BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Poster popups DTSTART;VALUE=DATE-TIME:20230511T131500Z DTEND;VALUE=DATE-TIME:20230511T133000Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-412@meetings.aip.de DESCRIPTION:Speakers: Andrei Gorobets (Leibniz-KIS)\, Carsten Denker (Leib niz Institute for Astrophysics Potsdam (AIP))\, Francesco Berrilli (Univer sity of Rome Tor Vergata)\, Malcolm Druett (KU Leuven)\, Meetu Verma (Leib niz-Institut für Astrophysik Potsdam (AIP))\, Saida Milena Diaz Castillo (Leibniz Institute for Solar Physics - KIS)\, Sanghita Chandra (Max Planck Institute for Solar System Research)\nFrancesco Berrilli - The Multiscale Magnetic Signature of the Solar Turbulent Magneto-Convection\nAndrei Goro bets - Co-existence of self-similarity and anomalous scaling in photospher ic turbulent small-scale magnetic fields\nMalcolm Druett - Comparing the e volution of mottles and fibrils in a radiation-MHD simulation\nCarsten Den ker - Instruments for High-resolution Solar Observations\nSaida Milena Dia z Castillo - Signatures of an impulsive jet in a small-scale magnetic torn ado: Spectro-polarimetric observations of a dynamic photospheric small-sca le magnetic vortex associated with a chromospheric swirl\n\nhttps://meetin gs.aip.de/event/24/contributions/412/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/412/ END:VEVENT BEGIN:VEVENT SUMMARY:Solar-cycle variation of the quiet-sun magnetism DTSTART;VALUE=DATE-TIME:20230511T102000Z DTEND;VALUE=DATE-TIME:20230511T103500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-337@meetings.aip.de DESCRIPTION:Speakers: Andreas Korpi-Lagg (Max Planck Institute for Solar S ystem Research / Aalto University)\nSolar dynamo models can explain the pr oduction and maintenence of the solar magnetic fields on two different spa tial scales: the large-scale solar dynamo\, manifested in the cycle-depend ent appearance of solar active regions\, and the small-scale solar dynamo\ , driven by the turbulent convective motions close to the solar surface. D isentangling these two mechanisms observationally is extremely challenging \, but provides important input for the dynamo models. Highly stable long- term observations with sufficient magnetic sensitivity are required.\n\nTh e Helioseismic Imager on board the Solar Dynamics Observatory (SDO/HMI) ha s measured the solar magnetic field for more than one solar cycle. In ths work\, we present the results of these 13-year long magnetic field measure ments in the most quiet patches of the solar surface after applying a comb ination of a temporal and spatial averaging algorithm and a careful select ion process. The results provide strong evidence for a solar-cycle modulat ion in even the most quiet patches when they include network fields. In co ntrast\, the modulation is absent in the internetwork fields\, where only the interior of the supergranular cells is included in the analysis.\n\nWe interpret the absence of a solar-cycle modulation in the internetork fiel ds as a consequence of them being generated by the small-scale (or fluctua ting) dynamo acting on scales smaller than a supergranular cell. The solar cycle modulation when including the network fields can be explained by ta ngling of the solar-cycle dependent large-scale sub-surface field.\n\nhttp s://meetings.aip.de/event/24/contributions/337/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/337/ END:VEVENT BEGIN:VEVENT SUMMARY:Data-driven model of temporal evolution of the solar Mg II h & k p rofiles over the solar cycle DTSTART;VALUE=DATE-TIME:20230511T100500Z DTEND;VALUE=DATE-TIME:20230511T102000Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-341@meetings.aip.de DESCRIPTION:Speakers: Julius Koza (Astronomical Institute\, Slovak Academy of Sciences)\nThe solar radiation in the cores of the Mg II h & k spectra l lines strongly correlates with solar magnetic activity and global variat ions of magnetic fields with the solar cycle. This work provides a data-dr iven model of temporal evolution of the solar full-disk Mg II h & k profil es over the solar cycle. Based on selected 76 IRIS near-UV full-Sun mosaic s covering almost the full solar cycle 24\, we find the parameters of doub le-Gaussian fits of the disk-averaged Mg II h & k profiles and a model of their temporal evolution parameterized by the Bremen composite Mg II index . The Markov Chain Monte Carlo algorithm implemented in the IDL toolkit So BAT is used in modeling and predicting temporal evolution of the Mg II h & k peak-to-center intensity ratio and the Bremen Mg II index. The relevan t full-disk Mg II h & k calibrated profiles with uncertainties and spectra l irradiances are provided as an online machine-readable table. To facilit ate utilization of the model corresponding routines\, written in IDL\, are made publicly available at GitHub.\n\nhttps://meetings.aip.de/event/24/co ntributions/341/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/341/ END:VEVENT BEGIN:VEVENT SUMMARY:Role of spots in stellar Ca II H & K emissions: what can we learn from spots on the Sun? DTSTART;VALUE=DATE-TIME:20230511T095000Z DTEND;VALUE=DATE-TIME:20230511T100500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-340@meetings.aip.de DESCRIPTION:Speakers: Sowmya Krishnamurthy (Max Planck Institute for Solar System Research)\nEmission in the Ca II H & K spectral lines is sensitive to the changes in the stellar magnetic activity and is a good proxy for s tudying stellar magnetic fields. This emission is most commonly characteri zed via the S-index\, representing the flux in the Ca II H & K line cores relative to the flux in the nearby continuum. The sources of stellar Ca II emissions are yet to be investigated in detail. Empirical and physics-bas ed models have shown faculae/plage to be the main source of Ca II emission s and thus neglect the contribution from spots. This is because the solar surface coverage by spots is much smaller than those by faculae. Further\, spots are assumed to be equally dark in the Ca II line cores and the cont inuum so that they do not affect the S-index. While this is a good approxi mation for old less-active stars such as the Sun\, for young active stars with large surface coverages by spots\, the role played by spots might bec ome significant. \n\n\nHere we use high quality sunspot observations in th e Ca II H line from the Swedish Solar Telescope to determine the Ca II flu x from chromospheric counterparts of sunspots. We find that spots are brig hter than the surrounding quiet regions in the chromosphere. Using the sun spot flux computed from observations in our physics-based model which also accounts for the effect of faculae\, we compute S-index for four solar ac tivity cycles. We find that sunspots lead to an increase in the S-index. H owever\, this increase is quite small to have a significant impact on the observed solar Ca II emissions. Further\, we compute S-indices considering cases of stars which are more active than the Sun. Previous studies have indicated that surface coverages of spots increase much faster with increa sing activity than the coverages by faculae. We show that with increasing activity and hence spot area coverages\, S-index increases steeply suggest ing that Ca II emissions of active stars have a significant contribution f rom spots.\n\nhttps://meetings.aip.de/event/24/contributions/340/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/340/ END:VEVENT BEGIN:VEVENT SUMMARY:Power supply and evolution of the solar dynamo DTSTART;VALUE=DATE-TIME:20230511T093500Z DTEND;VALUE=DATE-TIME:20230511T095000Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-338@meetings.aip.de DESCRIPTION:Speakers: Quentin Noraz (Rosseland Centre for Solar Physics\, University of Oslo\, P.O. Box 1029 Blindern\, Oslo\, NO-0315\, Norway)\nTh e solar magnetic field is generated and sustained by the combined action o f turbulent convection and differential rotation. This dynamo process can sometimes lead to magnetic cyclic variabilities\, like the solar 11 years cycle. Traces of magnetic cycles have also been detected in other solar-li ke stars\, ranging from a few years to a few tens of years. How is the sol ar cycle period controlled?\nRecent 3D numerical simulations of solar-like stars show that different regimes of differential rotation can be charact erized with the Rossby number (advection over Coriolis force). In particul ar\, “anti-solar” differential rotation (fast poles\, slow equator) ma y appear for high Rossby number (slow rotators). If large-scale flows tran sitions occur during the solar main sequence\, we may wonder how the magne tic generation will be impacted.\n\nWe present a numerical multi-D study t o understand the magnetic field generation and evolution of solar-like sta rs under various differential rotation regimes\, in a Sun in time context. We find that short and local cycles near the surface are favoured for sma ll Rossby numbers (fast rotators)\, while long and global cycles appear fo r intermediate (solar-like) Rossby numbers. Slow rotators (high Rossby num ber) are found to produce statistically steady dynamo with no cyclic activ ity in most cases considered. We further evaluate energy transfers in thes e models and quantify that dynamos can be powered by up to 3% of the stell ar luminosity\, part of it being then available to power surface events. I n this regard\, future Solar Orbiter observations outside the ecliptic wil l provide fantastic constraints on solar polar caps magnetic field\, and t hus on the type of dynamo that our Sun is most likely to operate.\n\nhttps ://meetings.aip.de/event/24/contributions/338/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/338/ END:VEVENT BEGIN:VEVENT SUMMARY:The relation of the Sun’s global magnetic field with the solar w ind parameters on solar cycle time-scales DTSTART;VALUE=DATE-TIME:20230511T081000Z DTEND;VALUE=DATE-TIME:20230511T082500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-339@meetings.aip.de DESCRIPTION:Speakers: Raffaele Reda (University of Rome Tor Vergata)\nVari ations of the solar magnetic field are the main sources of several manifes tations of the solar activity (e.g. flares\, CMEs\, solar wind). A way to quantify such variations is by means of a physical index\, the Ca II K ind ex\, which has been proven to be a great proxy for the line-of-sight unsig ned magnetic flux density along all phases of the cycle\, and not only whe n sunspots are present.\nIn this respect\, an assessment of the long-term behaviour of the solar wind is of paramount importance to understand the n ature of its relationship with the global magnetic field of the Sun and wi th its cycle-to-cycle variations. Here\, we study the variations of physic al proxies of the solar activity (i.e. Ca II K index\, Mg II index)\, on s olar cycle time-scales\, and how they are related to variations of solar w ind parameters. The available time series allow to evaluate this relation over the last five solar cycles (from 1965 to now).\nBy adopting a climato logical approach\, the results show that there is a delayed response of th e solar wind with respect to the solar activity\, but such response is not the same for the different solar cycles. The analysis offers the possibil ity to deepen the understanding of the processes that link the global dyna mo to solar variability and to the properties of the solar wind near the E arth.\n\nhttps://meetings.aip.de/event/24/contributions/339/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/339/ END:VEVENT BEGIN:VEVENT SUMMARY:Examining the Closed Magnetic Field Lines Crossing the Coronal Hol e Boundaries DTSTART;VALUE=DATE-TIME:20230511T075500Z DTEND;VALUE=DATE-TIME:20230511T081000Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-342@meetings.aip.de DESCRIPTION:Speakers: Chia-Hsien Lin (Department of Space Science and Engi neering\, National Central University)\nSolar coronal holes (CHs) are the regions with low coronal emissions and an unbalanced magnetic flux\, which led to the common expectation that their magnetic structures are mostly ` `open''\, or\, in other words\, extending to infinity. The objective of th is study is to examine the CH magnetic structures to verify this expectati on. The coronal holes are identified from the synoptic maps constructed us ing the AIA 193 images and HMI line-of-sight magnetograms from 2010 June t o 2020 February. The magnetic structures of the CHs are constructed using the Potential Field Source Surface (PFSS) model. As a comparison\, the dat a from a thermodynamic magnetohydrodynamic (MHD) model are also used. The results from both models reveal that there is a significant percentage of closed field lines extending beyond the CH boundaries\, leading to an unba lanced magnetic flux within the boundaries. The boundary-crossing field li nes tend to be located slightly closer to the CH boundaries\, and are more likely to be found in the lower latitudes during active times. The result s also show that more than 50% (17%) of PF (MHD) CHs do not contain open m agnetic field lines. The CHs without open field lines are often smaller an d less unipolar than those with open field lines.\n\nhttps://meetings.aip. de/event/24/contributions/342/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/342/ END:VEVENT BEGIN:VEVENT SUMMARY:Long-term variability of solar magnetic flux and irradiance DTSTART;VALUE=DATE-TIME:20230511T073000Z DTEND;VALUE=DATE-TIME:20230511T075500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-366@meetings.aip.de DESCRIPTION:Speakers: Natalie Krivova (Max Planck Institute for Solar Syst em Research)\nMeasurements of solar irradiance and surface magnetic flux s ufficiently accurate as to allow assessment of their variability are only available for roughly half a century. Variability on longer time scales is evidenced by proxies. Upon emergence\, the magnetic field on the Sun mani fests itself as dark (sunspots and pores) and bright (faculae/plage and ne twork) features. The combined effect of their evolution and the solar rota tion is the modulation of the solar irradiance. Models relating the variab ility of the solar irradiance to the evolution of the solar surface magnet ic flux account for almost all of the measured variability. Reconstruction s of past variability are\, however\, thwarted by the lack of reliable lon g-term proxies of solar surface magnetism\, in particular those describing bright magnetic features (faculae and network). We will review our recent efforts to improve understanding of the long-term changes in solar magnet ic activity and irradiance. These include recovery and analysis of suitabl e proxies of past solar magnetic activity\, examination of the link betwee n sunspot and facular emergence and evolution\, as well as modelling effor ts to tighten constraints on the long-term solar variability.\n\nhttps://m eetings.aip.de/event/24/contributions/366/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/366/ END:VEVENT BEGIN:VEVENT SUMMARY:Coronal flux ropes over Solar Cycle 24 DTSTART;VALUE=DATE-TIME:20230508T130500Z DTEND;VALUE=DATE-TIME:20230508T133000Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-355@meetings.aip.de DESCRIPTION:Speakers: Anthony Yeates (Durham University)\nQuasi-static mod elling of the Sun’s corona using the magneto-frictional approximation ma kes predictions of how its large-scale magnetic structure might vary over the solar cycle. Unlike the traditional potential field source surface mod el\, this approach is able to probe the effects of low coronal electric cu rrents and the corresponding free magnetic energy. In particular\, ongoing footpoint shearing and flux cancellation lead to the concentration of fre e energy within closed-field regions\, naturally forming sheared arcades a nd magnetic flux ropes. I will show model results for Cycle 24 driven by m agnetogram data from SDO/HMI\, with the aim of comparing to earlier result s from a decade ago for Cycle 23. In particular\, we will consider how sol ar flux ropes and their eruptions vary over the solar cycle\, at least acc ording to this model.\n\nhttps://meetings.aip.de/event/24/contributions/35 5/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/355/ END:VEVENT BEGIN:VEVENT SUMMARY:On the origin of the Solar Mean Magnetic Field DTSTART;VALUE=DATE-TIME:20230511T130000Z DTEND;VALUE=DATE-TIME:20230511T131500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-346@meetings.aip.de DESCRIPTION:Speakers: Vishnu M (Indian Institute of Astrophysics)\nThe Sol ar Mean Magnetic Field (SMMF) is the average value of the line-of-sight (L OS) magnetic field considered over the visible hemisphere of the Sun. Vari ous synoptic observations of the solar magnetic field have shown that the SMMF has a periodicity of ~ 27 days\, and an amplitude that varies accordi ng to the solar cycle\, from ±0.2 G during solar minima to ±2 G during s olar maxima. It has also been shown that the SMMF has a good correlation w ith the Interplanetary Magnetic Field (IMF). Nevertheless\, the origin of the SMMF is still a controversial subject. Till date\, SMMF measurements h ave always been carried out using photospheric spectral lines only. In thi s regard\, we utilised full-disk LOS magnetograms from the Vector Spectrom agnetograph (VSM) (one of the instruments in SOLIS - Synoptic Optical Long -term Investigations of the Sun)\, calculated the SMMF as the disk-average d magnetic field in each magnetogram\, and compared the SMMF at photospher ic and chromospheric heights. Our comparison showed that the SMMF at the c hromosphere is a factor of 0.6 times the SMMF at the photosphere\, with a correlation coefficient of 0.80\; indicating that a considerable fraction of the SMMF might be propagating outwards from the photosphere to the chro mosphere. This brings us one step closer to understanding the connection b etween the SMMF and the IMF. Further\, to understand the origin of the SMM F\, which is a magnetic flux imbalance\, we are studying the full-disk Sto kes I and Stokes V data from VSM\, which are disk-averaged to create Stoke s profiles. Any localised source of the SMMF should reflect in the Stokes V profile as a rotationally modulated doppler shift. Our initial analyses show that there is a periodicity in the Stokes V doppler shift. This perio dicity is being analysed along with associated magnetograms\, to understan d the source of the SMMF.\n\nhttps://meetings.aip.de/event/24/contribution s/346/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/346/ END:VEVENT BEGIN:VEVENT SUMMARY:The effects of the surface inflows on quenching of solar cycles DTSTART;VALUE=DATE-TIME:20230511T124500Z DTEND;VALUE=DATE-TIME:20230511T130000Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-345@meetings.aip.de DESCRIPTION:Speakers: MOHAMMED TALAFHA (Dept. of Space Physics and Technol ogy\, Wigner Research Centre for Physics)\nRecently\, there has been consi deration of two possible methods for the nonlinear modulation of solar cyc le amplitudes. The first mechanism\, known as Tilt Quenching (TQ)\, involv es a negative feedback relationship between the cycle amplitude and the me an tilt angle of bipolar active regions relative to the azimuthal directio n. The second mechanism\, known as Latitude Quenching (LQ)\, involves a po sitive correlation between the average emergence latitude of active region s and the cycle amplitude.\nHere we study the effects of quenching paramet ers on the Surface Flux Transport (SFT) models and the effects of implemen ting the surface inflows into the SFT models on the two different observab le nonlinearities: TQ and LQ \nOur SFT models are grid-based. We have meth odically investigated the extent of nonlinearity caused by TQ and LQ\, as well as their combination in the presence of surface inflows.\nA prelimina ry result is that there is a linear dependence of quenching parameters on the dipole moment. This is expected from the model. A second finding is th at the effects of introducing surface inflows to the SFT models will produ ce lower values of dipole moments for the different cases of quenching in the solar cycle.\n\nhttps://meetings.aip.de/event/24/contributions/345/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/345/ END:VEVENT BEGIN:VEVENT SUMMARY:Differential Rotation of the Solar Chromosphere using multidecadal Ca K spectroheliograms DTSTART;VALUE=DATE-TIME:20230511T123000Z DTEND;VALUE=DATE-TIME:20230511T124500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-343@meetings.aip.de DESCRIPTION:Speakers: Dibya Kirti Mishra (ARIES\, India)\nDifferential rot ation is a key aspect of the solar dynamo model and is well-established in the Sun's interior and photosphere. However\, our understanding of the ch romosphere and upper atmosphere's differential rotation is limited and has yielded contradictory results in previous studies. To address this\, we u tilized a century-long dataset of Ca II K images (1907-2007) from the Koda ikanal Solar Observatory (KoSO) to investigate the chromosphere's rotation profile during different solar cycles. By employing the image correlation analysis on sets of consecutive day images\, we found that the chromosphe re rotates 1.52% faster than the photosphere but with less differential ro tation compared to the photosphere values. To validate our method and resu lts\, we applied the same technique to MDI white light data and other Ca I I K data sources (Meudon and PSPT/Rome) and obtained consistent results. M oreover\, we examined the solar cycle dependence of differential rotation parameters and investigated the north-south asymmetry of the solar rotatio n profile.\n\nhttps://meetings.aip.de/event/24/contributions/343/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/343/ END:VEVENT BEGIN:VEVENT SUMMARY:Revisiting the long-term evolution of the Sun’s magnetic field: Solar wind sources and coronal rotation DTSTART;VALUE=DATE-TIME:20230511T121500Z DTEND;VALUE=DATE-TIME:20230511T123000Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-347@meetings.aip.de DESCRIPTION:Speakers: Adam Finley (CEA Paris-Saclay)\nThe Sun’s large-sc ale magnetic field undergoes periodic reversals due to the activity of the dynamo within the solar interior. The evolution of the Sun’s magnetic f ield has a clear impact on the structure of the corona and solar wind abov e. Here we show results from the spherical harmonic decomposition of the S un’s photospheric magnetic field\, using WSO\, SOHO/MDI and SDO/HMI syno ptic magnetograms that span sunspot cycles 21-24\, plus cycle 25 to presen t. From this\, trends in the magnetic field components (notably the lowest order\, dipole\, quadrupole and octupole) are extracted and compared betw een cycles. In addition\, we perform potential field source surface modeli ng of the coronal magnetic field\, in order to make inferences about the s olar wind sources and likely coronal rotation rate. These results are comp ared against scattered whitelight observations of the corona from MLSO/K-C or and SOHO/LASCO-C2. The role of nested flux emergence and poleward surge s of magnetic flux will be discussed in this context\, with future links t o heliospheric missions like Solar Orbiter and Parker Solar Probe.\n\nhttp s://meetings.aip.de/event/24/contributions/347/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/347/ END:VEVENT BEGIN:VEVENT SUMMARY:Solar Irradiance Variability - From Measurements to Modelling DTSTART;VALUE=DATE-TIME:20230511T115000Z DTEND;VALUE=DATE-TIME:20230511T121500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-360@meetings.aip.de DESCRIPTION:Speakers: Margit Haberreiter (PMOD/WRC)\nThe total and spectra l solar irradiance\, TSI and SSI\, respectively\, vary on many timescales from sub-daily variations to annual\, decadal\, centennial timescales. The variations of the SSI are also wavelength dependent\, with larger relativ e variations in the EUV/UV and smaller variations in the visible and IR. T hese irradiance variations allow us to understand\, on the one hand\, the physics of the Sun as a star and\, on the other hand\, the key energy sour ce for the Earth's climate system. In this talk I will review the availabl e irradiance measurements\, composite datasets\, models and how the underl ying physics\, which drives the irradiance variations\, is implemented.\n\ nhttps://meetings.aip.de/event/24/contributions/360/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/360/ END:VEVENT BEGIN:VEVENT SUMMARY:Changes in the Lower Solar Atmosphere throughout the Solar Cycle DTSTART;VALUE=DATE-TIME:20230512T070000Z DTEND;VALUE=DATE-TIME:20230512T071500Z DTSTAMP;VALUE=DATE-TIME:20240704T115550Z UID:indico-contribution-62-344@meetings.aip.de DESCRIPTION:Speakers: James Crowley (National Solar Observatory\; Universi ty of Colorado\, Boulder)\nThe change in the distribution of the magnetic field in the quiet Sun photosphere over the solar cycle could be expected to cause systematic variations in the photospheric thermodynamic structure . This could be due to changes in the dynamics of the convective overshoot or radiative properties. To look for such changes\, we use high spatial a nd spectral resolution spectropolarimetric observations obtained by Hinode SOT and apply the Spectropolarimetric Inversions Based on Response Functi ons (SIR) code to infer physical conditions in the lower solar photosphere . By using multiple homogeneous datasets acquired over 15 years\, we analy ze the distributions of the inferred parameters in the granules and interg ranules of magnetic and non-magnetic spectra throughout the solar cycle. T he final goal of our study is to characterize changes in the inferred atmo spheric parameters\, notably\, the temperature structure\, the line-of-sig ht velocities\, and magnetic properties.\n\nhttps://meetings.aip.de/event/ 24/contributions/344/ LOCATION:Haus H\, Telegrafenberg URL:https://meetings.aip.de/event/24/contributions/344/ END:VEVENT END:VCALENDAR