3%. And the comparison with reference concrete two with the associated EPD value received a percent climate reduction of only 2.8%. The future will require the construction and real estate industry to invest time and training to work with climate-smart concrete. More in-depth work could be explored and mapped as to which are the major obstacles in construction projects. How companies can work to get the entire value chain to work together for a climate-smart thinking and primarily to get the developer to invest in improved concrete with less climate impact