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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
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