P ojec : 101079231 — EXOHOST — HORIZON-WIDERA-2021-ACCESS-03
14-17 Oc obe 2025
Ta u, Es onia
EXPLORING
STAR-PLANET-DISK
CONNECTIONS
CONFERENCE ABSTRACT BOOK
Edi ed by Lau i s Leedjä and Alexand a Leh me s
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 2
Table o Con en s
In oduc ion ......................................................................................................................... 6
Session 1: Fundamen al S ella P ope ies ........................................................................ 7
In i ed Speake : Camilla Danielski - The S a Se s he S age: Unde s anding
Exoplane s Th ough Thei Hos s ..................................................................................... 7
Alix F eckel on - The G 8s a s Ca alogue: a Public Lib a y o FGKM Dwa Spec a
and Thei Homogeneously De i ed Pa ame e s. ............................................................. 8
La a Pisca e a - Acc e ion Makes Young S a s Look Old: Lessons om O ion ......... 8
Ma hias Ammle - on Ei - How o Imp o e he Cha ac e iza ion o Dis an S a s
wi h T ansi ing Exoplane s? ............................................................................................ 9
Nicola Mille - Eclipsing Bina ies as Benchma k S a s: Add essing he “E ec i e
Tempe a u e” Elephan in he Room ............................................................................. 10
And eas Qui enbach - Te es ial Plane s O bi ing Low-mass S a s ..................... 11
Tõnis Eenmäe - Enhancing No he n Sky Moni o ing: Upg ades o Ta u
Obse a o y’s 1.5 m Telescope o High
‑
Resolu ion Spec oscopy and Mul i
‑
Band
Pho ome y ..................................................................................................................... 11
Session 2: S ella Ac i i y ................................................................................................. 13
In i ed Speake : Sa i a Ma hu - Magne ic Li es o Sola -like S a s: Implica ions o
Exoplane S udy ............................................................................................................. 13
Telmo Mon ei o - Analysis o NIR Ac i i y Indices o Exoplane De ec ion and
Cha ac e iza ion ............................................................................................................ 14
Eike Wol Guen he - The Fi s Spec oscopic Sc eening o Exoplane Hos S a s o
PLATO ............................................................................................................................ 15
Hala Alqubela - Acc e ion Va iabili y and Bina i y in Young S a s: Insigh s om
DQ Tau and T ansi ion Disks ....................................................................................... 16
Fa emeh Zah a Majidi - Mau e: a Th ee-yea UV-Vis Su ey Dedica ed o Moni o
S ella Ac i i y and Va iabili y ..................................................................................... 17
Sim anp ee Kau - Pola ized Radio Emission om Scallop-shell S a s: The Case o
J0508-21 and DG C n.................................................................................................... 17
Glo ia Canocchi - Challenging Na De ec ions in he A mosphe es o Gian Exoplane s
wi h 3D Non-LTE S ella Spec a ................................................................................. 18
Be am Bi sch - In oduc ion o he COST Ac ion CA22133 PLANETS .................. 19
Session 3: S ella Chemical Composi ion ......................................................................... 20
In i ed Speake : Elisa Delgado Mena - The Impac o S ella Composi ion: om
Galac ic Chemical E olu ion o Plane Fo ma ion ........................................................ 20
Edi a S onku e - Chemical Signa u es o Plane -Hos ing S a s ................................ 21
Masanobu Kuni omo - New-Gene a ion Sola and S ella Models Including
Acc e ion ......................................................................................................................... 22
Neda Hejazi - A New Me hod o Measu e he De ailed Chemical Abundances o Cool
Dwa s and I s Applica ion o S a -Plane Chemical Connec ion S udies ................... 23
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 3
Jiayue Zhang - Un eiling he Chemical Abundance Pa e n o Sola Analogues
Hos ing Deb is Disks ...................................................................................................... 24
Sandipan Bo haku - S ella Pho osphe ic Con amina ion in Ea ly-Type S a s -
om P o oplane a y o Deb is Disks.............................................................................. 24
Ve onika Mi okhina - De ec abili y o Deu e ium in he Spec a o A- ype S a s ... 25
Ka olina Szewczyk - Disk Caugh a he T ansi ion om P o oplane a y o Deb is
S age ............................................................................................................................... 26
And ea Pe domo Ga cía - Mos Plane -Hos s Ha e Sub-Sola Me allici ies, Bu
Sola o Supe -Sola I on .............................................................................................. 27
Session 4: Elemen al Abundances in Plane Fo ma ion .................................................. 28
In i ed Speake : Diego Tu ini - Gene ic Links and Composi ional Connec ions
be ween S a s, Thei Ci cums ella Disks and Thei Plane s ....................................... 28
Be am Bi sch - The Limi s o Plane esimal Fo ma ion a Low Me allici y ............ 29
Daisy Tu ne - In es iga ing S a -Plane Composi ional Ties o Sys ems wi h Hos
S a s o Va ying Composi ion ........................................................................................ 30
Giulia Riccia di - Compac o La ge? CO Obse a ions o he Fain es Plane -
Fo ming Disks ................................................................................................................ 30
Hea he Johns on - The Rise and Fall o he Gian Plane Occu ence Ra e............ 31
Jason Ran - Bayesian Cons ain s on Plane Fo ma ion Models wi h Popula ion
Syn hesis and Simula ion Based In e ence ................................................................... 32
Nidhi Rohi Bange a - Unpacking Disequilib ium Chemis y in Exoplane
A mosphe es: F om C/O Cons ain s o Sulphu Pho ochemis y ................................ 33
Anna Thomas - Popula ion Syn hesis o In es iga e he E ec o Vola ile o Re ac o y
Sulphu Con e sion on he P oduc ion o Ho and Cold Gas Gian s ............................ 34
Sébas ien Paine - Pho oe apo a ed Dus Disk Models and Syn he ic Obse a ions . 34
Luke Key e - The Chemical Composi ion o Ex e nally I adia ed Disks .................. 35
Session 5: S ella Abundances & Plane Composi ion ..................................................... 36
In i ed Speake : Va dan Adibekyan - F om S ella A mosphe es o Plane a y
In e io s .......................................................................................................................... 36
Yoshi Eschen - Chemical Finge p in s: Decoding S ella Abundance In luence on
Plane a y Composi ion ................................................................................................... 37
Ma ia Tsan aki - The Exoplane Popula ion in he Galac ic Con ex om he A iel
Mission Candida e Sample ............................................................................................ 38
Ke in Schlau man - Te es ial Exoplane In e nal S uc u e Cons ain s on Plane
Fo ma ion Enabled by Comp ehensi e Hos S a Cha ac e iza ion ............................. 39
Alexand a Leh me s - S ella Abundance Anomalies in A–F Type S a s and he Role
o Plane a y Con amina ion ........................................................................................... 40
Subsession on Disks .......................................................................................................... 41
An onio Ga u i - 300 Disks Imaged, and Coun ing… ................................................ 41
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 4
Ka ina Mauco - Cha ac e iza ion o P o oplane a y Disks Nea and Fa : a
Complemen a y Pe spec i e ........................................................................................... 41
Ma i-Liis A u - S udying he E ec o he En i onmen on Disk E olu ion wi h
MUSE ............................................................................................................................. 42
Daniel Daza Valdebeni o - Hyd odynamical Simula ions o Plane -Disk
In e ac ions in PDS 70 ................................................................................................... 43
Thi My Hanh T an - Explo a ion o he Inne Region o he Sys em HD 142527 ...... 44
Zuzanna Jonczyk - Gone wi h he Wind: CO Deple ion in Magne ically-D i en
P o oplane a y Disks ...................................................................................................... 44
Yinuo Han - High-Resolu ion ALMA Imaging o Ex asola Plane esimal Bel s ....... 45
Session 6: Fu u e Ins umen a ion ................................................................................... 47
In i ed Speake : Gio anna Tine i - A iel Space Mission ......................................... 47
In i ed Speake : Heike Raue , Juan Cab e a, and he PLATO Team - PLATO ....... 48
In i ed Speake : Ana Ines Gomez de Cas o - The Unique Capabili ies o he
Habi able Wo lds Obse a o y o he In es iga ion o he E olu ion o Young
Plane a y Sys ems .......................................................................................................... 49
In i ed Speake : Daniel Ange hausen - LIFE Looks o Li e - Cha ac e izing Rocky
Wo lds wi h he La ge In e e ome e Fo Exoplane s Concep .................................... 50
In i ed Speake : Ma ica Valen ini - The Milky Way in he 4MOST e a ................... 51
In i ed Speake : En ic Palle - P obing he C adle o Plane s: How ANDES@ELT will
Un a el he Link be ween P o oplane a y Disks and Exoplane a y Sys ems ............... 52
Pos e session .................................................................................................................... 54
Colin Folsom - Chemical T aces o Selec i e Acc e ion in he HD 135344 Bina y
Sys em ............................................................................................................................ 54
Timo hy Rawle - ESA A iel Science A chi e .............................................................. 54
Tomoyuki Kudo - Low Wa e Ice Abundance in he Disk Su ace o AB Au : Insigh s
om Pola ime ic Obse a ions ..................................................................................... 55
Alexand a Leh me s - In es ing Ci cums ella A omic Radia ion-d i en Dynamics56
Anna Ma ia Weiß - The New Exoplane TOI 1147b: a Ho Jupi e O bi ing I s
Subgian -Class S a in a Highly Ellip ical O bi ......................................................... 56
P a eek Boga - Cha ac e izing A mosphe es o Ul a Ho Jupi e s wi h he 2m
Wendels ein Telescope. ................................................................................................... 57
Ugnė Jonauskai ė - Chemical Analysis o Sola Twin and Analogue S a s ............. 58
Hele i Ramle - Ho S a s in he A iel Mission Sample: In e media e-Mass S a and
Plane Co ela ions ........................................................................................................ 59
Nicola Mille - Towa ds a Homogeneous Sample o M-dwa P ope ies and
Abundances o he PLATO Mission .............................................................................. 59
Mohamad Ali-Dib - P o oplane a y co es d o e chond ule o ma ion ....................... 60
Scien i ic O ganising Commi ee ...................................................................................... 61
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 5
Local O ganising Commi ee ............................................................................................. 61
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 6
In oduc ion
The s udy o he s a -plane -disk connec ions is c ucial o unde s anding he
o ma ion and e olu ion o plane a y sys ems, including ou own. S a s, disks, and
plane s a e no isola ed en i ies, bu a e in insically linked by hei o ma ion
p ocesses and sha ed chemical en i onmen s. By examining how hese
componen s in e ac , we can gain insigh in o he ini ial condi ions ha go e n
plane o ma ion, he e olu ion o plane a y a mosphe es, and he po en ial
habi abili y o exoplane s. In an e a o apid ad ances in exoplane de ec ion and
cha ac e iza ion, his ield is mo e ele an han e e o un eiling he di e si y
o plane a y sys ems and unde s anding he o ces ha shape hem.
The scope o he con e ence “Explo ing S a -Plane -Disk Connec ions” will span a
wide a ay o opics, including me hods o s udy s ella a mosphe es, he
challenges o s ella cha ac e iza ion in he e a o la ge-scale space missions, and
he chemical p ocesses wi hin disks ha in luence plane o ma ion and
composi ion, p o iding a holis ic iew o plane a y sys em o ma ion and
e olu ion. This imely mee ing o e s a pla o m o esea che s o sha e hei
la es indings and collabo a e on solu ions o some o he mos p essing challenges
in he ield.
This is he inal con e ence o he EXOHOST p ojec being coo dina ed by he
Ta u Obse a o y, Uni e si y o Ta u om 2023 o 2025. EXOHOST is a
Twinning p ojec wi h he main goal o build excellence in spec al
cha ac e iza ion o exoplane hos s and o he s a s a Ta u Obse a o y. Ou
pa ne s in he p ojec a e Uppsala Uni e si y, Space Resea ch Ins i u e o he
Aus ian Academy o Sciences, and Uni e si y College London. This p ojec has
ecei ed unding om he Eu opean Union’s Ho izon Eu ope esea ch and
inno a ion p og amme unde g an ag eemen No. 101079231 (EXOHOST), and
om UK Resea ch and Inno a ion (UKRI) unde he UK go e nmen ’s Ho izon
Eu ope unding gua an ee (g an numbe 10051045).
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 7
Session 1: Fundamen al S ella P ope ies
Unde s anding he key physical p ope ies o s a s — such as mass, adius, age,
and empe a u e — ha a e c ucial o in e p e ing exoplane obse a ions and
e olu ion.
In i ed Speake : Camilla Danielski - The S a Se s he S age:
Unde s anding Exoplane s Th ough Thei Hos s
(Uni e si y o Valencia, Spain)
To unde s and he na u e o exoplane s, we mus mo e beyond s udying hem in
isola ion and ins ead cha ac e ize en i e plane a y sys ems. The undamen al,
chemical and dynamical p ope ies o hos s a s se he scale o plane a y
pa ame e s and shape hei e olu ion, while he Galac ic en i onmen in which a
sys em o ms can in luence he di e si y o plane a y a chi ec u es and
a mosphe es. Ensu ing consis ency in s ella cha ac e iza ion is also c ucial, so
ha obse ed co ela ions e lec genuine as ophysical ends a he han
analysis a e ac s. In his alk, I will gi e an o e iew o hese hemes and discuss
how expanding ou a ge selec ion ac oss a wide ange o chemical and dynamical
en i onmen s— om local o e densi ies o he Galac ic halo, and ac oss di e en
s ella e olu iona y phases—will be key o unco e ing how plane s o m and
e ol e unde di e se condi ions.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 8
Alix F eckel on - The G 8s a s Ca alogue: a Public Lib a y o FGKM
Dwa Spec a and Thei Homogeneously De i ed Pa ame e s.
(Uni e si y o Bi mingham)
Ad ances in ins umen a ion and echniques a e leading us in o a new e a o
s ella and exoplane a y s udies. A homogeneous, p ecise, and accu a e sou ce o
s ella pa ame e s o b igh s a s is c ucial o many s udies, including, bu no
limi ed o, designing adial eloci y exoplane su eys, pe o ming p ecision
s ella abundance analyses, and planning u u e di ec imaging su eys. I
in oduce he G 8s a s ca alogue, which cu en ly p o ides uni o mly o ma ed
spec a and homogeneous a mosphe ic pa ame e s, de e mined using he PAWS
pipeline, o 1715 FGKM main sequence s a s in he sola neighbou hood. Ongoing
expansions o he ca alogue will ul ima ely esul in he classi ica ion o nea ly
6000 main sequence s a s wi h G < 8, u he imp o ing he use ulness o G 8s a s
in s udying s ella composi ion, hos -s a cha ac e iza ion, and e olu iona y
ends. Fu u e plans o he G 8s a s collabo a ion include he compa ison o
a mosphe ic pa ame e s de e mined by a ying spec oscopic me hods ac oss
pa ame e space, s ella ac i i y in es iga ions, and de ailed s ella abundances
s udies. In his alk I will p esen he G 8s a s ca alogue, de ail he PAWS
spec oscopic pipeline and p esen he esul ing homogeneous p ope ies o hese
b igh nea by s a s.
La a Pisca e a - Acc e ion Makes Young S a s Look Old: Lessons
om O ion
(Eu opean Sou he n Obse a o y (ESO))
The obse ed decline in p o oplane a y disk equency wi h inc easing age in
nea by s a - o ming egions implies ypical disk li e imes o a ew My , se ing
cons ain s on he imescales o plane o ma ion and disk dispe sal. Howe e , in
he O ion Nebula, some p e-main sequence (PMS) s a s exhibi ing in a ed excess
and s ong H-alpha emission (signa u es o ongoing acc e ion) appea
anomalously old (≳10 My ) in op ical colou -magni ude diag ams (CMDs).
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 9
To in es iga e his disc epancy, we conduc ed a spec oscopic analysis o PMS
s a s loca ed in he O ion Nebula using VLT/X-Shoo e . We de i ed s ella
pa ame e s (e ec i e empe a u e, ex inc ion, s ella luminosi y), acc e ion
diagnos ics (acc e ion luminosi y, mass acc e ion a e), and li hium equi alen -
wid hs ac oss a sample o 40 PMS wi h isoch onal ages spanning om ~1 o >30
My . A e accoun ing o ex inc ion and excess con inuum emission coming om
he acc e ion p ocess, we ind ha mos o he seemingly old s a s occupy posi ions
in he HR diag am consis en wi h a younge popula ion (1–5 My ). S ong li hium
abso p ion and ypical acc e ion- o-s ella luminosi y a ios u he suppo hei
you h. Mo eo e , hese seemingly old s a s ypically show some o he highes
acc e ion luminosi ies in he sample.
This s udy highligh s how acc e ion a ec s he pho ome y o PMS s a s and he
impo ance o accoun ing o his e ec o ob ain eliable age es ima es. In his
alk, I will explo e how ongoing acc e ion can shi s a s in op ical CMDs, and how
his impac s ou unde s anding o s ella ages and disk e olu ion in young
clus e s.
Ma hias Ammle - on Ei - How o Imp o e he Cha ac e iza ion o
Dis an S a s wi h T ansi ing Exoplane s?
(MPI o Sola Sys em Resea ch)
The accu a e de e mina ion o he hos s a pa ame e s is essen ial o cha ac e ize
hei o bi ing plane s. In he PLATO mission, he a ge sample consis s o s a s
wi h V <= 13 mag, many o which may be oo ain o he ull cha ac e iza ion ia
as e oseismology and g ound-based spec oscopy, as is planned o he b igh e
a ge s. Addi ionally, hese s a s end o be dis an , making in e s ella ex inc ion
a mo e signi ican ac o compa ed o o he PLATO a ge s.
To assess he limi a ions o he s ella cha ac e iza ion and o explo e possible
solu ions in p epa a ion o PLATO, we e iewed he s ella pa ame e s o all 36
CoRoT plane hos s. These a e ypically ain (V=12-16 mag) and can be as dis an
as 1 kpc and mo e.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 16
Hala Alqubela - Acc e ion Va iabili y and Bina i y in Young S a s:
Insigh s om DQ Tau and T ansi ion Disks
(Eu opean Sou he n Obse a o y (ESO))
Acc e ing bina y sys ems in e ac dynamically wi h hei ci cums ella and
ci cumbina y en i onmen s, p oducing a iabili y ac oss mul iple wa eleng hs
and imescales. Unde s anding hese a ia ions is c ucial o cons aining
acc e ion physics and disk s uc u es.
DQ Tau is a sho -pe iod (15.698 days), highly eccen ic (e = 0.6), equal-mass
bina y exhibi ing sha p acc e ion bu s s nea pe ias on. The o bi al mo ion clea s
he inne egion, enabling he o ma ion o mul iple acc e ion disks. The
ci cumbina y acc e ion s eams a e s ongly in luenced by he sys em's o bi al
pa ame e s. Using VLT/UVES and VLT/X-Shoo e , we applied he b oadening
unc ion (BF) echnique o calcula e adial eloci ies (RVs) ac oss mul iple epochs.
The BF analysis e eals wo dis inc RV signa u es, con i ming he equal-mass
componen s. O e ime, we obse e changes in BF peak heigh s ( lux a ios) ied
o o bi al phase, o e ing insigh s in o eiling on each s a .
I will p esen esul s om spec al disen angling o DQ Tau, de i ing acc e ion
a es o bo h s a s, and show how pulsed acc e ion a ec s measu ed RVs o e 10
o bi s om a ecen JWST, LCO, X-Shoo e , and UVES campaign.
DQ Tau has shaped ou unde s anding o young bina ies, bu how a can we push
bina i y s udies in a iable acc e o s? I will highligh disks wi h la ge, dus - ee
ca i ies seen in ALMA con inuum images, p oposing hey a e ca ed by s ella o
subs ella companions. I will discuss RV a ia ions obse ed wi h
ESPRESSO/VLT o e 3 yea s o 12 ansi ion disks, and he possible bina y
con igu a ions esponsible o he obse ed ca i ies. Finally, I will add ess how o
disen angle RV a ia ions caused by s ella ac i i y e sus plane a y companions.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 17
Fa emeh Zah a Majidi - Mau e: a Th ee-yea UV-Vis Su ey
Dedica ed o Moni o S ella Ac i i y and Va iabili y
(Blue Skies Space)
Mau e is a sa elli e equipped wi h a 13 cm elescope and a UV-Visible
spec ome e (wi h an ope a i e wa eleng h ange o 200-700 nm) concei ed o
measu e he s ella magne ic ac i i y and a iabili y. The science p og amme will
be deli e ed ia a mul i-yea collabo a i e su ey p og amme, wi h housands o
hou s each yea a ailable o long baseline obse a ions o hund eds o s a s,
unlocking a signi ican ime domain as onomy oppo uni y. Mau e’s mission
li e ime is 3 yea s wi h he ambi ion o 5 yea s, and i will co e a b oad ield in
he sky (–46.4 o 31.8 deg ees in ICRS) du ing his pe iod. Booked o launch in
Oc obe 2025, Mau e’s science eam will o m p io o he launch da e, de ining
he obse a ion s a egy and a ge s.
This acili y was concei ed o suppo pilo s udies and new ideas in science and
is ully dedica ed o ime-domain as onomy. The main su eys o be execu ed by
Mau e a e long baseline obse a ions o la e s a s (e up i e Wol –Raye s a s,
UV Ce i s a s, e c.), RS CVn a iables, eclipsing bina ies, He big Ae/Be s a s,
exoplane hos s, ho s a s, e c. Besides hese majo science hemes, he
spec ome e ’s da a can be u ilized o suppo and complemen exis ing and
upcoming acili ies as a pa h inde , o conduc simul aneous/ ollow-up
obse a ions.
Sim anp ee Kau - Pola ized Radio Emission om Scallop-shell
S a s: The Case o J0508-21 and DG C n
(Ins i u e o Space Sciences (ICE-CSIC), Ba celona)
Scallop-shell s a s (SSSs) o Complex Pe iodic Va iables (CPVs) a e a ecen ly
disco e ed class o young M dwa s, which show quasi-pe iodic dips in hei op ical
ligh cu es ha a e s able o e ens o hund eds o o a ion cycles. The o igin o
hese dips is no well unde s ood, howe e he mos p omising scena ios in ol e
he p esence o gas apped in huge p ominences o dus om he deb is disk o a
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 18
dis up ing ocky plane a he co- o a ion adius. The alk will ocus on he adio
obse a ions o wo o he adio loud SSSs: J0508-21 and DG CVn. J0508-21 was
obse ed a 575–720 MHz wi h he uGMRT in wo epochs o 7 hou s each. We
de ec ed ~mJy le el luxes wi h high ci cula pola iza ion, along wi h an ~hou -
long helici y e e sal in bo h epochs, happening a a simila o a ional phase. This
sugges s p esence o wo emission componen s: a pe sis en gy o-synch o on
emission and a sho -du a ion, au o al like emission, likely powe ed by he ECM
mechanism, possibly esul ing om a Jupi e -Io like in e ac ion be ween he s a
and he occul ing ma e ial. On he o he hand, DG CVn displays a weakly
pola ized, quiescen componen along wi h ~100% pola ized bu s s las ing om
minu es o o e hal an hou du ing i s 14 hou s o VLA obse a ions a 1.5 GHz.
Some o hese bu s s also show a d i in equency and ime, which could be
caused due o beaming e ec s o he mo ion o he sou ce and a e consis en wi h
plasma o ECM mechanisms. O e all, hese obse a ions e eal ha he SSSs a e
no longe cons ained o op ical obse a ions only, and how he adio obse a ions
can help e eal he unde lying p ocesses, highligh ing he need o ha e mo e
con empo aneous/simul aneous mul i-wa eleng h obse a ions o such sys ems.
Glo ia Canocchi - Challenging Na De ec ions in he A mosphe es o
Gian Exoplane s wi h 3D Non-LTE S ella Spec a
(S ockholm Uni e si y)
T ansmission spec oscopy om high- esolu ion g ound-based spec og aphs is
one o he mos powe ul echniques o cha ac e izing he a mosphe es o gian
exoplane s. P e ious s udies ha e highligh ed he impo ance o co ec ing he
ansmission spec a o he cen e - o-limb a ia ion (CLV) and he Rossi e -
McLaughlin (RM) e ec a ising as he plane ansi s he s ella disk. I no
p ope ly co ec ed, hese e ec s can indeed esemble o cancel ou plane a y
abso p ion in ce ain cases, hus a ec ing he de e mina ion o elemen al
abundances in he plane a y a mosphe es, as shown by Yan e al. (2017).
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 19
Howe e , commonly used 1D plane-pa allel LTE a mosphe e models ail o
ep oduce spa ially esol ed obse a ions o he sola disk. 3D adia ion
hyd odynamic models and non-local he modynamic equilib ium (non-LTE) line
o ma ion a e equi ed o an accu a e modelling o he CLV e ec .
Sodium is by a he mos de ec ed species in ansmission spec a, h ough he
analysis o he Na I D lines, which a e a ec ed by s ong 3D non-LTE e ec s.
In his alk, I will p esen new esul s ega ding he analysis o hese lines in
ESPRESSO da a o se e al benchma k gas gian s, by modelling hei CLV and
RM e ec using 3D non-LTE adia i e ans e . These kinds o s udies will be
undamen al in p epa a ion o he ELT in o de o be able o ully exploi i s
capabili ies in he nea u u e.
Be am Bi sch - In oduc ion o he COST Ac ion CA22133
PLANETS
(Uni e si y College Co k)
COST Ac ions a e p ojec s unded by he Eu opean Union o b ing scien is s
wo king on simila opics oge he . In pa icula he COST Ac ion CA22133
PLANETS is designed o ad ance ou unde s anding o plane o ma ion by
ocusing on di e en aspec s om labo a o y expe imen s o simula ions. The
COST Ac ion also o ganizes (online) p esen a ions and wo kshops, mee ings and
allows membe s o apply o unding o isi con e ences as well as o isi
collabo a o s. In his alk I will in oduce he scien i ic goals o he COST Ac ion
CA22133 PLANETS, how you can become a membe o he COST Ac ion, and how
you can bene i om joining.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 20
Session 3: S ella Chemical Composi ion
Cha ac e izing he elemen al abundances o s a s o unde s and hei o ma ion
his o y and he chemical en i onmen whe e plane s eme ge.
In i ed Speake : Elisa Delgado Mena - The Impac o S ella
Composi ion: om Galac ic Chemical E olu ion o Plane Fo ma ion
(CAB, Spain)
The cha ac e iza ion o sola - ype s a s is undamen al o a ious ields in
as ophysics, including exoplane de ec ion and he chemical e olu ion o ou
Galaxy. In pa icula , he de e mina ion o chemical abundances o s a s a
di e en me allici ies and ages p o ides us wi h a key insigh on how and when
he a ious chemical elemen s we e o med wi hin he Galaxy. The chemical
ends obse ed in di e en pa s o he Galaxy ( hin disk, hick disk, bulge and
halo) also se e o unde s and how hose di e en popula ions we e o med. On
he o he hand, knowing he pa icula cha ac e is ics o a gi en s a is essen ial
o be able o de ec i s hos ed plane s as well as o cha ac e ize hei mass, adius,
s uc u e and bulk in e nal composi ion. The p obabili y o inding plane s is
clea ly ela ed o he chemical makeup o he s a s and hese plane s in u n can
ha e an in luence on he s ella composi ion. In his alk I will e iew some o he
impo an ad ances in hese opics.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 21
Edi a S onku e - Chemical Signa u es o Plane -Hos ing S a s
(Ins i u e o Theo e ical Physics and As onomy, Vilnius Uni e si y)
Wi h he ecen disco e y o nume ous exoplane s, ou obse a ional s udies aim
o unde s and he ela ionship be ween s a s and hei plane s by analysing he
elemen al composi ions o s a s ha hos hese plane s. Accu a e and consis en
de e mina ions o s ella a mosphe ic pa ame e s and chemical composi ions
ac oss a ious Galac ic componen s a e essen ial o ad ancing ou unde s anding
o exoplane o ma ion and e olu ion.
To achie e his, we equi e homogeneous abundance measu emen s o a
s a is ically signi ican numbe o plane -hos ing s a s, along wi h a subs an ial
compa ison sample. Ou ollow-up p og amme employs he high- esolu ion
Vilnius Uni e si y Echelle Spec og aph a he Mole ai Obse a o y's 1.65 m
elescope o s udy hese s a s. This s a e-o - he-a spec og aph allows us o
pe o m de ailed and p ecise analyses, making i an in aluable ool o ou
esea ch.
We ha e de e mined he a mosphe ic pa ame e s, kinema ics, ages, and
abundances o elemen s such as C, N, O, Mg, Si, and neu on-cap u e elemen s.
In his p esen a ion, I will sha e ou indings om he analysis o 160 s a s wi h
plane s, highligh ing he po en ial connec ions be ween s a s and hei plane a y
companions.
Ou wo k showcases he capabili ies o he ad anced ins umen a ion a ailable in
Li huania, emphasising he signi ican con ibu ions ha can be made o he ield
o exoplane a y science using he Vilnius Uni e si y Echelle Spec og aph.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 22
Masanobu Kuni omo - New-Gene a ion Sola and S ella Models
Including Acc e ion
(Ku ume Uni e si y)
We p esen ou heo e ical models o he Sun and o he s a s, including acc e ion
p ocesses. T adi ionally, s a o ma ion and plane o ma ion ha e been s udied
independen ly. Howe e , we now know ha he i s phase o s ella e olu ion is
a ec ed by he acc e ion om p o oplane a y disks. Plane o ma ion heo y
p edic s ha he composi ion o he gas acc e ed by he s a mus ha e been
a iable: he g ow h and inwa d d i o dus in he disk leads o a "pebble wa e"
o inc eased me allici y, ollowed by a phase in which he exhaus ion o he pebbles
and he o ma ion o plane s leads o he acc e ion o me al-poo gas. Ou sola
models show ha he low-me allici y p o osola acc e ion is imp in ed on o ou
Sun's co e, which has a highe me allici y by up o 5% and consequen ly, a highe
empe a u e han p edic ed by s anda d models. Ou model wi h acc e ion
simul aneously ep oduces he obse a ions o sola neu ino luxes and he low-
me allici y su ace (Asplund e al. 2021). In addi ion o he Sun, he me al-poo
p o os ella acc e ion has a s onge impac on A- ype s a s, which ha e a hin o
no su ace con ec i e zone. We a gue ha he acc e ion is a s ong candida e o
he o igin o λ Boo s a s.
In he main sequence, dynamical ins abili y o plane a y sys ems leads o
plane (esimal) acc e ion, which inc eases he s ella su ace me allici y. Again,
he acc e ion signa u e is expec ed o be s onge in A- ype s a s. Howe e , in his
scena io, one should also pay a en ion o he e ec o adia i e le i a ion, in which
adia ion p essu e pushes hea y elemen s upwa d in he s ella in e io . F om he
compa ison be ween he models o A- ype s a s and a la ge sample o s ella
abundances om GALAH and Gaia su eys, we ound ~30 s a s ha exhibi
acc e ion signa u es. We sugges ha hese s a s would be p ime a ge s
in es iga ed in de ail by PLATO.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 23
Neda Hejazi - A New Me hod o Measu e he De ailed Chemical
Abundances o Cool Dwa s and I s Applica ion o S a -Plane
Chemical Connec ion S udies
(Uni e si y o Kansas / Uni e sidad de Ta apaca)
JWST has opened up new is as o p ecisely de e mine he chemical composi ion
o exoplane s a ound low-mass s a s. Sea ching o chemical links be ween s a s
and hei plane s hus demands abundance measu emen s o JWST plane hos s.
We p esen a new me hodology o eliably measu e he de ailed abundances o
di e en key (up o 15) elemen s in cool dwa s wi h 3100<Te <4900 K using an
in-dep h high- esolu ion spec oscopy. We de elop an au oma ic, line-by-line,
syn he ic model- i ing code, Au oSpecFi , which pe o ms a se ies o
minimiza ion p ocesses along wi h a me iculous ou ine o locally no malize he
obse ed lux, and accoun s o he complex co ela ions be ween he abundances
o di e en elemen s ia an i e a i e p ocedu e. Using he high- esolu ion
(R=45,000), NIR IGRINS spec a, we measu e he abundances o he K dwa
WASP-107 (Hejazi e al. 2023) hos ing a supe -Nep une plane and he M dwa
K2-18 (Hejazi e al. 2024) hos ing a sub-Nep une plane ; bo h plane s ha e been
a ge ed by JWST obse a ions. Using ou in e ed C/O a ios, we ace he
o ma ion loca ion o hese plane s ela i e o he ice lines wi hin he
p o oplane a y disk, and along wi h Mg/Si, we cons ain he p opo ion o ock-
o ming silica es in hei ocky co es. By measu ing he C/O a io o a young M-
ype T Tau i s a , DH Tau A, using i s IGRINS spec a, we e eal a chemical
homogenei y be ween he s a and i s supe -gas gian companion, sugges ing a
di ec and as g a i a ional collapse, a he han a slow co e acc e ion p ocess o
he o ma ion o he companion (Hejazi e al. 2025). We u he measu e he
abundances o he M dwa GJ 341 using i s IGRINS spec a, which a e hen used
o es ima e he co e mass ac ion, i on mass ac ion, and bulk mola a ios o he
o bi ing small ocky plane (also a ge ed by JWST) h ough in e io models. We
a e cu en ly measu ing he abundances o 8 ocky-plane cool dwa s and he
ele an esul s a e discussed in his p esen a ion.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 24
Jiayue Zhang - Un eiling he Chemical Abundance Pa e n o Sola
Analogues Hos ing Deb is Disks
(Tsinghua Uni e si y)
The peculia deple ion o e ac o y elemen s in he sola pho osphe e compa ed
o nea by sola wins emains a mys e y in s ella as ophysics and s a -plane
connec ion. Recen s udies sugges possible links o plane o ma ion o disk-
ela ed p ocesses. Howe e , deb is disks, ace s o plane o ma ion, ha e been
la gely unexplo ed in his con ex . We p opose he i s sys ema ic obse a ions o
he chemical abundances o 69 sola analogues wi h con i med deb is disks using
high- esolu ion spec oscopy. By compa ing hei de ailed abundance pa e ns,
especially he [X/Fe] e sus condensa ion empe a u e (Tc) slope, wi h a la ge
con ol sample o o e 17,000 sola -analogue s a s, we aim o iden i y po en ial
chemical signa u es imp in ed by disk- ela ed e olu ion. Ou esul s will p o ide
c ucial insigh s in o he o igin o he sola abundance anomaly and cons ain he
chemical e olu ion pa hways o plane a y sys ems.
Sandipan Bo haku - S ella Pho osphe ic Con amina ion in Ea ly-
Type S a s - om P o oplane a y o Deb is Disks
(OeAW Space Resea ch Ins i u e)
Young s a s acc e e ma e ial om hei p o oplane a y disks, which can
con amina e he s ella pho osphe e. This is especially no iceable in ho s a s wi h
adia i e en elopes, whe e slowe mixing in he pho osphe e p ese es hese
con amina ion signa u es o e longe imescales. The acc e ed ma e ial ca ies a
chemical imp in , pa icula ly in disks wi h gaps, whe e dus is apped a he
ou e edge while gas mo es inwa d. This esul s in he acc e ion o dus -poo
ma e ial, leading o a pho osphe ic abundance pa e n wi h deple ion o e ac o y
elemen s (e.g., Fe, Mg), while ola ile elemen s (e.g., C, O) emain unchanged.
These chemically peculia s a s a e known as lambda Boo is ype s a s. These
con amina ion signa u es in he s ella pho osphe e gi e us aluable insigh s in o
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 25
he elemen al composi ion o he inne disk since he acc e ed ma e ial comes om
his egion.
In his alk, I will p esen ou s udy o he pho osphe ic composi ion o young A-
ype s a s hos ing deb is disks, a la e s age in p o oplane a y disk e olu ion.
While deb is disks ha e low acc e ion a es ha don' signi ican ly a ec he
s ella pho osphe e, he e has been li le wo k on abundance anomalies in hese
s a s. We analysed he high- esolu ion spec a o six such s a s and iden i ied wo
ha exhibi lambda Boo is ype peculia i ies. This alk will discuss he o igins o
hese peculia i ies in hese wo s a s and compa e young deb is disk-hos ing s a s
wi h hei p o oplane a y disk-hos ing coun e pa s. Unde s anding hese
anomalies may p o ide insigh s in o simila lambda Boo is ype s a s o e 100
million yea s old, whe e acc e ion om a ci cums ella disk is no expec ed.
Ve onika Mi okhina - De ec abili y o Deu e ium in he Spec a o
A- ype S a s
(Ta u Obse a o y, Uni e si y o Ta u)
Deu e ium (D) was p ima ily p oduced du ing Big Bang Nucleosyn hesis, wi h a
p imo dial abundance o [D/H] = (2.58 ± 0.13) × 10⁻⁵ (Cybu e al. 2016).
Deu e ium is easily des oyed in s ella in e io s h ough as a ion (Eps ein e al.
1976) making i s de ec ion in s ella a mosphe es unlikely unless ex e nal
p ocesses, such as plane a y engul men , empo a ily enhance su ace
abundances. A- ype s a s, wi h adia i e en elopes, p o ide a a ou able
en i onmen o he su i al o acc e ed deu e ium.
In his s udy, we explo e he de ec abili y o deu e ium in A- ype s a s, which
possess adia i e en elopes ha can delay he mixing and des uc ion o acc e ed
ma e ial. We gene a ed syn he ic spec a o s a s wi h e ec i e empe a u es
be ween 7500 and 12500 K and a su ace g a i y o log g = 4.0 using he ZEEMAN
spec um syn hesis code and a g id o ATLAS9 model a mosphe es. The linelis
was modi ied by manually inse ing he deu e ium lines, ocusing on he op ical
wa eleng h egion.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 32
Jason Ran - Bayesian Cons ain s on Plane Fo ma ion Models wi h
Popula ion Syn hesis and Simula ion Based In e ence
(Uni e si y College London)
The disco e y o housands o exoplane s has enabled ex ensi e s a is ical
analyses o exoplane demog aphics. Fu he , ad ancemen s in spa ially esol ed,
mul i-wa eleng h obse a ions o p o oplane a y disks ha e e ealed ich de ails
abou he dynamics, s uc u e, and chemis y o plane - o ming en i onmen s.
La ge-scale ca alogues o such disk obse a ions, combined wi h hos s a
in o ma ion, ha e opened new pa hways o demog aphic s udies ha a e c i ical
o he de elopmen o sel -consis en plane o ma ion heo ies.
One powe ul app oach o b idging disk and exoplane demog aphics is exoplane
popula ion syn hesis, which p o ides a amewo k o es ing plane o ma ion
models. Howe e , e en he simples such models a e highly nonlinea , in ol ing
complex, high-dimensional pa ame e spaces ha a e ypically add essed using
nume ical simula ions. This complexi y in oduces signi ican challenges in
cons aining model pa ame e s and compa ing compe ing o ma ion heo ies due
o po en ial degene acies.
In his alk, I will in oduce a no el Bayesian me hod o cons aining plane
o ma ion pa ame e s using no malizing lows and simula ion-based in e ence.
This machine lea ning echnique models he p obabili y densi y o plane
o ma ion ou comes condi ioned on o ma ion pa ame e s. By le e aging his
p obabilis ic app oach, we can obus ly quan i y unce ain ies, disen angle model
degene acies, and enable p incipled compa isons be ween compe ing heo ies in a
na u al Bayesian amewo k.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 33
Nidhi Rohi Bange a - Unpacking Disequilib ium Chemis y in
Exoplane A mosphe es: F om C/O Cons ain s o Sulphu
Pho ochemis y
(Ins i u ü Wel aum o schung)
The in e p e a ion o exoplane a y spec a is o en complica ed by a mosphe ic
disequilib ium p ocesses ha al e he expec ed chemical concen a ions. 1D
kine ic-pho ochemical models o e a amewo k o quan i y hese e ec s and o
cons ain elemen al a ios, such as he ca bon- o-oxygen (C/O) a io, which a e
belie ed o se e as ace s o plane o ma ion his o ies.
We apply such a 1D model o he a mosphe e o WASP-69b, explo ing a ia ions
in C/O, e ical eddy di usion s eng h (Kzz), and gas empe a u e. The esul ing
pa ame e space explo a ion e eals s ong degene acies among hese
pa ame e s, wi h mul iple combina ions p oducing equally iable i s o high-
esolu ion spec al da a. This analysis highligh s he sensi i i y o e ie ed
a mosphe ic p ope ies o p io assump ions and model con igu a ions. Ano he
key esul indica es ha he concen a ions o pho ochemically p oduced species
(e.g. C2H2 and HCN) a e in e sely ela ed o he s eng h o e ical mixing,
sugges ing a po en ial diagnos ic o cons aining Kzz.
The chemical ne wo k used in he model is u he ex ended o include sulphu -
ion species, allowing o a mo e comple e ea men o sulphu pho ochemis y
unde a ious a mosphe ic condi ions. Wi h his we aim o assess he sulphu - o-
ni ogen (S/N) a io as a complemen a y ace o plane a y o ma ion his o ies,
pa icula ly in scena ios wi h en iched me allici y and non-sola elemen al
abundances.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 34
Anna Thomas - Popula ion Syn hesis o In es iga e he E ec o
Vola ile o Re ac o y Sulphu Con e sion on he P oduc ion o Ho and
Cold Gas Gian s
(Uni e si y College London)
Plane popula ion syn hesis is an in eg al use ul ool o linking he cu en ly
obse ed exoplane popula ion o o ma ion en i onmen s (p o oplane a y disks).
We p esen he i s indi idual plane g ow h acks and example plane
popula ions om he code. Fu he mo e, we explo e hei composi ion. Mos
s udies a emp ing o link gian plane composi ion o hei o ma ion his o y ha e
ocussed on he ca bon- o-oxygen a io (C/O) in gas o solids. Sulphu has always
been assumed o be 100% e ac o y in such models, hus making i s abundance a
ace o acc e ed ocky solids. Howe e , sulphu also has a ola ile ese oi ha
is known o be dominan a he onse o s a and plane o ma ion. We ha e applied
a no el gas-g ain con e sion o sulphu o s udy how he o ma ion ajec o ies o
gian plane s ela e o he inal composi ion o hei co es and gas en elopes.
Sébas ien Paine - Pho oe apo a ed Dus Disk Models and Syn he ic
Obse a ions
(Queen Ma y Uni e si y o London)
The en i onmen in which ci cums ella disks e ol e plays a c ucial ole in hei
e olu ion and he o ma ion o plane s. In s ella clus e s, nea by la ge s a s will
i adia e gas and dus : hea ing he disk and en aining plane - o ming solids. An
impo an , bu unde -s udied aspec o his is wha sizes o dus ge en ained in
he disk wind. This a ec s he amoun and posi ion o plane - o ming solids, as
well as dus shielding he disk om UV adia ion. We ha e de eloped a pa icle
sol e o ack he en ainmen o dus in mul i-dimensional simula ions o pho o-
e apo a ing disks. Dus en ainmen a ies signi ican ly depending on whe e om
he disk su ace he dus is launched in o he wind: om sub-mic on abo e he
disk up o 100 µm nea he disk ou e edge. Howe e , we also ind ha he dus
opaci y is mos ly uni o m om all di ec ions. This has implica ions o he
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 35
s uc u e o gas mass loss and obse a ional cha ac e is ics o p oplyds. He e, we
p esen syn he ic images and SEDs o hese e apo a ed disk models a a ious
wa eleng hs, including op ical, IR and mm and discuss wha can be lea ned om
hem.
Luke Key e - The Chemical Composi ion o Ex e nally I adia ed
Disks
(Queen Ma y Uni e si y o London)
Mos s a s o m wi hin dense clus e s, whe e p o oplane a y disks a e exposed o
in ense ul a iole adia ion om nea by massi e s a s. Despi e he p e alence o
hese en i onmen s, ou unde s anding o how such adia ion in luences disk
composi ion emains su p isingly limi ed. In his alk, I will sha e ecen insigh s
in o how ex e nal UV i adia ion a ec s disk chemis y and shapes plane
o ma ion pa hways. Ou s udies unco e complex e ec s ha challenge
con en ional models. Al hough UV adia ion is quickly a enua ed nea he disk
su ace, ep ocessed adia ion can pene a e deepe , al e ing empe a u e p o iles
and changing ola ile abundances. Pho oe apo a i e winds induced by ex e nal
UV adia ion can signi ican ly enhance molecula emission, p oducing
obse a ional signa u es ha could be mis akenly in e p e ed as e idence o
al e ed disk chemis y. I will con ex ualize hese indings wi h espec o ecen
ALMA and JWST obse a ions, and discuss hei implica ions o in e p e ing
chemical in en o ies ac oss di e se s a - o ming egions — om isola ed disks o
dense clus e s whe e mos plane a y sys ems o igina e.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 36
Session 5: S ella Abundances & Plane Composi ion
Connec ing s ella elemen al abundances o he composi ion o exoplane s.
In i ed Speake : Va dan Adibekyan - F om S ella A mosphe es o
Plane a y In e io s
(IA, Po ugal)
S a s and plane s eme ge oge he om he same p imo dial ma e ial, shaping
and eshaping one ano he h ough a a ie y o in e connec ed p ocesses. S ella
adia ion go e ns he e olu ion o p o oplane a y disks and he eby plane
o ma ion, while, con e sely, p ocesses such as plane engul men can lea e
measu able chemical inge p in s on s ella a mosphe es. Because p o oplane a y
disks dissipa e wi hin jus a ew million yea s—well be o e mos plane s can be
de ec ed—s ella a mosphe es p o ide he only long-li ed eco d o he disk’s
o iginal chemis y. In his alk, I will e iew he composi ional link be ween s a s
and plane s, emphasizing how s ella abundances in o m ou unde s anding o
plane a y o ma ion, sys em a chi ec u e, and in e io chemis y.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 37
Yoshi Eschen - Chemical Finge p in s: Decoding S ella Abundance
In luence on Plane a y Composi ion
(Uni e si y o Wa wick)
Plane s and s a s o m om he same p o o-s ella ma e ial. Hence he s ella
e ac o y elemen al abundances a e assumed o be s ongly linked o ocky plane
in e io s. This is also ound o he e ac o y elemen al abundances o he Sun
and Ea h. Fo exoplane s, his composi ional link has been ecen ly sugges ed
and explo ed in small demog aphic s udies. Howe e , he sample o ocky plane s
a ound me al-poo , alpha-enhanced s a s is limi ed. This makes i challenging o
ind and alida e po en ially i al chemical ends. We p esen a no el machine
lea ning app oach o iden i y plane hos ing s a s o in e es o ill in he lack o
well-cha ac e ised small plane s a ound me al-poo s a s. This algo i hm
le e ages s ella abundances om he la ge s ella su eys o APOGEE and
GALAH o classi y hos s a s chemically. We hen sea ched o plane s a ound
hese golden a ge s.
We p esen newly cha ac e ized sys ems con aining supe -Ea hs and sub-
Nep unes a ound me al-poo , alpha-enhanced s a s o he hick disk. These
plane a y sys ems we e obse ed wi h ansi pho ome y and adial eloci y
allowing us o measu e hei adius and masses p ecisely. We used ou ob ained
plane p ope ies o model hei in e io s uc u es using specialized ools which
ou pu he co e and man le mass ac ions. These gi e insigh s in o he elemen al
abundance a ios o he plane s. Hence, we di ec ly s udy he connec ion be ween
he plane and hos s a abundances.
These new disco e ies signi ican ly add o he sample o ocky plane s a ound
hick disk s a s and will be ollowed by u he de ec ions and cha ac e iza ions
om ou machine lea ning algo i hm. Placing ou new and upcoming sys ems in
demog aphic con ex , we a e now able o u he explo e he link be ween s ella
e ac o y elemen al abundances and hei impac on small plane s in a la ge and
mo e di e se sample. This enables insigh s in o plane o ma ion ac oss he
Galaxy.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 38
Ma ia Tsan aki - The Exoplane Popula ion in he Galac ic Con ex
om he A iel Mission Candida e Sample
(Osse a o io As o isico di A ce i - INAF)
S ella popula ions di e signi ican ly ac oss he Galaxy in e ms o chemis y,
kinema ics, and age, which is likely o a ec plane demog aphics. Ou
neighbou hood is occupied by young, me al- ich s a s loca ed in he hin disk,
whe eas he halo and hick disk hos olde and me al-poo s a s. In his alk, I will
p esen ou esul s on he ole o he Galac ic en i onmen in shaping plane a y
sys ems based on he candida e sample om he A iel space mission in
collabo a ion wi h he A iel s ella cha ac e iza ion wo king g oup.
We i s de i ed p ecise s ella pa ame e s om high- esolu ion spec a and
homogeneous s ella masses om isoch one i ing o 358 plane hos s. We hen
in es iga ed he connec ion o plane a y p ope ies wi h he di e en Galac ic disk
popula ions. In pa icula , we ind ha gian plane s a e mo e equen a ound
mo e me al- ich s a s ha belong o he Galac ic hin disk, while lowe -mass
plane s a e ound in mo e me al-poo en i onmen s and a e mo e equen in he
hick disk, hus o bi ing olde s a s.
Addi ionally, ou analysis e eals a close ela ionship be ween s ella mass and
gian plane adius, wi h mo e in la ed plane s a lowe me allici ies. We also
in es iga e he co ela ions be ween s ella and plane a y masses and plane
mul iplici y. Ou esul s highligh he impo ance o Galac ic chemical e olu ion,
al hough o en o e looked, on he cu en dis ibu ion o plane popula ions.
Unde s anding plane o ma ion ac oss he Galaxy can shed ligh on he
habi abili y in he Galac ic con ex .
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 39
Ke in Schlau man - Te es ial Exoplane In e nal S uc u e
Cons ain s on Plane Fo ma ion Enabled by Comp ehensi e Hos S a
Cha ac e iza ion
(Johns Hopkins Uni e si y)
Exoplane mass and adius in e ences undamen ally ely on hos s a mass and
adius in e ences. Despi e he impo ance o hos s a mass, adius, and elemen al
abundance in e ences o he de i a ion o exoplane in e nal s uc u e
cons ain s, published cons ain s ha e o en been based on in e ences ha a e
no sel -consis en . Fo 24 dwa s a s hos ing e es ial exoplane s, we use
as ome ic and pho ome ic da a plus high- esolu ion spec oscopy o in e
accu a e, p ecise, homogeneous, and physically sel -consis en pho osphe ic and
undamen al s ella pa ame e s as well as elemen al abundances. We in e
upda ed plane a y masses and adii using hese da a plus Dopple and ansi
obse ables, hen use he comple e da a se o de i e cons ain s on he co e-mass
ac ions o hese e es ial exoplane s. We ind ha he popula ion o esonan
o plausibly esonan e es ial exoplane s ep esen ed by Keple -36 b and
Keple -105 c has a signi ican ly lowe mean co e-mass ac ion han he es o he
e es ial exoplane s in ou sample. Thei esonan con igu a ions sugges ha
hey mig a ed inwa ds om mo e dis an o ma ion loca ions, and we a ibu e
hei low densi ies o he inco po a ion and e en ion o signi ican amoun s o
wa e du ing hei o ma ion. We con i m ha he ul a-sho -pe iod exoplane s
55 Cnc e and WASP-47 e ha e densi ies inconsis en wi h pu e ock composi ions.
We p opose ha hey a e bo h he s ipped co es o mini-Nep unes and associa e
hei low densi ies wi h he p esence o signi ican amoun s o hyd ogen, helium,
wa e , and/o o he ola iles in hei in e io s. Con a y o p e ious s udies, we
ind no e idence o a signi ican popula ion o dense, supe -Me cu y ype plane s.
Likewise, we ail o eco e he ecen ly iden i ied ela ionship be ween hos s a
age and e es ial plane co e-mass ac ion. We show ha he la e ela ionship
is a consequence o obse a ional biases.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 40
Alexand a Leh me s - S ella Abundance Anomalies in A–F Type
S a s and he Role o Plane a y Con amina ion
(Ta u Obse a o y, Uni e si y o Ta u)
Close-in gian exoplane s a ound A–F ype s a s a e subjec o in ense s ella
i adia ion, leading o a mosphe ic e apo a ion and possible mass ans e
owa ds he hos s a . I a ac ion o his plane a y ma e ial is acc e ed, i could
modi y he s ella pho osphe ic composi ion, p oducing sub le abundance o
anomalies indica i e o s ella con amina ion. This mechanism was p oposed by
Je myn & Kama (2018) as a po en ial indi ec pa hway o p obing exoplane a y
a mosphe ic composi ion.
In his p elimina y s udy, we in es iga e whe he such con amina ion could
con ibu e o he obse ed chemical peculia i ies in A–F ype s a s hos ing close-
in gas gian s. We a e cu en ly iden i ying sui able sys ems and compiling s ella
abundance da a om li e a u e and spec oscopic ca alogues. The s ella sample
will be di ided in o wo g oups based on es ima ed ex eme-ul a iole (EUV) lux:
s a s wi h s ong EUV adia ion, whe e con amina ion is expec ed o be
supp essed due o e icien ionisa ion and dispe sal o plane a y ma e ial, and
s a s wi h weake EUV lux, whe e acc e ion may be mo e likely.
A e e ence “ze o-line” will be cons uc ed o ep esen baseline s ella
abundances, allowing compa ison wi h sys ems showing po en ial con amina ion
signa u es. The goal is o de e mine whe he abundance de ia ions co ela e wi h
condi ions a o able o plane a y ma e ial acc e ion, p o iding popula ion-le el
cons ain s on how o en and unde wha ci cums ances s ella pho osphe ic
con amina ion may occu .
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 41
Subsession on Disks
An onio Ga u i - 300 Disks Imaged, and Coun ing…
(INAF, Is i u o di Radioas onomia, Bologna)
The ex ensi e sample o high- esolu ion images om nea -IR high-con as
ins umen s and ALMA has now eached a le el o ma u i y ha allows o
comp ehensi e demog aphic s udies o plane - o ming disks. I p esen he cu en
s a e o disk e olu ion cha ac e iza ion, examining how a ious s ella and
en i onmen al ac o s in luence his p ocess based on a da ase o o e 300 disks
obse ed o e he pas decade.
Ka ina Mauco - Cha ac e iza ion o P o oplane a y Disks Nea and
Fa : a Complemen a y Pe spec i e
(Eu opean Sou he n Obse a o y (ESO))
Gi en he a ie y o p ope ies ound in plane a y sys ems in ou Galaxy, o
unde s and disk e olu ion and plane o ma ion, we mus analyse gene al disk
and hos s a p ope ies measu ed in a la ge s a is ical sample o sys ems a
di e en e olu iona y s ages and en i onmen s. Disks in nea by egions, wi hou
he p esence o massi e s a s, e ol e di e en ly han disks in highly i adia ed
en i onmen s, whe e he a -UV adia ion ields om OB- ype s a s dispe se he
closes p o oplane a y disks om he ou side in. Since he majo i y o (exo)plane
hos s a s (including ou Sola Sys em) o m in dense and massi e s ella clus e s
in which he p esence o OB- ype s a s domina es he adia ion ield, disk
e olu ion s udies mus conside in e nal as well as ex e nal ac o s shaping he
e olu iona y pa h o p o oplane a y disks in a complemen a y way.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 48
In i ed Speake : Heike Raue , Juan Cab e a, and he PLATO Team
- PLATO
(DLR, Ge many)
PLATO, he 3 d Medium class ESA’s mission, is being buil o de ec and
cha ac e ize ex asola plane s by pho ome ically moni o ing a la ge numbe o
s a s. PLATO will de ec small plane s a ound b igh s a s, including e es ial
plane s in he habi able zone o Sun-like s a s. PLATO will also s udy he (hos )
s a s using as e oseismology, allowing us o de e mine he s ella p ope ies wi h
high accu acy ( adius, mass, age), subs an ially enhancing ou knowledge o
s ella s uc u e and e olu ion. Radial eloci y obse a ions om g ound will
allow cha ac e izing plane s o hei adius and mass (hence densi y), and age
wi h high accu acy. The mission will p o ide a ca alogue o well-cha ac e ized
exoplane s up o in e media e o bi al pe iods, ele an o a meaning ul
compa ison o plane o ma ion heo ies and o be e unde s and plane
e olu ion. In addi ion, PLATO´s Gues Obse e p og amme will allow o a la ge
numbe o complemen a y science cases, based on p oposals om he communi y.
PLATO is scheduled o a launch da e a he end 2026 on an A iane 6 ocke . The
payload ins umen consis s o 26 came as wi h 12 cm ape u e each. Fo a leas
ou yea s, he mission will pe o m high-p ecision pho ome ic measu emen s o
abou 150,000 s a s pe ield, wi h 2 long poin ings o eseen.
The payload and he spacec a ha e ecen ly a i ed in a clean oom in he ESA
acili ies in he Ne he lands o u he es ing. In his alk we will p esen he
cu en s a us o he mission and e iew he expec ed science pe o mance o he
p ojec , esul ing in he key scien i ic esul s ha can be achie ed by he mission.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 49
In i ed Speake : Ana Ines Gomez de Cas o - The Unique
Capabili ies o he Habi able Wo lds Obse a o y o he In es iga ion
o he E olu ion o Young Plane a y Sys ems
(UCM, Spain)
The Habi able Wo lds Obse a o y (HWO) is he nex NASA lagship mission.
This la ge elescope will be equipped wi h ins umen a ion o image and analyse
he adia ion om Ea h-like plane s o bi ing nea by s a s. In his alk, I will
p esen a sho summa y o he cu en s a us o he mission and he Eu opean
pa icipa ion in i . I will also p esen he cu en s a us o ou unde s anding o
he s a -disk in e ac ion du ing he e olu ion o young plane a y disks and he
con ibu ion o u u e HWO ins umen a ion o he s udy o his p ocess.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 50
In i ed Speake : Daniel Ange hausen - LIFE Looks o Li e -
Cha ac e izing Rocky Wo lds wi h he La ge In e e ome e Fo
Exoplane s Concep
(ETH Zü ich, Swi ze land)
The de ec ion and a mosphe ic cha ac e iza ion o a signi ican numbe o
empe a e and ocky exoplane s, including he sea ch o habi able and po en ially
inhabi ed plane s, is a guably he majo goal o exoplane a y science and one o
he mos challenging ques ions in 21s cen u y as ophysics. In his con ibu ion
we p esen an upda e on he LIFE (La ge In e e ome e Fo Exoplane s) mission,
which add esses his challenge by in es iga ing he scien i ic po en ial and
echnological iabili y o an ambi ious mission employing a o ma ion- lying
nulling in e e ome e in space wo king a mid-in a ed wa eleng hs. LIFE, in
syne gy wi h o he planned u u e missions, will o he i s ime in human
his o y enable us o conduc s udies in “Compa a i e Exobiology” – unde s anding
li e and habi abili y in he con ex o he di e si y o plane a y sys ems ha migh
hos i . P og ess in ou unde s anding o he exoplane popula ion as well as
signi ican b eak h oughs in ele an echnologies jus i y he need, bu also he
easibili y o u u e li e de ec ing missions o in es iga e some o he mos
undamen al ques ions o humankind. LIFE di ec ly engages wi h he scien i ic
heme o iden i ying and cha ac e izing empe a e exoplane s in he mid-in a ed
(MIR), a opic acco ded 'highes scien i ic p io i y' by ESA’s Voyage 2050 Senio
Commi ee epo as a po en ial ocus o a u u e L-class mission wi hin he ESA
Science P og amme. We will p esen he unique disco e y space o a mid-in a ed
mission, in pa icula o he de ec ion o a mosphe ic biosigna u es in exoplane s
and summa ize addi ional ele an LIFE ela ed wo k. We will discuss he
in e na ional scope o he ini ia i e (including con ibu ions om he US, Japan
and Aus alia) and will highligh syne gies be ween LIFE and NASA's u u e
Habi able Wo lds Obse a o y mission.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 51
In i ed Speake : Ma ica Valen ini - The Milky Way in he 4MOST
e a
(AIP, Ge many)
4MOST is a new su ey acili y ha will be a ailable a he ESO's 4m-VISTA
elescope a Pa anal, Chile. 4MOST uniquely combines a la ge ield o iew (4.4
squa e deg ees) wi h a high mul iplex ib e posi ione . O he 2436 ib es a ailable
o science, 1624 ib es will eed wo low- esolu ion op ical spec og aphs (R = λ/Δλ
~ 6500) while 812 ib es will eed he high- esolu ion op ical spec og aph (R ~
20,000). A he end o Oc obe 2025, he i s scien i ic ligh is planned, and his
means ha he c ucial scien i ic e i ica ion phase will s a soon a e , wi h he
i s da a and esul s om 4MOST da a o eseen o mid-2026.
I will gi e an o e iew o he s a us o he ins umen and o he planned galac ic
science p ojec s ha will be pu sued h ough he Conso ium and he Communi y
p og ams ha cons i u es he unique ope a ional scheme implemen ed by
4MOST.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 52
In i ed Speake : En ic Palle - P obing he C adle o Plane s: How
ANDES@ELT will Un a el he Link be ween P o oplane a y Disks and
Exoplane a y Sys ems
(IAC, Spain)
The chemical and dynamical p ope ies o p o oplane a y disks se he ini ial
condi ions o plane o ma ion and ul ima ely dic a e he di e si y o obse ed
exoplane s. Howe e , a c i ical gap emains in ou unde s anding o he inne disk
egions (<20 au), whe e he majo i y o plane s a e belie ed o o m.
Cha ac e izing he gas p ope ies, acc e ion p ocesses, and angula momen um
ex ac ion mechanisms in his un esol ed egion is essen ial o connec ing disk
e olu ion o he inal a chi ec u es and a mosphe ic composi ions o plane a y
sys ems.
The ANDES spec og aph on he Ex emely La ge Telescope (ELT) will be a
ans o ma i e ins umen o his ield. I s unique combina ion o high spec al
esolu ion (R ~ 100,000) and high spa ial esolu ion ( ia an AO-assis ed In eg al
Field Uni ) will allow us o spa ially and spec ally esol e he inne egions o
nea by p o oplane a y disks. ANDES will di ec ly p obe he physics o disk winds
and je s— he p ima y mechanisms o disk dispe sal and angula momen um
anspo —by measu ing kinema ics in key o bidden lines like [O I] 630 nm and
[Fe II] 1.64 µm. Fu he mo e, i s possible ex ension o co e he K-band (cu en ly
a goal) would enable s udies o molecula winds (e.g., H₂ a 2.12 µm) and ho
molecula gas (e.g., CO o ib a ional bands), p o iding a comple e pic u e o he
disk's he mochemical s uc u e.
This de ailed cha ac e iza ion o he ini ial condi ions will be di ec ly linked o
ANDES's g oundb eaking s udies o he exoplane popula ions hese disks
p oduce. The ins umen will conduc a mosphe ic econnaissance o e e y hing
om young, acc e ing gian plane s o he a mosphe es o e es ial plane s in
he habi able zones o M-dwa s. By measu ing a mosphe ic composi ions,
dynamics, and iso opic a ios, ANDES will p o ide he empi ical da a needed o
es plane o ma ion and mig a ion models.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 53
In his alk, I will p esen he capabili ies o ANDES and demons a e how i s
obse a ions o disks, plane s, and hei hos s a s will p o ide an unp eceden ed,
holis ic iew o he li e cycle o plane a y sys ems. Ope a ing in syne gy wi h
con empo aneous acili ies like JWST, ALMA, and A iel, ANDES will
undamen ally ad ance ou unde s anding o he in ica e ela ionships be ween
s a s, hei disks, and he plane s hey nu u e.
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 54
Pos e session
Colin Folsom - Chemical T aces o Selec i e Acc e ion in he HD
135344 Bina y Sys em
(Ta u Obse a o y, Uni e si y o Ta u)
The chemical inge p in s o ecen acc e ion can be ound in spec a o some A-
and B- ype s a s. These s a s ha e adia i e a mosphe es, whe e mixing is slow,
and hus can build up a laye o ecen ly acc e ed ma e ial a hei su ace. When
he e is a dus ap in he disk a ound a s a , such as a gap in he disk due o
plane o ma ion, his can lead o an inne disk deple ed in e ac o y elemen s.
This e ac o y deple ion can hen be de ec able in he su ace chemical
abundances o he s a . The HD 135344 bina y sys em, wi h an A- ype p ima y
and an F- ype seconda y, is a pa icula ly in e es ing case. The p ima y displays
a clea e ac o y deple ion, while he seconda y is chemically no mal. In he
p ima y, acc e ion has hal ed and he cu en deple ions appea o be a elic o
ea lie acc e ion. In he seconda y, acc e ion is ongoing, al hough he s a has a
signi ican amoun o su ace con ec ion, po en ially washing ou any aces o
acc e ed abundances. In o de o mo e ully cha ac e ize ou unce ain ies, and
hus unde s and he di e ences be ween hese s a s, we used a no el MCMC
based app oach o de i ing chemical abundances om obse ed spec a.
Timo hy Rawle - ESA A iel Science A chi e
(Eu opean Space Agency)
ESA's A iel (A mosphe ic Remo e-sensing In a ed Exoplane La ge su ey) aims
o cha ac e ize he a mosphe es o mo e han 500 di e se exoplane s du ing a 3.5-
yea mission launching in 2029. A combina ion o op ical- o-mid-in a ed
spec oscopic and pho ome ic ime se ies, co e ing ansi s, eclipses and, in some
cases, en i e o bi al phase cu es, will enable analysis o he a mosphe ic
s uc u e, elemen al composi ion and a ia ion, including cloud p ope ies and
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 55
dis ibu ion, as well as u he in es iga ion in o he impac o s ella hos ac i i y.
The ESA A iel Science A chi e, hos ed by he ESAC Science Da a Cen e (ESDC)
nea Mad id in Spain, will se e he b oad communi y wi h all le els o scien i ic
p oduc gene a ed a he ESA Science Ope a ions Cen e using he o icial A iel
Mission Conso ium da a p ocessing pipeline. In his p esen a ion, we in oduce
he concep o he A iel A chi e and solici communi y inpu o ensu e i mee s
he demands o mode n Eu opean esea ch in o exoplane a y sys ems.
Tomoyuki Kudo - Low Wa e Ice Abundance in he Disk Su ace o
AB Au : Insigh s om Pola ime ic Obse a ions
(Suba u elescope / Na ional As onomical Obse a o y o Japan)
Wa e (H2O) ice g ains play an impo an ole in plane o ma ion and ela ed
ma e s. The e o e, e ealing wa e ice dis ibu ion wi hin a p o oplane a y disk
is a c i ical wo k o unde s anding plane o ma ion. Pola ime ic obse a ions
a e a powe ul echnique o acing sca e ed ligh om dus g ains a he disk
su ace. We deployed he mal in a ed (TIR) pola iza ion capabili ies on he
exis ing IRCS+AO a he Suba u Telescope, Hawaii. Wa e ice has a s ong
spec al ea u e a a wa eleng h o 3 μm. A compa ison o high- esolu ion
pola ized images ob ained a 3 μm and i s adjacen wa eleng hs allows us o p obe
he p esence o H2O ice g ains in disks. We ca ied ou pola iza ion imaging
obse a ions o AB Au in he K, H2O ice and L'-bands. The disk s uc u e has
been clea ly de ec ed in all bands. Compa ed o he adia i e ans e models, ou
esul s a e consis en wi h a wa e -ice mass ac ion less han ∼ 5%. We canno
ule ou he p esence o ice- ich g ains in he disk su ace i a ca bonaceous
ma e ial exis s as a highly abso p i e o m. Howe e , i he ice-poo scena io is
he case, he in e ed wa e -ice abundance is lowe han wha has been ound in
o he s udies, such as disk obse a ions and sola sys em obse a ions, sugges ing
an e icien emo al o wa e ice om he nea -in a ed sca e ing su ace. Adding
pola ized imaging da a in he J-, H-, and Ks-bands om Suba u/HiCIAO, we also
ound ha he pola ized disk-sca e ed ligh colou is be e explained by po ous
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 56
g ains han non-po ous g ains. In his pos e , we epo de ailed esul s on he
p esence o H2O ice and he dus p ope ies in he disk su ace a ound AB Au .
Alexand a Leh me s - In es ing Ci cums ella A omic Radia ion-
d i en Dynamics
(Ta u Obse a o y, Uni e si y o Ta u)
In ou s udy, we in es iga e how ea ly- ype s a s in luence he gases escaping
om exoplane a mosphe es in o space. We ocus on wo key aspec s: how he
s a 's adia ion o ce and g a i y a ec he pa h o hese gases, and how as
neu al a oms speed up be o e changing in o ions. By combining heo ies and
models, we aim o unde s and hese p ocesses be e . Ou esea ch no only
deepens ou unde s anding o exoplane s bu also sheds ligh on hei ela ionship
wi h he s a s hey o bi . Addi ionally, ou models could help p edic which
chemical elemen s end up acc e ing on o he hos s a . Fo ea ly- ype s a s, ou
p edic ions migh e en show up as obse able pa e ns in hei spec a, because
one o he unique ea u es o ea ly- ype s a s is ha ma e ial acc e ing on o hem
can easily “pollu e” he pho osphe e.
Anna Ma ia Weiß - The New Exoplane TOI 1147b: a Ho Jupi e
O bi ing I s Subgian -Class S a in a Highly Ellip ical O bi
(Leibniz-Ins i u e o As ophysics Po sdam)
This s udy aims o iden i y and cha ac e ize a no el ex asola plane a y sys em.
To achie e his, pe iodic ansi e en s we e analysed wi hin he ligh cu es
ob ained om he T ansi ing Exoplane Su ey Sa elli e (TESS). To de e mine
he na u e o he ansi ing objec , i s mass was es ima ed using adial eloci y
measu emen s.
TOI 1147 was subsequen ly obse ed u ilizing he STELLA Échelle Spec og aph
a he Izaña Obse a o y, Tene i e. The ligh cu es o TOI 1147 exhibi a pe iodic
dimming e en occu ing e e y 10.9 days. O e app oxima ely 280 days o
Explo ing S a -Plane -Disk Connec ions con e ence, 14-17 Oc obe 2025
Page | 57
obse a ional da a, he same pe iodici y de ec ed in TESS da a was con i med.
These measu emen s acili a ed he de e mina ion o he sys em’s a chi ec u e
and he assessmen o addi ional plane a y bodies. The newly disco e ed
exoplane , TOI 1147b, has a de i ed mass o 1.3 𝑀𝐽 and a adius o 2.3 𝑅𝐽,
classi ying i as a ""pu y"" exoplane . Mo eo e , i s o bi is highly ellip ical, wi h
an eccen ici y o 𝑒 = 0.64. Spec oscopic analysis using STELLA Échelle
Spec og aph p o ided insigh s in o he hos s a , pa icula ly h ough he
e alua ion o he H𝛼-Index. The esul s indica e ha TOI 1147 is a Sun-like, low-
ac i i y s a unde going s ella e olu ion. Addi ionally, adial eloci y da a
e ealed he p esence o a hi d, long-pe iod companion in he sys em, which was
no de ec ed ia ansi obse a ions. This objec also exhibi s a high eccen ici y,
wa an ing u he in es iga ion. These indings con ibu e o he b oade
unde s anding o plane a y sys em di e si y and o ma ion mechanisms. The
ongoing obse a ional campaign a he Izaña Obse a o y aims o e ine he
o bi al and physical pa ame e s o he sys em h ough addi ional spec oscopic
da a collec ion. Fu u e s udies will ocus on cha ac e izing he long-pe iod
companion and i s dynamical in luence on he plane a y sys em.
P a eek Boga - Cha ac e izing A mosphe es o Ul a Ho Jupi e s
wi h he 2m Wendels ein Telescope.
(Ludwig Maximilian Uni e si y / Uni e si a S e nwa e München)
Ul a Ho Jupi e s (UHJs) a e gas gian exoplane s loca ed close o hei hos
s a s, making hem some o he b igh es a ge s o exoplane s udies. Thei
ex eme exposu e o s ella adia ion esul s in s ong spec al ea u es, enabling
de ailed in es iga ions in o hei chemical makeup, he mal p o iles, and
a mosphe ic dynamics. While la ge-ape u e elescopes ha e ypically been used
o a mosphe ic s udies, his p ojec aims o showcase he capabili ies o medium-
ape u e acili ies, speci ically he Wendels ein 2m elescope wi h he FOCES
high- esolu ion (HR) spec og aph, o achie e compa able esul s.
