ABSTRACTS OF
9TH INTERNATIONAL SCIENTIFIC CONFERENCE
“BALTIC APPLIED ASTROINFORMATICS AND SPACE DATA PROCESSING”
1
Abs ac s o
9 h In e na ional Scien i ic Con e ence
“Bal ic Applied As oin o ma ics and Space Da a P ocessing”
(BAASP)
No embe 12 - 13, 2025
Ven spils Uni e si y o Applied Sciences
h ps://en. en a.l /baasp2025
DOI: 10.5281/zenodo.17552759
Edi o s: Vladisla s Bez uko s & I a s Šmelds & Aija Kalniņa
2025
2
The BAASP Con e ence Se ies se es as a pla o m o es ablishing and s eng hening c oss-bo de
pa ne ships and knowledge exchange in e na ionally in he Bal ic egion and globally. These
con e ences uni e as onome s, space esea che s and enginee s, as well as expe s in ela ed
disciplines including in o ma ics, elec onics, sa elli e echnologies, geodesy, emo e sensing, and
en i onmen al sciences.
Con e ence Theme
Space science is inc easingly d i en by he Big Da a equi ing obus da a acquisi ion,
managemen , p ocessing, and in e p e a ion capabili ies. The in e disciplina y na u e o
as oin o ma ics combines space science wi h high-pe o mance compu ing, AI, and machine
lea ning, leading o b eak h oughs in obse a ional as onomy, sa elli e echnologies, and Ea h-
space in e ac ions.
In ecen yea s, Eu ope has con inued o play an impo an ole in nex -gene a ion
as onomy. The con inued expansion o he Low F equency A ay (LOFAR), an enna a ay
elescope ne wo k ac oss he con inen , including he Bal ic egion, has enabled high- esolu ion
s udies o cosmic magne ism, sola ac i i y, and ansien adio phenomena. The Eu opean VLBI
Ne wo k (EVN) has u he enhanced i s eal- ime e-VLBI capabili ies and b oadband sensi i i y,
wi h suppo om UK-based acili ies such as Jod ell Bank and e-MERLIN. These ad ancemen s
ha e con ibu ed signi ican ly o he p ecise localiza ion o as adio bu s s and compac
ex agalac ic sou ces.
Technical de elopmen s also acili a e au oma ed, apid- esponse obse a ion modes, which a e
essen ial o ad ancing mul imessenge as onomy. This eme ging ield in eg a es adio, op ical,
g a i a ional wa e, and neu ino da a o p obe ene ge ic cosmic e en s such as neu on s a me ge s
and magne a ou bu s s.
Concu en ly, b eak h oughs in AI-d i en da a mining, edge compu ing o sa elli e payloads, and
quan um-enhanced algo i hms a e opening new on ie s in eal- ime analysis and au onomous
decision-making o bo h Ea h obse a ion and deep-space missions. Meanwhile, he g owing use
o CubeSa s and modula sa elli e pla o ms is eshaping he landscape o low-cos , high-impac
space esea ch, demanding new models o da a in eg a ion, secu i y, and in e ope abili y ac oss
domains.
BAASP 2025 will con inue he dialogue on how eme ging echnologies ans o m as onomy,
space science, geoscience, and emo e obse a ion.
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CONTENTS
Ad ances in Sola Radio As onomy: Au oma ion and Imaging wi h he RT-32 Telescope
a I bene 5
Agui e E. Bez uko s V., Bez uko s D., Bouza houn El A. W., Janices I., Š einbe ngs J.,
O bidans A.
Un a eling he Galac ic E olu ion o CNO: P ecision Abundance Analysis Ac oss S ella
Popula ions 6
Amb osch M., Mikolai is Š., Smiljanic R., E nandes H., D azdauskas A., Viscasillas-Vázquez
C., Bale B., Ću ju ić B., Bagdonas V.
In oducing he pos -doc o al p ojec : Re ealing he physical mechanism o mass
ejec ion a ound young massi e s a s ia CH3OH mase s 7
Abe eld s A.
Mic owa e Obse a ions o Co onal Holes a he 25 h Sola Cycle 8
Bez uko s D.
Inspi ing he nex gene a ion o s uden s h ough ac i e pa icipa ion in adio as onomy
esea ch ia in e na ional pa ne ships. 9
Bez uko s V., Díaz S., Ruiz R., Yanguas P., Michalowski M., Kamiński K., Białobłocki P.,
Caza es J., Kalniņa A., Bel án I., Blanco C., González L., Lagzdiņa I., Jako icka S.,
Kowalewska K., Zię a a-G zesiak W., Palacián J. F., Bosque R., A angu en I. C.
Mul i-Epoch Radio Va iabili y o BL Lace ae Obse ed wi h he I bene In e e ome e and
MOJAVE A chi al Da a 10
Bez uko s V., Bu ns R. A., Š einbe gs J., Šķi man e K., Abe elds A., Shmeld I.
Explo ing VIRAC’s Capabili ies o Radio De ec ion o Quasi-Pe iodic Pulsa ions in Sola
and S ella Co onae 11
Bez uko s V., Bu ns R. A., Kolo ko D. Y., Naka iako V. M., Š einbe gs J., Šķi man e K.,
Abe elds A., Shmeld I., Bez uko s D., Belo S.A., Kalniņa A.
Va ia ions in he adio con inuum emission o high-mass p o os a s 12
Bu ns R. A., Abe elds A., Shmeld I., Š einbe gs J., Šķi man e K., Bez uko s V.
As e oid Obse a ions om he Mino Plane Cen e Da abase: Oppo uni ies and
Challenges o Ligh Cu e Analysis 13
Egli is I., Nagainis K., Sokolo a A.
Tempe a u es o dus g ains in some ci cums ella en i onmen s 14
F eimanis J.
Modeling Cosmogenic Iso opes as a Tool o S udy Sola Ene ge ic E en s 15
Golubenko K., Rozano E., Ba oni M., Ba d E., Sukhodolo T.
Come a y ac i i y modelling o ESA’s Come In e cep o mission 16
Jasmon s G., Šķi man e K., Sla inskis A., Blumbe gs K.
Visualiza ion Tools o Real-Time Nea -Field RFI Moni o ing a he LOFAR S a ion in
I bene 17
Janices I., Bez uko s V., Š einbe gs J.
The la es de elopmen s and pa e ns ela ed o space deb is issues. 18
Jo kus N.
4
Pa hs o o ma ion o in e s ella dense cloud co es 19
Kal āns J.
S uc u e and a iabili y o as ophysical mase s 20
Kalniņa A., Abe elds A.
Recen de elopmen s in I bene an enna complex 21
O bidāns A., Bleide s M., Bē ziņš A., Lau ino ičs R., Rasmanis R., e .al.
Geomagne ic dis u bances o he ea h's magne ic ield in he a ea o he S u e geode ic
a c me idian 22
O lyuk M., Romene s A., Ma chenko A., O liuk I.
A T ans o me -Based Fo ecas ing Model o GNSS-VTEC and i s Applica ion S udy O e
Nige ia 23
Osa a e A. W., Iluo e C., Abiye B., Ozegin K. O.
Sola e up ions nea elonga ed egions o open magne ic ields 24
B.I. Ryabo ., V uble skis A.
On he p og ams o moni o ing s udies o space wea he based on adio as onomical
and magne ome ic obse a ions. 25
Ryabo M. I., Sukha e A.L., Usoskin I., O lyuk M. I., Bez uko V., Š einbe gs J., Romene s
A.O., Zabo a D.A.
PauseMake : Sa elli e communica ions wi h he mowing objec 26
Šneps-Šneppe M.
P elimina y esul s o obse ing ionosphe e ac i i y using 3C sou ces 27
Š einbe gs J., Me ius M., Shule ski A.
MSCA Doc o al Ne wo k E-Sailo s: Elec ic sola wind sail doc o s 28
Sla inskis A.
Ionosphe ic and magne osphe ic esponses o he 2025 sola eclipses 29
Sukha e A., O lyuk M. I., Ryabo M. I., Usoskin, Ke o A., Romene s A., Suma uk Y.,
Kashuba V. I. , Bez uko s V., S einbe gs J.
I adia ion-Induced S uc u al Changes in Amino Acids: A Theo e ical S udy 30
Tamuliene J.
Using Jupi e 's Radio S o ms o P obe he Sola Co ona 31
Ulyano O., Za ka P., Tibu zi C., She so a A., Zakha enko V., Kono alenko O., Wuckni z
O., Lamy L., . G ießmeie G-M., Sko yk M. , K a so I., Bez uko s V., Š einbe gs J.,
Ski man e K., B azhenko A., F an suzenko A., Sko yk A.
Millennium-scale sola e up i e e en s: Ex eme space haza ds 32
Usoskin I.
Bu s hub: ge as onomical bu s s oge he 33
Zheng S., Xiong S.
Powe -law Indices o EUV In ensi y Powe Spec um in Fla ing Co onal Ac i e Regions 34
Zhong S., Kolo ko D. Y., Naka iako V. M.
5
Ad ances in Sola Radio As onomy: Au oma ion and Imaging wi h he RT-32
Telescope a I bene
Agui e E., Bez uko s V., Bez uko s D., Bouza houn E.A.W., Janices I., Š einbe gs J.,
O bidans A.
Agui e Endika - Depa men o Elec ical, Elec onic and Communica ion Enginee ing o he Public
Uni e si y o Na a a (UPNA), Pamplona, Spain; endikagui [email protected]
This wo k ocuses on ecen ad ancemen s in sola adio as onomy a he Ven spils In e na ional
Radio As onomy Cen e (VIRAC), highligh ing he mode niza ion and au oma ion o
obse a ional wo k lows using he RT-32 adio elescope. A comp ehensi e, ull-s ack web-based
sys em has been de eloped and deployed o s eamline sola obse a ions a cen ime e
wa eleng hs.
The p ima y goal o his sys em is o p o ide a secu e, use - iendly en i onmen ha allows
ope a o s o manage he en i e obse a ional pipeline— om planning and scheduling o da a
acquisi ion and image gene a ion—wi h minimal manual in e en ion. A he co e o he pla o m
is a powe ul web in e ace ha enables use s o gene a e p ecise posi ion iles o sola acking,
schedule obse a ion sessions, and moni o he s a us o ongoing wo k in eal ime.
The sys em inco po a es au oma ed pos -p ocessing ou ines, including he c ea ion, s o age, and
isualiza ion o sola maps buil om da a collec ed ia an an enna spi al scanning p ocedu e. This
aw da a is p ocessed using ad anced image econs uc ion echniques, such as bilinea
in e pola ion and Gaussian il e ing, which ans o m he aw obse a ional samples in o
scien i ically meaning ul sola b igh ness maps.
The en i e in as uc u e was buil using open-sou ce echnologies and Py hon-based as onomical
lib a ies. The esul is a obus , scalable, and ully ope a ional pla o m ha signi ican ly enhances
he e iciency, ep oducibili y, and accessibili y o sola adio obse a ions. This solu ion ma ks a
subs an ial s ep o wa d in mode nizing he wo k lows o single-dish adio elescopes.
6
Un a eling he Galac ic E olu ion o CNO: P ecision Abundance Analysis
Ac oss S ella Popula ions
Amb osch M., Mikolai is Š., Smiljanic R., E nandes H., D azdauskas A., Viscasillas-Vázquez C.,
Bale B., Ću ju ić B., Bagdonas V.
Amb osch Ma kus - Vilnius Uni e si y, Ins i u e o Theo e ical Physics and As onomy;
ma kus.amb osch@ . u.l
Ca bon, ni ogen, and oxygen (CNO) a e cen al o bo h s ella and Galac ic chemical e olu ion,
ye hei en ichmen his o y ac oss he Milky Way is s ill no ully unde s ood. This alk p esen s a
p ojec aimed a deli e ing a homogeneous and high-p ecision analysis o CNO abundances in a
la ge and di e se sample o s a s spanning all majo Galac ic componen s.
Ou s a egy combines new spec oscopic obse a ions wi h da a om la ge s ella su eys,
ancho ed by a se o well-cha ac e ized e e ence s a s. This enables accu a e calib a ion o s ella
pa ame e s and abundance measu emen s, along wi h p ecise age de e mina ions (~10%) ia
isoch one i ing. By in eg a ing chemical abundances, s ella ages, and o bi al dynamics, we
pe o m a popula ion-le el and adial mig a ion analysis o ace he spa ial and empo al e olu ion
o CNO ac oss he Galaxy.
To ully exploi he ich da ase s om mode n su eys, we employ bo h classical physics-based
spec oscopic me hods and no el machine-lea ning echniques. This dual app oach enhances he
p ecision, consis ency, and scalabili y o ou analysis.
Beyond Galac ic en ichmen , he p ojec in es iga es he ole o s ella mixing and magne ic
ac i i y in shaping su ace abundances—an a ea s ill lacking obus obse a ional cons ain s.
These e ec s a e c ucial o unde s anding abundance pa e ns in e ol ed s a s and imp o ing
s ella e olu ion models.
7
In oducing he pos -doc o al p ojec : Re ealing he physical mechanism o
mass ejec ion a ound young massi e s a s ia CH3OH mase s
Abe elds A.
Abe elds A is - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); a is.abe elds@ en a.l
This p ojec aims o shed ligh on he physical mechanism d i ing hose s iking ou lows obse ed
ubiqui ously a ound young s a s in ou Galaxy. The la ge amoun o gas and dus ejec ed away
along he pola di ec ions o a young s a is gene ally e e ed o as an "ou low". Ou low
phenomena a e s ic ly ela ed o he p ocess o mass acc e ion in o a s a , egula ing he ime-scale
o he acc e ion p ocess and, in u n, he inal s ella mass. The e o e, hei unde s anding is
undamen al o assessing ou pa adigm o s a o ma ion. He e, I p opose o exploi he in o ma ion
coming om me hanol mase emission, a unique ace obse ed a he base o p o os ella
ou lows, o sys ema ically s udy, o he i s ime, how ci cums ella gas is blown away a adii o
a ew 100 au (o less) om he s a . O e all, his p ojec is designed on a ine uning be ween
scien i ic objec i es and ins umen al acili ies, wi h he aim o s ill enhance i s impac wi h nex -
decades obse a ional acili ies and o maximize my chances o becoming a majo expe in he
ield.
8
Mic owa e Obse a ions o Co onal Holes a he 25 h Sola Cycle
Bez uko s D.
Bez uko s Dmi ijs - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); dmi ijs.bez uko s@ en a.l
S udies o co onal holes and co onal hole-like a eas wi h educed b igh ness empe a u es in
mic owa es ha e a signi icance o unde s and mani es a ions o he sola ac i i y, dis ibu ions o
plasma pa ame e s in he sola co ona and condi ions o he c ea ion o he sola wind and space
wea he . I 's well known ha he mic owa e emission o co onal holes has a low con as o clea ly
obse e and i s isibili y depends on he phase o he sola cycle and ea u es o an ins umen as
well.
The adio elescope RT-32 o Ven spils In e na ional Radio As onomy Cen e (VIRAC) p o ides
ou ine 2D ca og aphy o he pola ized mic owa e emission o he Sun in wa eleng hs o 7.5-2.3
cm (4.1-14.2 GHz) wi h he low noise mul ichannel spec al pola ime e . Taking in o accoun ha
he mic owa e emission is c ea ed a di e en heigh s in o he co ona spec al pola ime ic
obse a ions o e he possibili y o analyse he educ ion o plasma densi ies and i s dis ibu ion
in o co onal holes.
The p esen a ion conce ns compa ison o he mic owa e emission o some cha ac e is ic co onal
holes obse ed wi h he adio elescope VIRAC RT-32 in 2019-2020 and 2024-2025 ( he minimum
and maximum o 25 h sola cycle). Some a emp s o e alua e he heigh dis ibu ion o plasma
elec on densi ies in he co ona a e p esen ed also.
15
Modeling Cosmogenic Iso opes as a Tool o S udy Sola Ene ge ic E en s
Golubenko K., Rozano E., Ba oni M., Ba d E., Sukhodolo T.
Golubenko Kseniia - Uni e si y o Oulu, Physics and As onomy; kseniia.golubenko@oulu. i
Unde s anding he long- e m beha iou o he Sun is essen ial o bo h as ophysical esea ch and
assessing he po en ial impac s o ex eme sola ac i i y on Ea h. Di ec obse a ions o sola
ene ge ic pa icles (SEPs) co e only he pas ew decades o he space age. To in es iga e s onge
and a e e en s o e millennia, indi ec e idence p ese ed in na u al a chi es is equi ed. One o
he mos powe ul app oaches elies on cosmogenic iso opes such as adioca bon (14C) in ee
ings, and be yllium-10 (10Be) and chlo ine-36 in pola ice, which a e p oduced in he a mosphe e
when cosmic ays o sola pa icles in e ac wi h ni ogen and oxygen nuclei.
Nume ical modeling o iso ope p oduc ion p o ides a link be ween measu ed concen a ions in
a chi es and sola p ocesses. By combining physics-based simula ions o pa icle anspo in he
a mosphe e wi h ca bon cycle and clima e models (e.g. SOCOL model), i becomes possible o
econs uc he in ensi y and iming o pas sola ene ge ic pa icle e en s. This app oach has
e ealed se e al ex eme his o ical e en s ha exceed any hing obse ed du ing he ins umen al
e a by o de s o magni ude.
We demons a e how iso ope modeling quan i ies he magni ude and occu ence ime o pas sola
pa icle s o ms, ou line unce ain ies ela ed o a mosphe ic dynamics and da a esolu ion, and place
econs uc ed e en s in he con ex o mode n obse a ions. Such econs uc ions no only expand
knowledge o sola a iabili y bu also help assess po en ial isks om ex eme space wea he o
p esen -day echnology.
16
Come a y ac i i y modelling o ESA’s Come In e cep o mission
Jasmon s G., Šķi man e K., Sla inskis A., Blumbe gs K.
Jasmon s Gin s - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); gin s.jasmon s@ en a.l
ESA’s Come In e cep o will pe o m a apid lyby o a dynamically new come o igina ing om
he ou e Sola Sys em, po en ially p ese ing ma e ials ha p eda e he Sola Sys em i sel .
Because such objec s ollow highly eccen ic o bi s and a e o en disco e ed only a ew mon hs
be o e pe ihelion, he mission will wai a he Sun-Ea h L2 poin un il a sui able a ge is iden i ied.
This “unknown a ge ” pa adigm complica es p e-launch planning, since ins umen de elopmen
and calib a ion ypically ely on well-cha ac e ized bodies.
We add ess his challenge wi h physics-based models ha span plausible come ac i i y s a es,
including coma, ansien ou bu s s, collima ed je s, and esul ing ail mo phology. These models
a e embedded in a Blende based digi al win o he lyby, p oducing syn he ic obse a ions o
MIRMIS, OPIC, and EnVisS ac oss a ange o phase angles, spin s a es, and ac i i y le els. The
en i onmen enables assessmen o da a quali y agains ins umen objec i es as well as showcases
unplanned scena ios o da a acquisi ion.
By le e aging he physically based Cycles ende ing engine, we simula e ligh sca e ing o dus
pa icles using phase unc ions and densi y ields de i ed om ou models, yielding
pho ome ically consis en image y. We p esen ep esen a i e scena ios, compa isons o p e ious
obse a ional da a, and ongoing wo k o e ine dus dynamics and pho ome ic ideli y. This
capabili y ad ances ins umen eadiness and ope a ions planning when he eal a ge emains
unknown un il la e in he mission imeline.
17
Visualiza ion Tools o Real-Time Nea -Field RFI Moni o ing a he LOFAR
S a ion in I bene
Janices I., Bez uko s V., Š einbe gs J.
Janices Iñaki - Public Uni e si y o Na a e Dp . o Elec ical, Elec onic and Communica ions
Enginee ing; ijanices[email p o ec ed]
Radio F equency In e e ence (RFI) emains a c i ical challenge in low- equency adio as onomy,
pa icula ly o so wa e-de ined a ays like LOFAR (Low F equency A ay). This s udy p esen s
a comp ehensi e app oach o nea - ield RFI de ec ion and isualiza ion a he LOFAR s a ion in
I bene, La ia, ope a ed by he Ven spils In e na ional Radio As onomy Cen e (VIRAC).
Le e aging single-s a ion in e e ome y and in e nal isibili y da a, we de eloped a modula
imaging pipeline capable o gene a ing nea - ield powe maps ac oss equency, ime, and heigh
dimensions.
The sys em in eg a es calib a ion ou ines, sweep-based imaging, and a eal- ime mul i h eaded
p ocessing engine wi h a web-based in e ace. This enables li e moni o ing o in e e ence sou ces
and suppo s ield es ing wi h con olled emi e s. Field campaigns conduc ed a I bene alida ed
he sys em’s abili y o de ec and localize RFI sou ces wi h me e -le el p ecision, e en unde
cons ained condi ions.
Key con ibu ions include:
• Adap a ion o he open-sou ce lo a imaging amewo k and use in nea - ield.
• Implemen a ion o sweep ou ines o dynamic RFI cha ac e iza ion.
• De elopmen o a eal- ime imaging and con ol in e ace wi h li e acking.
• Deploymen o a Docke -based en i onmen o ep oducibili y and po abili y.
This wo k imp o es LOFAR’s awa eness o local in e e ence and es ablishes a ounda ion o
ope a ional, s a ion-le el RFI moni o ing ools. The sys em is publicly a ailable ia Gi Hub and
suppo s u u e in eg a ion in o b oade diagnos ic amewo ks."
18
The la es de elopmen s and pa e ns ela ed o space deb is issues.
Jo kus N.
Jo kus Nansija - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); nansija.jo [email protected]
The issue o space deb is is escala ing due o an inc easing numbe o sa elli e launches, ageing
de unc sa elli es and agmen s esul ing om collisions and an i-sa elli e es s. Recen
de elopmen s indica e echnological and egula o y p og ess aimed a mi iga ing his isk, hough
signi ican challenges emain.
The ESA has upda ed i s Space Deb is Mi iga ion Policy and Requi emen s (as o No embe 2023),
sho ening he disposal phase o Low Ea h O bi (LEO) objec s om 25 yea s o 5 yea s, aising
he success p obabili y h eshold o disposal ope a ions and in oducing in e aces o acili a e
se icing o emo al in he e en o sa elli e ailu e.
Meanwhile, he p oposed EU Space Ac (due o be in oduced in mid-2025) seeks o s anda dise
egula ions ac oss Membe S a es, ensu ing he sa e y, esilience and en i onmen al sus ainabili y
o space ope a ions. This includes he in oduc ion o s ic e ules o deb is acking and
mi iga ion.
The e is also inc easing indus y coope a ion: he ESA's “Ze o Deb is Cha e ” encou ages en i ies
o commi o p e en ing new deb is, and dialogues a e aking place (e.g. wi h comme cial
ope a o s) abou joining hese olun a y cha e s.
19
Pa hs o o ma ion o in e s ella dense cloud co es
Kal āns J.
Kal āns Ju is - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); ju is.kal ans@ en a.l
The s a less co es o in e s ella clouds a e a s anda d case o simple as ochemical modelling,
o en used o es new me hods and heo ies. The physical o ma ion o such dense co es is egula ed
by la ge-scale p ocesses and canno be desc ibed by an isola ed e olu ion scena io o he co e i sel .
We desc ibe se e al pa hs how e ol ing physical condi ions a i e a hose cha ac e is ic o dense
co es. The alidi y o each scena io is es ed wi h an as ochemical model by compa ing calcula ed
abundances o in e s ella ice species o obse a ions. Fi e cen al densi y e olu ion pa hs we e
conside ed: exponen ial, linea , sigmoid (S- ype), and asymp o ic g ow h, as well as g a i a ional
in all. Two ime-scales – 1 My and 3 My – we e applied o each case. Inc ease o he cen al
densi y was accompanied by con ac ion o a sphe ical (1D) molecula cloud wi h a cons an mass.
Resul s. The exponen ial, in all, linea , and sigmoid densi y e olu ion scena ios a e appa en ly all
able o eplica e obse ed ice composi ion, each wi h i s own ime-scale. Addi ional chemical
e olu ion in long-li ed co es wi h s eady condi ions is essen ial o explaining disag eemen s in ice
abundances. The esul s indica e a consis en 0.5 My -long ac i e g ow h s age o dense cloud
co es, in addi ion o pe iods o slowe con ac ion be o e o a e he ac i e s age. Finally, we ind
ha he o en-used simple models s a ing wi h a omic chemical composi ion in dense co e
condi ions p oduce ice species' abundances ha a e incompa ible wi h obse a ions.
20
S uc u e and a iabili y o as ophysical mase s
Kalniņa A., Abe elds A.
Kalniņa Aija - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); aija.kalnina@ en a.l
We obse ed 2 me hanol mase sou ces G32.03+0.06, G35.20 -1.74 (W48) a 6.7 GHz using he
Eu opean VLBI Ne wo k (EVN). These mase s ha e been sys ema ically moni o ed o e he pas
i e yea s wi h he I bene 16 m and 32 m adio elescopes [1]. Selec ed sou ces ha e di e en
a iabili y ypes pe iodic, quasi-pe iodic, long- e m dimming. Ou p ima y objec i es a e o
in es iga e he p ope mo ions, a iabili y mechanisms, sou ce mo phology, and cloudle s uc u e
e olu ion o hese mase s. We aim o iden i y he physical p ocesses d i ing mase a iabili y and
imp o e ou unde s anding o he unde lying as ophysical condi ions.
[1] A. Abe elds, J. Š einbe gs, I. Shmeld, R. A. Bu ns, ‘’Fi e yea s o 6.7-GHz me hanol mase moni o ing wi h
I bene adio elescopes” Mon hly No ices o he Royal As onomical Socie y,Volume 526, Issue 4, Decembe 2023,
Pages 5699–5714, h ps://doi.o g/10.1093/mn as/s ad3158
21
Recen de elopmen s in I bene an enna complex
O bidāns A., Bleide s M., Bē ziņš A., Lau ino ičs R., Rasmanis R., e .al.
O bidāns A ū s - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); a u s.o bidans@ en a.l
Du ing he las ew yea s, mul iple p ojec s ha e been ca ied ou o con inuously upg ade he
ecei ing capabili ies o he I bene an ennas RT-32 and RT-16, as well as o es ablish ansmi ing
capabili ies o bo h an ennas. De elopmen o new eed ho ns, RF ne wo ks, ecei e s, and
c yos a s e c. has been unde aken wi h he goal o enabling deep-space communica ions, wi h
special emphasis on u u e Luna missions.
In pa allel, he needs o adio as onomy a e being add essed h ough he de elopmen o new
c yogenic L/S-band ecei e and by suppo ing a ious in e na ional scien i ic p ojec s. These
imp o emen s signi ican ly enhance he o e all sensi i i y and ope a ional lexibili y o he I bene
an enna complex, posi ioning i as a key in as uc u e o bo h scien i ic esea ch and space
mission suppo .
Du ing his alk, he audience will be in oduced o he cu en echnical capabili ies o he I bene
an ennas, ecen de elopmen achie emen s, and u u e plans o expanding hei ole in deep-space
and adio as onomical esea ch.
22
Geomagne ic dis u bances o he ea h's magne ic ield in he a ea o he
S u e geode ic a c me idian
O lyuk M., Romene s A., Ma chenko A., O liuk I.
O lyuk Mykhailo - Subbo in Ins i u e o Geophysics o he Na ional Academy o Sciences o Uk aine;
[email p o ec ed]
A p esen , he issues o sola - e es ial in e ac ions a e e y ele an , especially he mechanisms
o ansmission o deep space dis u bances o he Ea h's su ace. One o he main componen s o
he sola - e es ial in e ac ions is he magne ic ield. I , on he one hand, se es as a link be ween
he Sun and he Ea h, and, on he o he hand, causes a di e en esponse o he same impac
depending on he “ elie ” o he Ea h's in e nal magne ic ield. To do his, we in es iga ed he
“ eac ion” o he Ea h's magne ic ield o he co onal mass ejec ion o May 7, 2024, which eached
he Ea h's o bi on May 10, 2024, and he associa ed magne ic s o m ha las ed mo e han 24
hou s. The in luence o high-ene gy sou ces o ex e nal o igin on magne osphe ic-ionosphe ic
p ocesses and ela ed pe u ba ions o he Ea h's ou e and inne shells is well unde s ood. The
in e ac ion o he magne osphe ic-ionosphe ic geomagne ic dis u bance wi h he Ea h's in e nal
magne ic ield emains less s udied. In his ega d, we s udied he pe u ba ions o he Ea h's
magne ic ield along he me idian S u e Geode ic A c (SGA). The SGA me idian is cha ac e ized
by signi ican changes in he Ea h's main magne ic ield (co e ield) and anomalous magne ic ield
(li hosphe e ield). The e a e 7 magne ic obse a o ies in he icini y o he SGA, which makes i
possible o assess he na u e o magne ic s o m on May 10-13, 2024, depending on he global and
egional cha ac e is ics o he Ea h's in e nal magne ic ield.
23
A T ans o me -Based Fo ecas ing Model o GNSS-VTEC and i s Applica ion
S udy O e Nige ia
Osa a e A. W., Iluo e C., Abiye B., Ozegin K. O.
Osa a e Aghedo Williams - Uni e si y o Nige ia, Depa men o Physics and As onomy, Nsukka 400241,
Nige ia; aghedowilliamsosa a [email protected]
This pape p esen s a no el app oach using channel-independen pa ch ime se ies T ans o me
(Pa chTST) o GPS-VTEC o ecas ing. This is he i s ime ha a Pa ch Time Se ies T ans o me
(Pa chTST) amewo k has been in eg a ed in o GPS-VTEC o ecas ing, demons a ing i s
applicabili y o ionosphe ic p edic ion. We cons uc he GPS-VTEC da ase using obse a ions
om Nige ia, le e aging da a collec ed om ionosphe ic moni o ing s a ions. Fac o s in luencing
GPS-VTEC a ia ions, such as seasonal changes, diu nal pa e ns, magne ic ac i i y, and sola
ac i i y, a e iden i ied and inco po a ed as inpu pa ame e s o he models. T aining is conduc ed
using da a om he yea 2012–2021, while he model pe o mance is e alua ed using he yea 2022
da a, a pe iod o high sola ac i i y. We compa e he pe o mance o Pa chTST, MLP, LSTM,
BiGRU, and CNNBiGRU models, e alua ing hei o ecas ing accu acy using oo mean squa ed
e o (RMSE), mean absolu e pe cen age e o (MAPE), and co ela ion coe icien (R). The
Pa chTST model achie es an RMSE o 4.731 TECU, a MAPE o 2.351%, and an R- alue o 0.986,
ou pe o ming adi ional deep lea ning models in sho - e m (1-day) and mid- e m o ecas ing.
The hyb id CNNBiGRU model also shows s ong p edic i e capabili y, achie ing an RMSE o
3.046 TECU and an R- alue o 0.896, e ec i ely cap u ing diu nal a ia ions o GPS-VTEC.
Addi ionally, unce ain y analysis e eals ha Pa chTST exhibi s supe io adap abili y o model
unce ain y, showing a 62.9% imp o emen in mean e o (ME) and a 40.5% imp o emen in
s anda d mean e o (STDE) compa ed o benchma k models. Compa isons wi h IRI-2016 and
NeQuick-2 models indica e ha while Pa chTST p o ides mo e accu a e p edic ions han all he
models including he deep lea ning models and he empi ical models in cap u ing seasonal
a ia ions ac oss he da ase .
24
Sola e up ions nea elonga ed egions o open magne ic ields
Ryabo . B.I., V uble skis A.
Ryabo Bo iss - Enginee ing Resea ch Ins i u e Ven spils In e na ional Radio As onomy Cen e (ERI
VIRAC) o Ven spils Uni e si y o Applied Sciences (VUAS); bo iss @ en a.l
Sola la es and co onal mass ejec ions (CMEs) a e he mos powe ul phenomena on he Sun
belie ed o be caused by ins abili ies in sola magne ic ields. We examine how na ow elonga ed
egions o open magne ic ields ela e o hese phenomena. Fo his pu pose CMEs and he
associa ed sola la es a e aced nea an elonga ed open- ield egion du ing Janua y - Ma ch 2013.
By modelling co onal ields wi h he Po en ial Field Sou ce Su ace model (PFSS), we e eal high
squashing o ield lines. Since such high squashing p omo es econnec ion o magne ic ield lines,
we ecognize he e he po en ial o igge ing he e up ions. A se o ex eme ul a iole images
om he AIA ins umen on boa d he Sola Dynamic Obse a o y also implies long-las ing (up o
5 - 10 hou s) e en s o magne ic econnec ion in he pos - la e a cade and he co onal dimming
accompanying a CME. We conclude ha by enabling sus ained ield line econnec ion he na ow
egions o open- ields a e possibly linked o he nea by sola e up ions.
This esea ch is unded by he Eu opean Regional De elopmen Fund, p ojec "ERA Chai in
As ophysics, 350 Ins umen a ion, G ound Segmen Technologies and Space Pho onics a he
Uni e si y o La ia", p ojec No. 351 1.1.1.5/2/24/A/004.
31
Using Jupi e 's Radio S o ms o P obe he Sola Co ona
Ulyano O., Za ka P., Tibu zi C., She so a A., Zakha enko V., Kono alenko O., Wuckni z O.,
Lamy L., G ießmeie G-M., Sko yk M., K a so I., Bez uko s V., Š einbe gs J.,
Ski man e K., B azhenko A., F an suzenko A., Sko yk A.
Ulyano Oleg - Ins i u e o Radio As onomy, Na ional Academy o Sciences o Uk aine, Kha ki , 61002
Uk aine; oulya[email p o ec ed]
Low- equency obse a ions o a ious ypes o bu s s gene a ed in he sola co ona ha e one
common ea u e. In he decame e -me e anges, hey all ha e p edominan ly one ci cula
pola iza ion. This pola iza ion is associa ed wi h he no mal mode o ha o dina y/ex ao dina y
wa e, which has a lowe a enua ion coe icien . One possible explana ion o hese pola iza ion
cha ac e is ics o low- equency sola bu s s is ha hey o igina e a ela i ely high al i udes (1.5-
2 Rsun), whe e he in ensi y o he magne ic ield in he sola co ona is ~ 1G. Fu he mo e,
p opaga ing owa ds Ea h, one o hese wa es a enua es mo e han he o he due o g ea e
in e ac ion wi h he Sun's magne ic ield and, acco dingly, g ea e op ical hickness. Howe e , his
explana ion is incomple e, as i does no explain how magne ic ields wi h low in ensi ies keep
sub ela i is ic elec on beams, which gene a e a ious ypes o bu s s, om Coulomb epulsion.
On he o he hand, he ci cula pola iza ion may be imposed by he mo ing elec ons hemsel es
o e la ge sec ions o he co onal magne ic ield, in which case he pola iza ion o sola bu s s is
de e mined by he elec on’s mo ion.
Fo a mo e de ailed s udy o he co ona plasma p ope ies, obse a ions o Jupi e 's eclipse by he
Sun's co ona we e ca ied ou . These obse a ions we e ca ied ou om May o Augus 2025. In
his case, decame e adio s o ms, which occu ed episodically in he Jupi e -Io ube, we e
conside ed by us as a poin b oadband pulsed sou ce o ellip ically pola ized adia ion. This adio
emission was used o p obe he Sun's co ona a a ious elonga ions. In pa icula , we managed o
eco d a Jupi e adio s o m 2 deg ees om he Sun cen e . To de e mine he pa ame e s o he sola
co ona plasma, we will s udy such p opaga ion e ec s as sca e ing and dynamic o a ion measu e,
which will allow us o es ima e he pa ame e s o magne ized plasma in he Sun's co ona.
32
Millennium-scale sola e up i e e en s: Ex eme space haza ds
Usoskin I.
Usoskin Ilya - Uni e si y o Oulu, Sodankylä geophysical Obse a o y; ilya.uso[email p o ec ed]
The Sun is a a iable s a , some imes p oducing e up i e e en s such as la es and co onal mass
ejec ions, which can dis up he nea -Ea h en i onmen and pose signi ican h ea s o mode n
echnological socie y. As disco e ed ecen ly using indi ec p oxy da a, he Sun can a ely p oduce
ex eme sola pa icle e en s (ESPEs). P esen ly, se en e en s and wo candida es a e known o
he pas 14 millennia, making hem millennium-scale e en s. ESPEs can be o de s o magni ude
s onge han he s onges e en s di ec ly obse ed du ing he las decades. A summa y o he
cu en knowledge o he occu ence a es and econs uc ed pa ame e s o he ESPEs is discussed
in he con ex o he possible e es ial e ec s, such as adia ion dose and egional clima e.
33
Bu s hub: ge as onomical bu s s oge he
Zheng S., Xiong S.
Zheng Shijie - Ins i u e o High Ene gy Physics, CAS, Pa icle As ophysics Cen e ; [email protected]
In he e a o mul i-messenge mul i wa eleng h as onomy, i is o c i ical impo ance o make join
obse a ions wi h a ious elescopes and ins umen s in a imely manne .
These obse a ions usually will be epo ed as a ious ypes o Messages in di e en pla o ms,
which is somewha incon enien o esea che s.
We collec hese Messages om a ious pla o m and g oup hem in o as onomical bu s E en s
wi h AI and p o ide s a is ics o all and he la es E en s and Messages and highligh he mos
popula E en s (called Ho E en s).
34
Powe -law Indices o EUV In ensi y Powe Spec um in Fla ing Co onal
Ac i e Regions
Zhong S., Kolo ko D. Y., Naka iako V. M.
Zhong Sihui - KU Leu en, Depa men o Ma hema ics; sihui.zhong@kuleu en.be
Sola in ensi y powe spec a a e usually cha ac e ised by colou ed noise, wi h he spec al ene gy
ollowing a segmen ed powe -law unc ion o equency, S( ) ∝ ⁻ᵅ o e di e en equency anges.
Typically, he powe -law index exceeds 1 in he low- equency pa (αₗ ) and is a ound 0 a high
equencies (αₕ ). This wo k in es iga es he spa ial and empo al e olu ion o he powe -law
indices o co onal EUV in ensi y powe spec a in la e-hos ing ac i e egions.
The spa ial dis ibu ion o he powe -law index in he low- equency domain (αₗ ) closely mi o s
EUV in ensi y images, indica ing ha αₗ can e eal he dynamics o co onal plasma s uc u es.
Tempo ally, αₗ emains s able in quiescen ac i e egions, bu i exhibi s signi ican a iabili y
be o e he la e onse . Mo i a ed by his beha iou , we analysed 14 la e e en s, quan i ying he
empo al a ia ion o he indices αₗ and αₕ as po en ial la e p ecu so s. In all la e e en s
conside ed, no able de ia ions o αₗ beyond a de ined h eshold consis en ly occu ed a he la e
si e wi hin a ew minu es be o e he la e. In some cases, he change in he alue o αₗ − αₕ was
de ec ed wi hin 30–90 minu es be o e he la e. These indings sugges ha he empo al a ia ion
o he powe -law indices in co onal EUV in ensi y powe spec a could po en ially se e as sho -
e m p ecu so s o sola la es, which needs o be alida ed on a la ge la e sample.
35
