Meeting of Young Astronomers and Astrophysicists - FIKUT NEXTGEN

4 Nov 2026, 09:00 → 6 Nov 2026, 18:00 Europe/Budapest

HUN-REN Wigner Research Centre for Physics

The Meeting of Young Astronomers and Astrophysicists (Fiatal Csillagász és Asztrofizikus Kutatók Találkozója - FIKUT NEXTGEN) returns after 12 years, bringing together a new generation of researchers.

The aim of the meeting is to provide BSc, MSc and PhD students, as well as recent PhD graduates, with an opportunity to present their work, learn about each other’s research, and publish their findings. FIKUT NEXTGEN embraces the full diversity of modern astrophysical research — including theoretical studies, numerical modelling, data analysis, space engineering, AI‑based methods, observations, instrumentation, and interdisciplinary frontier areas such as astrochemistry, planetary and atmospheric chemistry, and fields that connect astronomy with physics, computer science, and data‑driven sciences.

Organising institutions: Wigner, CSFK CSI, ATOMKI, ELTE.

The Organizing Committee:

• Dóra Tarczay-Nehéz (chair, HUN-REN CSFK CSI)

• Borbála Cseh (co-chair, HUN-REN CSFK CSI)

• Bálint Seli (HUN-REN CSFK CSI)

• László Molnár (HUN-REN CSFK CSI)

• Balázs Kacskovics (HUN-REN Wigner FK)

• Gergely Gábor Barnaföldi (HUN-REN Wigner FK)

• Emese Forgács-Dajka (ELTE TTK)
• György Gyürky (HUN-REN ATOMKI)

 

Wednesday 4 November

09:30 Registration

Opening Talks

Conveners: Borbála Cseh (Konkoly Observatory, HUN-REN CSFK), Dóra Tarczay-Nehéz (HUN-REN CSFK CSI), Dr Gergely Barnafoldi (HUN-REN Wigner Reseach Centre for Physics), György Gyürky (HUN-REN Institute for Nuclear Research (ATOMKI), Debrecen, Hungary), Krisztina Gabanyi (Departments of Theoretical and Experimental Physics, University of Szeged), Róbert Szabó (HUN-REN CSFK Konkoly Observatory)

FIKUT_NEXTGEN_2026.pdf

TND_Opening.pdf

welcome_talk_gyurky.pdf

Stellar Pulsations, Activity, and Evolution

Convener: Róbert Szabó (HUN-REN CSFK Konkoly Observatory)

1 Light Curve Modelling of the peculiar interacting SN 2019vxm

Massive stars can undergo substantial mass loss through several mechanisms, including nuclear flashes, pulsational pair instability (PPI), and convection waves depositing energy in the stellar envelope. Such mass-loss episodes are expected to create dense circumstellar environments that significantly affect the light curves of subsequent supernova explosions through ejecta–circumstellar material (CSM) interaction.
Type IIn supernovae (SNe) exhibit luminous light curves that can be strongly affected by this effect. This type of SNe exhibits a myriad of evolutionary profiles, with diversity in luminosity, dynamics, interactions, CSM morphology, and dust formation.

In our study, we examine SN 2019vxm, an interacting supernova that belongs to the class of long-lasting Type IIn events, whose precise model parameters remain a subject of debate to this day.
Thus, we investigate the modelling approaches used in previous studies of SN 2019vxm, comparing the models adopted to reproduce its observed light curve and the physical parameters derived from them.

Our aim is to create a completely separate modeling method, where we combine stellar evolution models generated by MESA (Modules for Experiments in Stellar Astrophysics) with synthetic light curves calculated using SNEC (Supernova Explosion Code).
Since SNEC only considers radioactive Ni decay and does not include luminosity generated by ejecta–CSM interaction, we propose to investigate the CSM contribution separately.

Speaker: Boróka Hanga Pál (Szegedi Tudományegyetem)

2 The TESS view of AGB pulsators: opportunities and limitations

The Transiting Exoplanet Survey Satellite (TESS) has accumulated an extensive photometric dataset for pulsating stars across the sky. Its scientific value for long-period pulsators depends strongly on the available time baseline. A single 27-day sector often covers only a fraction of a pulsation cycle, whereas stars in overlapping sectors may be monitored for several months, with coverage approaching one year in the continuous viewing zones (CVZs). Light curve quality also depends on target brightness, source crowding, and the ability to mitigate instrumental systematics.
Pulsators on the asymptotic giant branch (AGB) and beyond include semiregular variables (SRVs), OGLE small amplitude red giants (OSARGs), and RV Tauri stars in the post-AGB phase. These stars often exhibit irregular variability, with multiple pulsation modes contributing to the light curves of SRVs and OSARGs and alternating deep and shallow minima characterizing RV Tauri stars. Typical periods range from tens to several hundred days, and amplitudes vary from less than 0.1 mag to a few magnitudes.
We examine the available TESS data with particular attention to AGB stars in the Large Magellanic Cloud (LMC), which lies within the southern CVZ and therefore benefits from extended temporal coverage, while also presenting challenges due to severe crowding. Our study aims to provide a practical overview of the strengths and limitations of TESS observations for AGB variables and to identify promising targets and datasets for future studies of long-period stellar variability. Among the three types, we found SRVs to be the most promising targets for period analysis with TESS and therefore focus on these stars, comparing their TESS-derived periods with literature values.

Speaker: Marcell L. Kovács (HUN-REN CSFK Konkoly Observatory, Eötvös University Institute of Physics)

11:00 Coffee break

Stellar Pulsations, Activity, and Evolution

Convener: Róbert Szabó (HUN-REN CSFK Konkoly Observatory)

3 SN 2026ejy: a peculiar 1987A-like supernova with an early-phase luminosity excess

Supernova (SN) explosions are fundamental phenomena representing the final stages of stellar evolution, during which an enormous amount of energy is released over a short period of time. The radiation emitted during the explosion can interact with the circumstellar material (CSM), which can significantly affect the observed light curves (LCs) and spectra.
A classic example of this phenomenon is SN 1987A, a hydrogen-rich Type II SN. Interestingly, its spectroscopic properties resembled those of Type IIP SN, while its LC exhibited a different evolution. Objects similar to SN 1987A constitute a rare class of SNe, although the circumstances of their formation are still not fully understood. The hypothesis of this research is that the properties of peculiar SNe resembling SN 1987A but exhibiting stronger radiation–matter interaction – such as the shape of the LC, late-time rebrightening, or the appearance of characteristic emission lines – can be explained by substantial mass loss prior to the explosion and the presence of dense circumstellar material.
In recent years, several peculiar SNe similar to SN 1987A but exhibiting more pronounced radiation–matter interaction have been identified; SN 2026ejy is one such example. The physical properties of SN 2026ejy make it a suitable target for investigating the physical characteristics indicative of circumstellar interaction with sufficient accuracy using the available instruments and data-processing methods. The aim of my research is to perform a consistent analysis of the observations of these objects, with particular focus on SN 2026ejy, complemented by the observations of the 80 cm telescope of the SZTE Baja Observatory, and to determine their physical parameters and perform a comparative analysis using photometric and spectroscopic methods. This investigation may contribute to a deeper understanding of the nature of SN 1987A-like SNe.

Speaker: Zsófia Vig

FIKUT_SN2026ejy_VZS.pdf

4 Analysis of the Gaia Alerted eruptive young star candidate Gaia24bux

Young stellar objects (YSOs) show variability on very different time scales and with different amplitudes due to several physical mechanisms including changes in the mass accretion rate. Eruptive YSOs show variability on longer time scales (from several months to a year or from decades to a century) and with amplitudes up to 6 magnitudes. Studying these examples of episodic accretion is important for understanding how Sun-like stars accumulated their mass.

Gaia24bux is a YSO candidate at a distance of $\sim$946 pc. It had a Gaia Alert in 2024 due to an approximately 2 year long brightening by about 3.4 magnitudes. The star had a previous, about 1.5 year long brightening event in 2015-2016, which had an amplitude of $\sim$2.8 magnitudes.
I used archival optical and infrared photometry, as well as near-infrared spectra obtained with the NASA Infrared Telescope Facility to understand the physical properties of Gaia24bux, as well as its recent brightening.
Based on its infrared photometry, I classified Gaia24bux as a Class II YSO. I used a grid of radiative transfer models to fit the quiescent spectral energy distribution of the star and found that it is most consistent with an effective temperature of 3672 K, a mass of 0.47 M$_\odot$ and a radius of 5.63 R$_\odot$.

The IRTF spectra of the star obtained at three epochs during the outburst show significant similarities to the spectra of FUor-type eruptive young stars, such as the absence of emission lines, weak hydrogen lines, a “triangular” H-band continuum, and strong CO absorption bands. However, there also are a few key differences between the spectra of Gaia24bux and FUors: it does not show molecular bands other than CO, and the equivalent widths of the CO lines versus the Na I (2.208 micron) and Ca I (2.256 micron) lines are more consistent with classical T Tauri stars rather than FUors. Also, Gaia24bux has faded back to its quiescent brightness after more than two years, which is inconsistent with FUors.

Based on our current results, Gaia24bux is most consistent with the Peculiar/V1647 Ori-like/MNor class of eruptive YSOs, which objects show intermediate properties of the two traditionally defined classes of eruptive YSOs.

Speaker: Dániel Estók (ELTE, HUN-REN CSFK CSI)

Dániel_Estók_Gaia24bux_FIKUT.pdf

5 Evolution of photoevaporative disk dead zone

The observed lifetimes of protoplanetary disks are well established, but the mechanisms responsible for their dispersal are still under investigation. In the classical α-viscous model angular momentum transport is assumed to be driven by the magnetorotational instability (MRI), which requires sufficient ionization. The ionization structure of a disk is spatially non-uniform: highly ionized inner and outer regions surround a dead zone which is magnetically inactive. High-energy radiation launches a thermal wind that contributes to disk dispersal in the process called photoevaporation. The viscous evolution of the disk with dead zone and photoevaporation interact to shape the gas and dust distribution, which plays an important role in planetary accretion and migration. In this work, I present one-dimensional disk evolution models on 1Myr timescale that account for photoevaporation and the formation of the dead zone. I will also discuss some potential implications for planet formation.

Speaker: Anna Császár (ELTE, HUN-REN CSFK CSI)

Anna_Csaszar_FIKUT_2026.pdf

Conference Photo

12:30 Lunch Break

Planetary Systems, Exoplanets, and Habitability

Convener: Zsolt Sándor (Eötvös Lorand University Department of Astronomy)

6 Exploring the dust properties of protoplanetary discs in ALMA Bands 1 and 10

Protoplanetary discs are the birthplaces of planets and small bodies, where small dust grains grow into larger particles during the early stages of planet formation. Observations at millimeter and submillimeter wavelengths can trace this dust, study its distribution within the disc, and investigate the conditions under which dust grows. The Atacama Large Millimeter/submillimeter Array (ALMA) provides observations across these wavelengths. I will present preliminary results from ALMA Band 1 (43 GHz) and Band 10 (872 GHz) continuum observations of a few protoplanetary discs in the Ophiuchus molecular cloud (2024.1.00253.S; PI: L. Cieza). The data are reduced and calibrated in phase and amplitude using the Common Astronomy Software Applications (CASA) package, followed by continuum imaging in both bands. I will also show the estimated intensity radial profiles and discuss the variations in the emission observed at the two wavelengths. These preliminary results will later be incorporated into a broader multi-frequency analysis to investigate the dust properties and the amount of solid material available for planet formation.

Speaker: Botond Máté Marosi (Eötvös Loránd University)

ALMA_fikut.pdf

7 Hunting for lightning in protoplanetary disks

Studies of chondritic meteorites originating from the Solar System have revealed that chondrules - small, spherical silicate inclusions - can be formed by intense, rapid heating followed by rapid cooling. A viable explanation for their formation is that in the primordial stages of the protoplanetary disk electrical discharges or lightning can occur and cause melting of the different size dust grains and chemical interaction with the gas. Such lightning phenomena may occur due to charge separation in the disk. In the protoplanetary disk charge separation occurs inside pressure maxima or anticyclonic vortices.
In this talk I will show this phenomenon using hydrodynamical simulations. My results indicate that dust grains of different sizes present in the material of a protoplanetary disk become spatially separated. Assuming that dust grains of different sizes carry different electrical charges, this spatial separation can lead to energetic discharges, ie. lightning. Such short duration brightening events may reveal a novel phenomenon in planet formation.

Speaker: János Pető (HUN-REN Research Centre For Astronomy and Earth Sciences)

János_Pető_Presentation_FIKUT.pptx

8 Planetary Migration Revisited: Can the Back-Reaction from Solids Flip Disc Torques?

The migration of low-mass planets is governed by the interplay between gravitational torques from the gaseous and solid components of the protoplanetary disc. Performing 2D global hydrodynamic simulations in locally isothermal discs, we investigate the often-neglected back-reaction of solid material on gas dynamics across varying metallicities, Stokes numbers, and accretion efficiencies. Our results demonstrate that the combined effect of back-reaction and planetary accretion frequently flips total torques from negative to positive, particularly for Earth-sized embryos. To validate these findings, we performed simulations using Adaptive Mesh Refinement (AMR) to allow for self-consistent migration tracks. The observed changes in migration behaviour show qualitative agreement with our calculated torque trends. In metal-rich discs, standard linear scaling prescriptions fail for weakly coupled solid species, as feedback-driven gas perturbations in the co-orbital region heavily modify the gas torques. We conclude that including solid back-reaction is essential for accurate migration modelling.

Speaker: András Németh (Eötvös Loránd University)

FIKUT_András_Németh.pdf

9 Time-Domain Complementary Science with Ariel: Young Stellar Objects, Debris Discs and Exocomets

Young stellar objects (YSOs) exhibit variability over a wide range of timescales and amplitudes, driven by stellar activity, variable extinction and disc accretion. Disentangling these processes remains challenging, yet their variability provides key insights into stellar mass assembly and the evolution of young planetary systems. The broad wavelength coverage and spectroscopic capabilities of the Ariel space mission offer a unique opportunity to extend its scientific return through time-domain observations of variable circumstellar environments.

We investigate Ariel's potential for complementary observations of a representative sample of YSOs and planetary systems exhibiting transient extinction phenomena. As a first step, we perform scheduling simulations to assess the cadence and integration times available for complementary targets. We then use preliminary instrument performance simulations to estimate the achievable signal-to-noise ratio across Ariel's wavelength range for representative sources. Particular attention is given to both quiescent and outbursting YSOs, where structural changes in the inner disc drive pronounced photometric and spectroscopic variability. Ariel's 1–8 $\mu$m coverage is especially sensitive to hot dust near the inner disc rim, while longer wavelengths probe cooler material and trace changes in disc structure.

We also examine complementary science cases involving transient dust-producing events. Extreme debris discs exhibit strong warm-dust emission and significant infrared variability, making multi-epoch Ariel observations well suited to tracking the evolution of dust emission and composition following catastrophic planetesimal collisions. In addition, radiative-transfer modelling indicates that the wavelength dependence of exocomet transit signatures can constrain dust composition and grain-size distributions, providing new insights into the physical processes governing these events. Such signatures are expected to be detectable with Ariel.

Our results provide a first assessment of Ariel's potential for time-domain complementary science beyond its core exoplanet programme, demonstrating how repeated photometric and spectroscopic observations can probe accretion, dust evolution, and transient phenomena in young planetary systems.

Speaker: Nóra Takács (HUN-REN CSFK Konkoly Observatory)

NoraTakacs_ArielCS_YSO_Exocomets.pptx

10 Developing a Protocol for establishing the methodology of Lunar Construction

The development of sustainable lunar infrastructure requires construction materials that can withstand extreme temperature variations and persistent radiation exposure while reducing dependence on Earth-supplied resources. Materials intended for in situ resource utilisation (ISRU), including polymers, metallic composites, aerogels and lunar regolith analogues, must be evaluated under relevant environmental conditions to determine their suitability for long-term lunar operations. However, systematic assessment requires a reproducible methodology that integrates environmental simulation, material characterisation and predictive modelling.
This research aims to develop a protocol for evaluating the response and durability of candidate lunar construction materials under simulated lunar environmental conditions. The proposed methodology combines ion irradiation experiments, thermal cycling, and post-exposure characterisation to investigate radiation-induced damage and thermally driven structural changes. Spectroscopic and microscopic techniques are used to assess chemical and morphological changes, while complementary modelling approaches provide insight into the underlying atomistic mechanisms.
A key objective is to establish a systematic framework for selecting relevant exposure conditions, defining experimental parameters, characterising material changes and comparing the responses of different material classes. Particular attention is given to the effects of radiation and thermal cycling, both individually and in combination, to identify potential degradation mechanisms and evaluate their implications for material performance.
Building on previous atomistic simulations of space materials under lunar-like thermal conditions, this work seeks to integrate experimental observations and computational modelling into a consistent assessment methodology. The resulting protocol is intended to support the comparative evaluation of ISRU-relevant materials and inform material selection and radiation-mitigation strategies for future lunar habitats.

Speaker: Adrija Bhowmick (HUN-REN Atomki, Debrecen, Hungary)

15:15 Coffee break

Visiting the Svábhegy Observatory

Announce_1104_afternoon.pdf

Thursday 5 November

Astrochemistry and Nuclear Astrophysics

Convener: György Gyürky (HUN-REN Institute for Nuclear Research (ATOMKI), Debrecen, Hungary)

11 Radiation-Driven Sulphur Chemistry on the Surfaces of Jupiter's Galilean Moons: New Results from Laboratory Experiments

The cycling of sulphur on the surfaces of Jupiter’s Galilean moons (i.e., Io, Europa, Ganymede, and Callisto) is a key process that may be directly linked to the putative habitability of these moons. This process is largely driven by ionising radiation from Jupiter’s sulphur-rich magnetosphere. Despite the astrochemical and astrobiological importance of sulphur cycling and chemistry on the surfaces of the Galilean moons, there is still much that remains unknown regarding this radiation-driven chemistry. For instance, the source of the solid sulphur dioxide (SO$_2$) observed on the surfaces of Europa and Ganymede is still not known with any certainty, despite the first detection of this species on these moons having been made $\sim$45 years ago. Moreover, the physical and chemical processes involving this solid surface SO$_2$ that are triggered by its interaction with magnetospheric radiation have yet to be accurately quantified, therefore limiting our understanding of sulphur surface and near-surface cycling (and its astrobiological implications) on the Galilean moons.

In this presentation, I will outline recent experimental work performed in the Space Chemistry Group at the HUN-REN Atommagkutató Intézet aimed at addressing some of the unresolved questions regarding the radiation-driven cycling of sulphur on the Galilean moons. Following a contextual introduction to the problem, experiments that were performed to test whether the implantation of sulphur ions from Jupiter’s magnetosphere into the surface ices of Europa and Ganymede could contribute to the SO$_2$ observed there, will be described. This will be followed by a discussion on an alternative mechanism for the radiolytic synthesis of SO$_2$, namely the irradiation of icy surface components in the presence of elemental sulphur, and experiments carried out to determine whether such a mechanism is reasonable in the context of Europa and Ganymede. Finally, new (preliminary) results on the physical and chemical processes triggered in solid SO$_2$ at low temperatures as a result of its interaction with ionising radiation will be shared.

Speaker: Duncan Mifsud (HUN-REN Atommagkutató Intézet)

Duncan_V_Mifsud_FIKUT NEXTGEN Presentation (20261105).pdf

12 Irradiation of Methanol Ices as an Analogue for Astrochemical Processes

Ices are observed across the universe, including on planetary bodies, comets, within the interstellar medium (ISM), and in protoplanetary disks [1]. In these environments are subjected to a flux of UV irradiation, electron bombardment, cosmic rays bombardment, solar wind and thermal chemistry, which drive structural modifications, induce the desorption of molecules and radicals from the grains, and generate new species through radiolytic processes [2].

One of the most important constituents of these ices is methanol (CH3OH), which could have originated from surface interactions occurring in the ice mantles on the grains and is a key component in radiolytic processes due to its significant abundance in comets, in dense clouds, around low mass protostars, and around massive protostars [3]. For this reason, if this compound survived the impact processes during accretion, it would have contributed substantially to the geological and chemical evolution of large icy bodies.

Considering the above and the importance of analysing the chemical evolution of ices in the interstellar medium and and on the surfaces of planetary bodies, in this project, we simulate the conditions from icy moons, especially Enceladus surface and irradiate ices of methanol in order to analyse the changes that take place.

This project is titled “Systematic Studies of Astrophysical Ices and Materials within Simulated Space Environments” and is being carried out at the Ice Chamber for Astrophysics/Astrochemistry (ICA) at the Tandetron Accelerator, operated by the HUN-REN Institute for Nuclear Research in Debrecen under the supervision of Professor Nigel J. Mason.

In this project, we experimentally investigate how methanol ices respond to proton irradiation (simulating solar wind conditions) at different energies (250 keV, 500 keV, 750 keV, and 1 MeV). For this purpose, in an ice chamber maintained under high-vacuum conditions (10⁻⁹ mbar), we deposit methanol ices at different temperatures, obtaining crystalline ice at 130 K and amorphous ice at 20 K. Subsequently, we irradiate the samples with the required proton energy, and the infrared spectrum is obtained.

Using these infrared spectra, we proceed with the identification and quantification of the products formed by irradiation (carbon monoxide, carbon dioxide, methane, and formaldehyde), as well as the estimation of the amount of methanol destroyed during the process.

Finally, in this project we also investigates the structural changes that take place in crystalline ice when exposed to radiation through a process known as amorphization. This process is of great importance for understanding the chemical evolution of these ices on icy moons such as Enceladus, where material ejected through cryovolcanic plumes is deposited onto the surface and subsequently exposed to radiation.

These findings enhance our understanding of how ices affect the formation of icy moons and their chemical evolution and may help interpret data from upcoming space missions like JUICE.

                        References.

[1] Dartois, E., et al. Heavy ion irradiation of crystalline water ice Cosmic ray amorphization cross-Section and sputtering yield. Astronomy & Astrophysics 576 (2015).

[2] Boogert, AC. Adwin, Perry A. Gerakines and Douglas CB Whittet. Observations of the icy universe. Annual Review of Astronomy and Astrophysics 53.1 (2015):541-581.

[3] Cruz-Diaz, Gustavo., et al. Negligible photo desorption of methanol ice and active photon-induced desorption of its irradiation products. Astronomy & Astrophysics. 592. (2016): A68.

Speaker: Rodrigo Zamudio Ramírez (University of Debrecen / HUN-REN ATOMKI)

136. Rodrigo Zamudio - FIKUT NEXTGEN.pdf

13 Uncovering the importance of (p,n) reactions in the weak r-process

Nucleosynthesis above the iron region mainly proceeds via successive neutron capture processes, such as the s- and r-processes. However, in the case of neutrino-driven ejecta from a core-collapse supernova, nucleosynthesis runs relatively close to the valley of stability, hence it proceeds mainly via (α,n) and (p,n) reactions towards higher mass numbers [1]. Sensitivity studies have shown that (α,n) reaction uncertainties can be up to an order of magnitude, mainly due to differences in α-nucleus optical model (αOM) potentials [2]. This nuclear uncertainty significantly impacts network calculations and calculated abundances [3,4].

Therefore, substantial effort has been devoted to measuring key (α,n) reactions that influence the weak r-process. These measurements have also been used to justify the adoption of a new αOMP, ATOMKI-V2 [5]. However, our latest reaction network study carried out with WinNet suggests that the impact of (p,n) reaction uncertainties should not be so easily disregarded as has been done so far. In this presentation, we will share details on our reaction network studies, the application of ATOMKI-V2, the significance of (p,n) reactions, and the astrophysical implications of our latest experimental data [6,7].

[1] A. Arcones and F. Montes, ApJ, 731 5 (2011).
[2] J. Pereira and F. Montes, Phys. Rev. C, 93 034611 (2016)
[3] J. Bliss, A. Arcones, F. Montes, and J. Pereira, Phys. Rev. C, 101 055807 (2020)
[4] A. Psaltis et al., ApJ, 935 27 (2022)
[5] P. Mohr et al., Eur. Phys. J. A, 61 89 (2025)
[6] G. G. Kiss et al., ApJ, 988 170 (2025)
[7] S. R. Kovács, submitted to ApJ

Speaker: Sándor Kovács (HUN-REN ATOMKI)

SRKovacs_FIKUT.pptx

14 Stellar nucleosynthesis in the laboratory: LUNA results and perspectives

The energy production, chemical evolution and elemental abundances of stars are governed by thermonuclear reactions occurring at energies far below the Coulomb barrier. Measuring their cross sections is the central challenge of experimental nuclear astrophysics: at stellar energies the Coulomb repulsion suppresses the cross sections by many orders of magnitude, down to the picobarn-femtobarn range, so that cosmic-ray and environmental backgrounds become the limiting factor. At LUNA (Laboratory for Underground Nuclear Astrophysics), located under 1400~m of rock at the INFN Gran Sasso National Laboratory (Italy), the cosmic-ray background is suppressed by several orders of magnitude, making it possible to reproduce in the laboratory the reactions that take place in stars. I will introduce the LUNA project and its role in astrophysics through a selection of landmark measurements. I will then focus on two crucial reactions of the CNO cycle: 19F(p,ag)16O and 19F(p,g)20Ne. The ratio between the two channels determines whether material is recycled within the CNO cycle or leaks towards the Ne-Na region, with consequences for the fluorine abundance and for the nucleosynthesis in AGB stars, massive stars and novae. I will present the recent results for the (p,ag) channel. Finally, I will outline the scientific perspectives of LUNANOVA, the recently awarded ERC Synergy Grant, which will open new frontiers for underground nuclear astrophysics.

Speaker: Riccardo Biasissi (Università degli Studi di Padova, ATOMKI)

FIKUT_Biasissi.pdf

15 Measurement of the 14N (p, γ) 15O Reaction Cross Section Using Inverse Kinematics

The CNO cycle plays a paramount role in the evolution of massive stars. Above 1.3 solar masses, the CNO cycle becomes the dominant energy-generation mechanism, overtaking the role of the proton-proton chain. In the CNO cycle, carbon and nitrogen isotopes act as catalysts, helping the fusion of hydrogen into helium.
The reaction rate of the entire cycle is governed by its slowest reaction, the 14N (p, γ) 15O, which has the smallest cross section among the reactions in the cycle. Since several astrophysical parameters are depending on the rate of the cycle – including the ages of the oldest globular clusters and indirectly, the age of the Universe – its precise determination is of particular importance in nuclear astrophysics.
At astrophysically relevant energies, this reaction has an extremely low probability. Thus, reducing the natural background in the detection system is critical for a precise measurements, as the radiation produced by the reaction would be undetectable in the presence of a high background. For this reason, previous in-beam gamma-ray spectroscopy measurements have been carried out at ultralow-background facilities, including the underground laboratory of the LUNA collaboration beneath the Gran Sasso Mountain in Italy and a similar facility used by the JUNA collaboration in Jinping, China. In addition, valuable information can be obtained at the Earth's surface using the activation technique, which measures the radioactivity of the produced 15O. The feasibility of this approach has already been demonstrated at ATOMKI.
Building on the results of previous ATOMKI experiments, our measurements employ a new, alternative approach to determine the reaction cross section: inverse kinematics, in which a hydrogen-containing target is bombarded with 14N ions. This method avoids high-energy proton activation, thus preventing the unwanted radioactivity of the measurement environment, and substantially reduces the in-beam gamma-ray background.
To date, we have used thick targets, pressed from titanium hydride powder, in our measurements. Cyclic irradiation was employed, where the prompt gamma-rays from the reaction was detected during the irradiations, while the radioactivity of the produced 15O was measured independently in the off beam periods. This demonstrates the feasibility and usefulness of cross-validation of the two methods. To improve measurement accuracy, we are refining the preparation techniques for thick targets. In parallel, the production of thin targets, with thicknesses of a few tens of nanometres, is underway using a plasma sputtering system.
Following our preliminary measurements at ATOMKI, we plan to continue our research at an underground laboratory to reach even smaller bombarding energy and cross section regions. This would enable a precise determination of the cross section at astrophysical energies and, consequently, the CNO-cycle reaction rate. The improved accuracy may help refine estimates of the age of the Universe and our understanding of the Sun's core composition.

Speaker: Gábor Bihari (HUN-REN ATOMKI)

Gábor_Bihari_FIKUT előadás2.pdf

16 Silicon nucleosynthesis in classical novae: New experimental constraints on the 29Si(p,γ)30P reaction

Classical nova explosions contribute to the chemical enrichment of the inter-
stellar medium and are potential sources of presolar grains found in primitive
meteorites. The silicon isotopic ratios 29Si/28Si and 30Si/28Si provide im-
portant signatures for identifying the stellar origin of these grains [1, 2].
However, uncertainties in nuclear reaction rates limit our ability to establish
the nova paternity of these grains. In particular, the 29Si(p,γ)30P reaction
influences silicon isotopic abundances and the production of 30P [3, 4].

While considerable progress has been made in determining the strengths of
astrophysically important resonances [5, 6], the nonresonant contribution
to the 29Si(p,γ)30P cross section has not been experimentally investigated
before. We measured this contribution for the first time at four proton
energies between 1.0 and 1.43 MeV, using the activation technique.

The nonresonant astrophysical S-factors calculated from the measured cross
sections are a factor of 4.3 ± 0.6 higher than previous theoretical direct-
capture component predictions [5]. Although the nonresonant contribution
becomes dominant only at temperatures below approximately 30 MK, this
discrepancy may indicate a limitation in the existing theoretical descrip-
tion. Our results provide new experimental constraints for calculating the
29Si(p,γ)30P reaction rate and motivate further investigations of nonresonant
proton capture in this mass region. Ultimately, improved nuclear reaction
rates will help refine predictions of silicon isotopic abundances and their
interpretation in presolar grains.

REFERENCES
[1] J. José et al., Astrophys. J. 612, 414 (2004).
[2] L. N. Downen et al., Astrophys. J. 928, 128 (2022).
[3] C. Iliadis et al., Astrophys. J. Suppl. Ser. 142, 105 (2002).
[4] J. José et al., Astrophys. J. 560, 897 (2001).
[5] L. N. Downen et al., Phys. Rev. C 105, 055804 (2022).
[6] Zs. Mátyus et al., Eur. Phys. J. A 60, 218 (2024).

Speaker: Zsolt Mátyus (HUN-REN INSTITUTE FOR NUCLEAR RESEARCH)

Mátyus_FIKUT_NEXTGEN_2026.pdf

10:30 Coffee break

Compact Objects, Relativistic Astrophysics, and Gravitational Waves

Convener: Dr Gergely Barnafoldi (HUN-REN Wigner Reseach Centre for Physics)

17 Characteristic Gluing and Conserved Charges in General Relativity

This work studies the characteristic gluing problem in asymptotically flat spacetimes. In particular, it investigates the conditions under which initial data on different null hypersurfaces can be glued together to form a solution of the Einstein equations. The main focus is on the obstructions to such a gluing construction and their interpretation in terms of conserved quantities. Within the Bondi–Sachs formalism, two families of radially conserved charges are derived from the null constraint equations and identified as gauge-invariant gluing obstructions. Their relations to ADM and BMS charges are investigated, and further gauge-dependent obstructions are discussed.

Speaker: Zita Csapó (Wigner RCP, ELTE)

csz_fikut_slides.pdf

18 Charged black holes in higher dimensional supergravity

This project investigates analytical and numerical black hole solutions in Anti-de-Sitter spacetimes. These geometries are of particular interest due to their holographic interpretation in gauge/gravity duality, representing states of a strongly coupled N=4 super Yang-Mills theory with a large number of colors, residing on a three-sphere. First, we derive the equations of motion from a supergravity action that descends from a consistent truncation of IIB supergravity on a five-dimensional sphere. Furthermore, exact solutions for a constant scalar field are obtained, yielding geometries such as the pure AdS and the Bertotti-Robinson spacetime. For non-trivial scalar field configurations, a computational code is constructed in Mathematica, which numerically integrates the differential equations, relying on a strictly analytical Taylor series expansion to determine the boundary conditions just outside the black hole event horizon. The numerical results demonstrate that the solutions are asymptotically AdS far from the horizon. To study this asymptotic behavior further, we apply the Fefferman-Graham expansion near the AdS boundary. Finally, a thermodynamic analysis is performed by calculating the physical Bekenstein-Hawking entropy density and the Hawking temperature.

Speaker: Nefeli Chatziioannou (University of Crete)

charged black holes.pptx

19 Continuous Gravitational Waves from Supermassive Black Hole Binaries

We investigate the prospects for detecting nanohertz gravitational waves from individual supermassive black hole binaries (SMBHBs) using pulsar timing arrays (PTAs). We review the formation and gravitational radiation of SMBHBs, the principles of pulsar timing, and the current observational capabilities of PTAs, with particular emphasis on the expected sensitivity improvements offered by the Square Kilometre Array (SKA). Using electromagnetic observations to estimate the gravitational-wave parameters of four SMBHB candidates—OJ 287, 3C 66B, NGC 5548, and S5 1928+738—we calculate their expected strain amplitudes and signal-to-noise ratios for several future PTA configurations. Our sensitivity forecasts indicate that, under idealized white-noise assumptions and the adopted binary models, gravitational waves from OJ 287, 3C 66B, and NGC 5548 could exceed the nominal detection threshold of the SKA. S5 1928+738 may also become detectable with sufficiently sensitive configurations. Furthermore, comparison with a larger population of electromagnetically identified SMBHB candidates suggests that numerous additional sources could approach or exceed the SKA detection threshold. These results highlight the potential of the SKA to detect continuous gravitational waves from multiple individual SMBHBs, opening new opportunities for multimessenger astronomy and for understanding the formation and evolution of supermassive black holes.

Speaker: Richárd Tamás Varga (University of Szeged)

Richard Varga Continuous Gravitational Waves from Supermassive Black Hole Binaries.pdf

20 Imaging Parallel Universes via Kerr Black Holes: Observational Tests of Cauchy Horizon Instability

Black holes can connect different regions of spacetime: in the Kerr solution, geodesics may pass through or around the ring singularity without destruction. Although perturbations are thought to destabilize such passages by generating additional singularities, their possible existence has direct observational consequences. We show that if Sgr A or M87 is described by the maximally extended Kerr geometry, the Event Horizon Telescope (EHT) could detect photons originating from a second asymptotic region or the Cauchy horizon. Such photons would appear to emerge into our universe from within the black hole shadow. Tracing light rays in the extended Kerr spacetime defines a map between the observers image plane and the source-sky of the photons. Features of this map provide observational templates for searches in current and future EHT data, offering a direct test of whether astrophysical black holes realize the global Kerr extension or whether the Cauchy horizon instability precludes such passages.

Speaker: Dávid Szepessy (ELTE Fizika Doktori Iskola)

KFKI_Wigner_FIKUT_eloadas_Szepessy.pdf

21 Modelling Neutron Stars in Scalar-Tensor Theories

In this work, we model slowly rotating neutron stars in massive scalar-tensor gravity, focusing on the massive Damour-Esposito-Farese model. Scalar-tensor theories of gravity with a dynamical scalar field coupling non-minimally to matter via a conformal factor $A(\phi)$ pose computational challenges beyond standard general relativistic solvers. In this theory, matter is coupled to an additional scalar field, and sufficiently compact stars can undergo spontaneous scalarization, where the scalar field grows inside and around the star and changes its macroscopic properties. It is implemented within the Hartle slow-rotation expansion at first-order.

We solve the stellar structure equations using the APR equation of state, interpolated via PCHIP in geometrized units throughout and a shooting-based numerical scheme using the Nelder-Mead optimizer. Two numerical improvements are introduced. First, the outer boundary condition is chosen to match the expected Yukawa decay of a massive scalar field, leading to a Robin boundary condition that strongly reduces sensitivity to the finite outer boundary. Second, the stellar surface is recalibrated using energy-density gradients and sequence-based smoothing, improving radius-dependent observables while preserving genuine physical peaks.

Using this framework, we compute mass-radius relations, central-density sequences, moments of inertia, and other stellar profiles for different scalar coupling strengths and scalar masses. We find that stronger coupling and lighter scalar fields produce the largest deviations from general relativity, including higher masses and modified radii. These results show that accurate boundary treatment and surface identification are essential for robust predictions of scalarized neutron stars and for connecting scalar-tensor gravity to future astrophysical observations.

Speaker: Ashika Achuthankutty (University of Szeged and HUN-REN Wigner RCP)

Ashika_AchuthankuttyFIKUT NEXTGEN.pdf

22 Radioactive isotopes as power sources in the late-time evolution of core-collapse supernova light curves

Massive stars end their hydrostatic evolution in energetic explosions known as core-collapse supernovae (CCSNe), synthesizing and ejecting intermediate-mass and iron-peak isotopes into the interstellar medium. Following the initial explosion, CCSNe can be observed for several hundred days, powered primarily by the radioactive decay of newly synthesized radioactive isotopes, mainly associated with Ni. In this study, I analyze the light curves of 10 observed CCSNe to compare two different theoretical modeling approaches. For light curves extending beyond 500 days, I utilized an upgraded version of an open-source Python-based fitting code to model late-time light curves and determine the isotopic yields driving their radioactive tails. This approach allows the examination of the late-time emissions and facilitates direct comparisons with 1D CCSN models developed in recent decades. To make accurate long-term light curve predictions, tighter constraints on isotopic ratios like 44Ti/56Co and 60Co/56Co are required. For this, I utilized a hydrodynamic evolution code to fit the plateau phase of the observed light curves, enabling the calculation of the resulting explosive nucleosynthesis yields. From the synergy of these observational and theoretical approaches, we can better understand explosion dynamics and mixing mechanisms and establish robust constraints for future supernova research, bridging the gap between photometric observations and explosive CCSN nucleosynthesis.

Speaker: Gábor G. Balázs (Konkoly Observatory, HUN-REN CSFK)

fikut_BGG.pdf

12:30 Lunch Break

Cosmology, Galaxies, and Large-Scale Structure

Convener: Krisztina Gabanyi (Departments of Theoretical and Experimental Physics, University of Szeged)

23 Searching for extra dimensions in neutron stars and black holes

In the Kaluza–Klein theory, one extra spatial dimension is added to usual spacetime. On one hand, particles moving in it gain excitations leading to a mass spectrum, which can be associated with hadronic states. Neutron stars are modelled using the equation of state of an extra-dimensional interacting zero-temperature Fermi gas. Macroscopic observables are calculated, compared to astronomical data, and a range of extra dimension sizes with the possibility of detection is given [1].

On the other hand, the extra dimension introduces a scalar field into the theory, which modifies the curvature of spacetime. On a curved background, the uncertainty relation of particles is modified, resulting in a modified dispersion relation and thermodynamics. Such effects become significant near the horizon of black holes, where even gravity induced particle decay is possible [2].

[1] A. Horváth, E. Forgács-Dajka, G.G. Barnaföldi: "Application of Kaluza-Klein Theory in Modeling Compact Stars: Exploring Extra Dimensions", MNRAS https://doi.org/10.1093/mnras/stae2637 (2024)
[2] A. Horváth, A. Wojnar, GG. Barnaföldi: "Modified Dispersion Relation in Kaluza–Klein Theory". Particles. 2026; 9(3):87. https://doi.org/10.3390/particles9030087

Speaker: Anna Horváth

AnnaHorvath_fikut26.pdf

24 Long-term gamma-ray variability and multimessenger activity of the blazar GB6 J1542+6129

Blazars are promising candidate sources of high-energy astrophysical neutrinos, but the location of neutrino production in blazars remains uncertain. In our study (Kun et al. 2026), we investigate the temporal connection between a suspected IceCube neutrino flare and the gamma-ray and radio emission of the blazar GB6 J1542+6129. We performed a likelihood analysis of 17 years of Fermi-LAT data and constructed a gamma-ray light curve to investigate the temporal relationship between the gamma-ray emission, the suspected neutrino flare, and the VLBI core activity. The analysis combines these gamma-ray observations with approximately 14 years of Very Long Baseline Interferometry (VLBI) data from the MOJAVE programme. The suspected neutrino flare precedes both a gamma-ray flare and an increase in the inferred Doppler factor of the VLBI core by up to approximately one year. Furthermore, the duration of the subsequent gamma-ray activity is comparable to that of the neutrino flare. These temporal relationships are consistent with a scenario in which neutrinos originate in a compact, photon-rich region upstream of the parsec-scale radio core, while a propagating disturbance subsequently enhances the electromagnetic emission as it reaches the radio core. This study demonstrates the potential of time-domain multimessenger observations to constrain the location of neutrino production in active galactic nuclei.

Speaker: Anna Göblyös (Szegedi Tudományegyetem)

fikutnextgen_GoblyosAnna.pdf

25 Nonequilibrium thermodynamics and gravity in astrophysics

The methods of nonequilibrium thermodynamics allow the proper handling of local specific gravitational energy of a self-gravitating fluid. The hydrodynamic framework allows various models to be integrated, for example the Ohanian form of gravitational energy density, which is thermodynamically distinguished. The resulting field equations also allow a thermodynamic coupling to exist, which results in a modified Poisson's equation. This result is investigated in relation to astrophysical phenomena, such as galactic rotation curves, which are usually attributed to dark matter instead.

Speaker: Máté Pszota (Wigner RCP, Eötvös University)

fikut26.pptx

26 Escaping the torus of numerical cosmology

Almost every cosmological simulation of the past four decades has been run in a periodic cube. The choice is so universal that it is rarely stated as an assumption, yet it is one: it gives the simulated universe the topology of a $3$-torus. But what that assumption costs us and how to deal with the problems it introduces? A cube is not rotationally symmetric, so angular momentum is not conserved. The sum over infinitely many periodic images makes the gravitational force deviate from Newton's law in a direction-dependent way. The discrete set of allowed wavelengths cuts off large-scale power differently along different directions. None of this is motivated by observations. Why did the torus nevertheless became the standard? In what scenarios can we expect its artefacts to matter? What should a better, alternative simulation topology provide? As an example we present the first $\Lambda$CDM simulations in a spherical, cylindrical, and dodecahedral topologies, in which the cosmic web forms as expected from observations.

Speaker: Balázs Pál (Wigner Research Centre for Physics)

pal-balazs-fikut-nextgen-2026-11-05.pdf

27 Neutral hydrogen — star formation relationship in a nearby low-surface brightness galaxy

Areas of massive star formation are heavily affected by stellar winds and supernovae, therefore we expect enhanced turbulent flows in such regions. I present kinematic properties in dwarf galaxy DDO 43 (d = 7.8 Mpc), revisiting the high-resolution HI 21-cm VLA spectra of the LITTLE THINGS survey. The line profiles are carefully analysed in the CLASS radioastronomical data reduction software, and the resulting distribution maps of spectral line properties are investigated together with available GALEX and WISE data, to provide additional insights to the characteristics of local and global neutral gas flows in massive star forming regions.

Speaker: Enikő Pichler (University of Debrecen)

FIKUT26_HI-SF_in_faint_dwarf_PichlerEniko.pdf

15:15 Coffee Break

Cosmology, Galaxies, and Large-Scale Structure

Convener: Krisztina Gabanyi (Departments of Theoretical and Experimental Physics, University of Szeged)

28 Observational effects on cosmic voids

The cosmic web of galaxies carries information about the growth and expansion history of the universe. Mapping the large-scale structure of the universe is the main goal of several current galaxy surveys, while also providing insights about the nature of dark matter and dark energy, which make up 95% of the universe.
Cosmic voids are huge underdense regions in the galaxy distribution that are especially sensitive to dark energy, but their statistical analysis is challenging due to the sparse sampling of galaxies. Observations of galaxies are less pristine than simulations, due to observational effects such as survey completeness or redshift errors - which can further bias the void statistics and the inferred cosmological parameters, too.
I am focusing on cosmic voids at the time of the cosmic noon (redshift 1<z<2), which refers to the peak of structure formation, right before dark energy begins dominating the dynamics of the universe. Utilizing simulations, I study the effects of different observational errors on cosmic void statistics in this redshift range. Exploring these systematic effects will help us reconstruct more unbiased cosmologies.

Speaker: Júlia Katona

Julia_Katona_FIKUT_2026.pdf

29 The impact of central supermassive black holes on the gas content of galaxy groups in IllustrisTNG

The large-scale structure of the Universe has been primarily shaped by the gravitational collapse of dark matter. On the largest scales, galaxies are distributed across galaxy groups, galaxy clusters, and filaments which surround vast cosmic voids. My work focuses on systems with masses in the range of 1012 - 1014 M☉. Although less massive than galaxy clusters, these structures are much more common, thus contributing significantly to the overall matter distribution of the Universe.

Feedback processes, primarily driven by active galactic nuclei (AGN), counteract the effects of gravitational collapse by redistributing baryonic matter within their host dark matter halos. In galaxy groups, AGN feedback can eject gas beyond the virial radius of the host halo. Due to the complexity of the underlying gravitational and hydrodynamic processes, the evolution of these systems cannot be fully described by analytical models alone, making numerical simulations essential. In this project, I use the state-of-the-art IllustrisTNG cosmological simulation, which models the gravitational evolution of dark matter alongside the evolution of baryonic matter, including gas, stars, and black holes, while accounting for hydrodynamics, star formation, and feedback processes.

This project investigates how the supermassive black hole at the center of the host halo affects the gas content of galaxy groups and their dynamical evolution. To address this question, I analyse the relationship between gas mass and halo mass in galaxy groups from the IllustrisTNG-300 simulation, taking into account the mass of the central black hole. The evolution of the gas mass fraction points to gas ejection in both low- and high-mass galaxy groups; however, in more massive halos, previously expelled gas appears to undergo reaccretion. I compare my results with previous studies based on the Magneticum and FLAMINGO simulations, looking for similarities and differences across different halo mass ranges.

Speaker: Agnes Bogdan (ELTE)

Fikut.pdf

30 VLBI imaging of sub-kiloparsec-scale dual AGN candidates in merger systems

Dual active galactic nuclei (AGN) play a crucial role in understanding supermassive black hole growth and evolution in merger systems. The milliarcsecond resolution provided by Very Long Baseline Interferometry (VLBI) is indispensable for resolving these closely separated systems. In this talk, I will present the high-resolution VLBI imaging investigations of two sub-kiloparsec-scale dual AGN candidates: MCG-03-34-64 and UGC 4211. No dual compact radio core structures were detected, and both targets exhibit core-jet morphologies. The multi-wavelength analysis of the VLBI-detected nuclei provides unique insights into the black hole accretion state and jet launching in such dusty and highly obscured merger environments. In addition, I will mention the radio survey cross-matching and detectability results for recently published samples of dual AGN candidates.

Speaker: Wancheng Xu

FIKUT NEXTGEN.pptx

Astronomical Instrumentation, Observational Techniques, and Space Plasma Physics

Convener: Sándor Frey (Konkoly Observatory, HUN-REN CSFK)

31 Stellar Intensity Profiles with Synspec for Ariel Transit Modeling

This work presents a methodology for computing stellar intensities using the Synspec software, providing the foundation for deriving more accurate limb-darkening coefficients (LDCs) for exoplanet-characterization space missions such as ESA's Ariel. Because exoplanetary transit light curves are sensitive to the center-to-limb intensity variation of the host star, precise LDCs are critical for mitigating systematic degeneracies in both stellar and planetary parameterization. Utilizing these Synspec-derived intensity profiles will allow us to derive more precise LDCs and eventually modelling the light curves more accurately.

Speaker: Borbála Nagy (Eötvös Loránd Tudományegyetem)

FIKUT_Nagy_Borbála_2026.pptx

32 Tracing Radial-Velocity Drift in the ACE Spectrograph: Instrumental Stability and Environmental Effects at Piszkéstető

Through the investigation of radial-velocity measurements of standard stars, we study the stability of the ACE fiber-fed échelle spectrograph at Piszkéstető and how instrumental and environmental effects influence the measured radial velocities. Understanding these effects is important in stellar spectroscopy, since systematic shifts in the measured spectra can affect the velocities derived from observations and consequently the physical conclusions obtained from them. Our work consisted of identifying which factors can contribute to these inaccuracies. Using existing data, conducting our own observations, and a physical site visit to inspect the spectrograph, we were able to identify a considerable drift.

We benchmarked our measurements against the well-known radial velocities of standard stars and used piszkespipe, a spectral-reduction pipeline specifically developed for the spectrograph, to obtain the radial velocities, which we then compared with the reference values to calibrate the instrument and account for any drift. Furthermore, suspecting the existence of same-night systematic drift due to environmental factors, we studied the individual and combined effects of different environmental factors such as humidity, atmospheric pressure, and temperature, both indoors and outdoors. We found a global zero-point offset of approximately +0.50 km/s, which can be corrected consistently, while we also found evidence that environmental factors affect the measured radial velocities. However, we were not able to find a reliable correction that worked across all stars and nights. Following the identification of two anomalous observing nights, we also investigated atmospheric seeing as a potential contributor to the observed radial-velocity deviations.

Speakers: Mohamed OUKLILENE (Budapest University of Technology and Economics), Mr Yazdan Mostajabaldaveh (Budapest University of Technology and Economics)

Astro-Presentation-Final.pdf

17:00 Coffee break

Astronomical Instrumentation, Observational Techniques, and Space Plasma Physics

Convener: Sándor Frey (Konkoly Observatory, HUN-REN CSFK)

33 Testing shock jump predictions using THEMIS observations

After crossing the bow shock and entering the magnetosheath, the solar wind experiences substantial modifications: plasma
temperature, magnetic field strength, and particle density increase significantly, while the flow velocity decreases and its
direction is deflected. Magnetohydrodynamic (MHD) theory provides quantitative predictions for the changes in these
plasma parameters across the shock transition. The THEMIS spacecraft constellation, operating on comparable orbital
trajectories, offers an excellent platform for testing these MHD bow shock jump conditions through in situ magnetic field
and ion plasma observations. In this study, we investigated two events on 26 July 2007 and 2 September 2007, during which
one THEMIS spacecraft was located upstream of the bow shock in the pristine solar wind, while another spacecraft was
simultaneously positioned downstream within the magnetosheath. For both events, average values of plasma density,
magnetic field magnitude, and solar wind velocity were determined on either side of the shock. Shock normal vectors were
calculated using both Minimum Variance Analysis (MVA) and coplanarity techniques, applied consistently to the same
upstream and downstream intervals. Subsequently, the downstream-to-upstream ratios of magnetic field strength and solar
wind velocity were derived and compared with theoretical expectations.
Our results show good agreement with the Rankine–Hugoniot relations for both events, within the uncertainties associated
with the measurements.

Speakers: Abdul Rahuman Mohamed Nawrouse (University of Pecs, Pecs, Hungary), Dr Gabor Facsko (Wigner Research Centre for Physics, Department of Space Physics, Budapest, Hungary)

Abdul_Rahuman_Thesis_consul.pdf

34 LED testing strategy and optical optimisation of the THESEUS Infrared Telescope’s Calibration Unit

We present the Phase B planning of the Transient High-Energy Sky and Early Universe Surveyor (THESEUS) Infrared Telescope’s Calibration Unit, carried out during Phase A, with emphasis on LED-based calibration concepts and optical design considerations. The work outlines a structured testing strategy that combines individual device characterization with batch-level validation to ensure consistent and reliable performance. In parallel, we investigate how different LED configurations and mounting approaches influence the optical behavior of the system. Ray-tracing simulations are used to explore light propagation and assess potential systematic effects impacting calibration accuracy. By integrating planned experimental activities with simulation-driven studies, this work establishes a solid foundation for the development of a robust and well-characterized calibration unit in Phase B.

Speaker: Bendegúz Koncz (University of Debrecen, GTGM Kft.)

Bendegúz_KONCZ_FIKUT_2026_Theseus_LED_test.pptx

35 Mechanical Design Concept Challenges for the THESEUS InfraRed Telescope’s Calibration Unit

The InfraRed Telescope (IRT) aboard the proposed THESEUS mission requires a stable and well-characterised detector response to achieve its science objectives, particularly for the rapid localisation and redshift determination of high-energy transients. This is enabled by an internal Calibration Unit designed to provide spatially uniform and temporally stable near-infrared illumination throughout the mission lifetime, representing the second near-infrared LED-based calibration unit of its kind following Euclid’s Near-Infrared Calibration Unit (NI-CU).

We present the main challenges driving the mechanical design concept of the IRT Calibration Unit, including strict volume and mass limits, ease of manufacturing and assembly, and the need for structural rigidity and thermal stability. We discuss the solutions adopted to integrate an optical system capable of providing highly uniform illumination within the IRT-specific constraints.

Speaker: Mr András Péter Joó (ELTE / Konkoly-Thege Miklós Csillagászati Intézet)

THESEUS_fikut_irt-cu-mech-talk_joo_261104.pdf

Conference dinner

Announcement_11_05_afternoon.pdf

Friday 6 November

Planetary Systems, Exoplanets, and Habitability

Convener: Bálint Seli (HUN-REN CSFK, Konkoly Observatory)

36 Examining the biological effects of UV-C radiation on Drosophila melanogaster in relation to exoplanet habitability around flaring stars

Our project’s aim is to find out more information about the impact of UV-C radiation on multicellular organisms connected to space exploration and exoplanet habitability. It is an interdisciplinary collaboration between the fields of astronomy and biology. Through the examination of TESS and Kepler lightcurves of different flaring stars with exoplanets in their habitable zone, such as Proxima Centauri and TRAPPIST-1, several stellar flares can be identified and characterized. Using stellar spectral models, the UV-C radiation received by an exoplanet at its orbital distance during stellar flares can be estimated. These calculations provide the basis of our laboratory experiment, in which fruitflies (Drosophila melanogaster) are irradiated using a UV-C lamp. The biological effects of different doses of radiation on fruitflies can show intriguing new information about living systems’ reactions to UV-C radiation in connection with space exploration and exoplanet habitability.

Speaker: Veronika Napsugár Csillag (ELTE, HUN-REN CSFK CSI)

Csillag_Napsugár_FIKUT.pdf

37 Modeling liquid water-trapping micro-environments on the Martian surface

This presentation introduces a theoretical model that explores the
possibilities of how liquid water could persist on the surface of
Mars. Indeed, hygroscopic salt crystals found on the surface are
capable of binding atmospheric water vapor, thereby forming a liquid
solution. The main challenge is preserving these solutions in the
extremely dry daytime environment. The model is based on volume
changes caused by significant daily temperature fluctuations, which
generate internal stress and can cause cracks to form in the salt crystals.
As a result of low evening temperatures and the concomitant increase
in relative humidity, the deliquescent liquid can flow into an
internal cavity of the crystal; then, as the temperature rises during the day, the
cracks may close, thereby isolating the solution from the dry outdoor
environment. Based on a simulation run on Ca(ClO4)2 salt crystals, the
probability of liquid formation as deliquescence can reach as high as 100–130 sols on
average per year near Acidalia Planitia. An analysis of this process
reveals a strong correlation with surface thermal inertia (TI);
elucidating the underlying mechanisms could lead to a better
understanding of physical processes on Mars. To this end, a detailed
analysis of specific locations is of paramount importance to gain a
more precise insight into which factors play a role in this phenomenon
and to what extent.

Speaker: Anna Bognár (Konkoly Observatory, HUN-REN CSFK / Eötvös Loránd University)

Bognar_Anna_FIKUT.pdf

38 The mystery of Warm Jupiters

The formation of Warm Jupiters (with a period about 30 days and highly eccentric orbit (e > 0.3)) is still an open question. I investigated their possible early origins, ie. still embedded in the protoplanetary disk using numerical hydrodynamical simulations with the code GFARGO2. Assuming that planets are orbiting in the inner cavity of the disk, I found that planets can reach highly eccentric shrinking orbits. As a result, planets migrate under the Roche limit of the star and fall apart. This raises the question: is it possible for the planet to migrate into the cavity in the first place? Slight modification to the inner boundary condition of the hydrodynamic simulations allows the planet entering the inner cavity. However, in this case the eccentricity excitation stays moderate. My results indicate that further study requires the formation of Warm Jupiters.

Speaker: Katalin Nagy

FIKUT - The mystery of warm Jupiters.pptx

39 Refined Description of Slim Disks around Tidal Disruption Events

Tidal Disruption Events (TDEs) occur when a star gets too close to a black hole, and its gravitational pull tears the star apart. These events result in a bright burst of electromagnetic radiation and provide important information about the black hole’s environment. When the star is disrupted, approximately half of its material forms an accretion disk around the black hole. The event is mostly detected in the optical bands, although the accretion disk’s radiation lies in the X-ray regime. This phenomenon is still a subject of debate. With the Legacy Survey of Space and Time (LSST) expected to discover a vast number of new TDEs; therefore, an accurate theoretical description of these events is essential.
One of the explanations, the so-called slim disk model, states that when the fallback rate of the material exceeds the Eddington limit, a super-Eddington wind is released from the surface of the disk. The disk can sustain stability in the long term, because internal inhomogeneities reduce the effective opacity, keeping it locally sub-Eddington. The wind is optically thick, absorbing the radiation of the disk and re-emitting it at longer wavelengths.
An analytical model of TDEs based on aforementioned theory introduces a parameter describing the ratio of the wind to the disk material. The parameter largely affects the light curve of the event; therefore, its fine-tuning is crucial.
To achieve this, we present an implementation of the stationary super-Eddington slim disk model calculated for a wide parameter range of outer accretion rates and black hole accretion efficiency. This model can follow the evolution of the fallback-accretion rate and light curves of the TDEs more precisely. We used the so-called TiDE code to calculate monochromatic light curves of TDEs with our results. These light curves are compared to calculations with the old prescriptions, as well as with observations. These results demonstrate a physically consistent connection between the disk and the wind, providing an improved framework for fitting light curves of TDEs.

Speaker: Domonkos Szabó (Konkoly Observatory)

Domonkos_Szabo_talk.pptx

40 Giant Planet Formation and Migration in Protoplanetary Disks Evolving under Viscous Accretion and Magnetically Driven Winds

The formation and orbital evolution of giant planets are strongly influenced by the physical properties and dynamical evolution of their protoplanetary disks. In this work, we investigate giant planet formation and migration in protoplanetary disks evolving under the combined effects of viscous accretion and magnetically driven disk winds. We adopt an analytical disk model to describe the time evolution of the gas surface density and temperature, coupled with prescriptions for planetary gas accretion, gap opening, and migration driven by planet–disk gravitational interactions. We employ the Kanagawa migration model to account for the reduction of migration torques associated with planetary gap opening, providing a continuous description of migration from low-mass planets to gap-opening giant planets. We examine how disk viscosity, magnetically driven winds, and the evolving gas distribution influence planetary growth and orbital evolution. Our aim is to understand how the relative contributions of viscous accretion and magnetically driven disk winds to disk evolution affect the growth, migration, and final orbital distribution of giant planets.

Speaker: István Gergely Hegedüs (ELTE, CSFK)

FIKUT.pdf

41 Molecular transitions in supernova spectra: from quantum chemistry to astrophysics

Molecular astrophysics in supernova is gaining momentum in recent years, especially since the start of the science mission of James Webb Space Telescope (JWST). Applying radiative transfer theory is a key to connect these two fields of research: we can take into account molecular abundances and generate model spectra, which could allow us to deduce molecular components in the supernova material. I am working with radiative transfer codes, without the convenience of local thermal equilibrium (non-LTE), so the population of molecular states are not determined by the Boltzmann equation only. For non-LTE calculations, we need to know the collisional transfer rates for the typical collisional partners, which are mostly known to molecules and physical circumstances found in protoplanetary disks or in the interstellar medium.
My goal is to get these collisional transfer rates for supernova environments: to achieve it, I need to calculate potential energy surfaces of specific molecular systems, using quantum scattering theorem. Here I present the main steps of the methodology, as well as preliminary results on CO-O collisions, which can be an important step to model CO molecular transitions seen in JWST spectra of different types of supernovae.

Speaker: Márton Truszek (University of Szeged)

Márton_Truszek_presentation.pdf

10:30 Coffee Break

Stellar Pulsations, Activity, and Evolution

Convener: László Molnár (MTA CSFK)

42 From the death of stars to the dawn of life: dynamical effects of mass loss around high-mass stars

Stars shed a large fraction of their mass during their lifetimes through dense stellar winds and supernova explosions. Because the gravitational potential that changes as this mass is lost, the orbits of planets, moons, and stellar companions can widen, become eccentric, or unbind entirely. Here, I present a series of studies that examine these consequences using variable-mass N-body simulations with a homologous envelope expansion model, complemented by analytical and orbit-averaged secular methods.

In my talk, I will discuss several interesting phenomena associated with stellar mass loss, drawing on half a decade of research. How stable are planetary orbits around a star that explodes as a core-collapse supernova? If the orbit unbinds, and a rogue planet forms, can it retain its moons, and on what orbits? Can those moons sustain liquid subsurface oceans similar to those on Europa or Enceladus? In massive binary systems, can subsequent supernova explosions explain the observed population of double neutron stars? Is it possible to form a compact binary with a mass-gap black hole during a supernova-explosion? Finally, can tidally enhanced mass loss account for the exceptionally high eccentricity of Wolf-Rayet binaries?

Speaker: Viktória Fröhlich (Universität Bern)

Fröhlich_Viktória_FIKUT_talk.pdf

43 Exploring Young Stellar Variability with THESEUS

The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) will provide new opportunities for time-domain studies of young stellar objects through its soft X-ray, hard X-ray/γ-ray, and near-infrared capabilities. We investigate the potential of coordinated multi-wavelength observations of Galactic star-forming regions, with emphasis on X-ray flares, ultraviolet followup, and the most energetic megaflare events. Since predicted flare yields alone do not fully characterize the suitability of different regions for coordinated observations, we introduce a simple comparative metric that combines flare yield with source distance. The resulting ranking favours nearby star-forming regions for detailed multi-wavelength studies, while distant massive complexes remain valuable for statistical investigations of rare energetic events. We also present an order-of-magnitude estimate of the prospects for detecting gamma-ray megaflares with THESEUS/XGIS based on published Fermi-LAT results, illustrating how source distance and stellar population together influence the expected scientific return of high-energy observations.

Speaker: Nóra Varga (Eötvös Loránd University)

Varga_Nora_FIKUT.pptx

44 A search for strange modes in non-linear Cepheid models

Strange modes are unusual, non-classical pulsation behaviors that arise when the outer envelope of a Cepheid decouples from the interior. Mapping their expected instability regions based on stellar models is essential for the future observational identification of these objects. While prior research successfully established the theoretical instability strip of strange mode Cepheids on the Hertzsprung-Russell diagram using linear stability analysis, determining their actual pulsation amplitudes and the final outcome of mode selection requires a non-linear approach.
Continuing this research, I simulated stellar pulsations using the MESA RSP hydrodynamical software package, utilizing an extensive, well-defined parameter grid. To process the simulated data, I developed a custom Python-based framework that automatically classifies the different pulsational behaviors of the models and plots them on the Hertzsprung-Russell diagram. By comparing the obtained results with established stellar evolutionary tracks, the instability regions expected in reality can be accurately identified.

Speaker: Lívia Blanka Bárány (ELTE, HUN-REN CSFK CSI)

Bárány Lívia Blanka - A search for strange modes in non-linear Cepheid models.pdf

45 Pushing the Limits: Studying SN 2025zi and the Nature of Type Iax Supernovae

Type Ia supernovae are one of the most significant stellar explosions since they can be used for distance measurements in the universe. Among their subclasses, Type Iax supernovae show the highest diversity while being the lowest energy explosions of all Type Ia. Our aim is to study their origins and the possibility of expanding the distance ladder with them. One of the key steps of my work was to build a database that helps to explore their properties and estimate the rate of these explosions. I found that there are about 12 Type Iax for every 100 normal Type Ia, making them the most common peculiar supernovae. The database has also been created for the public and will be available online for everyone. I also studied one of the faintest Type Iax supernovae ever, SN 2025zi, and concluded that even these explosions fit into previously investigated correlations, despite the fact that no existing hydrodynamical simulation matches their observed properties.

Speaker: Erika Mochnács (University of Szeged)

fikut_2026_mochnács.pdf

46 TESS flares and chromospheric variability in three open clusters

Magnetic activity in cool stars is closely linked to stellar rotation and dynamo processes. Open clusters offer a controlled environment for investigating stellar activity because their members share ages, distances, and chemical compositions. We investigate how stellar age and effective temperature influence flare activity in cool stars, and search for signatures of coronal mass ejections (CMEs) in young and intermediate-age cluster stars. We analyze 120-s cadence TESS photometry of members of the Pleiades (100 Myr), Hyades (700 Myr), and Praesepe (700 Myr). We identify and characterize flares, calculate their energies, and derive flare frequency distributions for different stellar temperature and activity groups. We also analyze time-resolved hydrogen alpha spectra of Pleiades and Praesepe stars obtained with OSMOS at MDM Observatory to search for CME signatures and measure chromospheric activity. The flare frequency distributions have power-law indices of 1.8–2.8. The Pleiades exhibit the highest flare rates across the investigated spectral types. K dwarfs in the Pleiades flare about an order of magnitude more frequently than those in the Hyades, while M-dwarf flare rates are comparable between the two clusters. The M-dwarf flare rate peaks at ~3200–3300 K effective surface temperature, near the transition between partially and fully convective stars. No CME signatures are detected in the OSMOS spectra. Our main conclusions are the following: Stellar age and effective temperature strongly influence flare activity, with particularly enhanced activity in young K dwarfs and near the fully convective boundary in M dwarfs. The absence of detected CMEs provides an upper limit on their occurrence rates in these clusters. These results provide observational constraints on the evolution of magnetic activity and flaring in cool stars and offer insights into how stellar structure and age shape magnetic phenomena that may influence the environments of orbiting planets.

Speaker: Anna Görgei (HUN-REN CSFK, Konkoly Observatory)

TESS flares and chromospheric variability in three open clusters.pdf

47 High-velocity spectral features in thermonuclear supernovae

Type Ia supernovae (SNe Ia) are thermonuclear explosions of white dwarfs in binary systems, and have been widely used for astronomical distance measurements for decades. Despite their long history of observation however, there are many unknowns about the physical parameters of the progenitor star and the explosion mechanism itself. One of these unknowns is the presence of so-called high-velocity features (HVFs).

High velocity (25-30000 km/s) features are absorption lines of Ca II, and sometimes Si II that can be seen in the early spectra of SNe Ia at velocities significantly higher than that of the photosphere. First discovered in 1999, they have since been proven to be ubiquitous in SNe Ia. However, their exact origin still remains unclear to this day. They appear to form in a higher velocity layer above the photosphere, and show varying strengths and velocity evolution from object to object.

We used 15 years of early-phase optical/near-infrared spectra obtained by the Hobby-Eberly Telescope (HET) of 57 supernovae to determine the velocity, strength and evolution of these features.
We confirm a connection between the light-curve width and the strength (and velocity) of the HVFs, with brighter SNe Ia showing stronger (and faster) high velocity lines. Through our investigation, we conclude that HVFs are most likely a consequence of the explosion mechanism itself, and their further study could help constrain the explosion mechanism.

Speaker: Zsófia Bora (Hun-Ren CSFK KTM CSI)

bora_hvf_fikut26.pdf

12:30 Lunch Break

Astrochemistry and Nuclear Astrophysics

Convener: Balázs Kacskovics (HUN-REN Wigner Research Centre for Physics)

48 Evolving Dark Energy: Past, Future Fates, and Physical Bounds

In the standard $\Lambda$CDM model of cosmology, the equation-of-state for dark energy is $w = p_{DE}/\rho_{DE} = -1$, which implies a constant energy density throughout the evolution of the Universe. However, recent observations of cosmic expansion and gravitational lensing increasingly favour a dynamic, time-varying dark energy. In the literature, the Chevallier–Polarski–Linder (CPL) parametrisation is widely used to describe this behaviour; it is a first-order Taylor expansion centred on the present-day scale factor ($a = 1$). The CPL model is a linear approximation, and its applicability is limited far from the present epoch: at high redshifts, it can cross into the "phantom" regime ($w < -1$), a region that is physically problematic for scalar-field models, while in the distant future, it diverges asymptotically. A few alternative dynamic dark energy models have been investigated in the last couple of decades; however, these often address only one of these issues, focusing either on avoiding future divergence or on preventing a transition into the phantom regime in the past at high redshifts.

The objective of my project is to analyse the evolution of various dynamic dark energy parametrisations in a theoretical framework. I examined quantities describing cosmic expansion and structure formation, such as the matter density parameter, the density of dark energy, and the linear growth factor and rate, and, based on their asymptotic behaviour, formulated physical and phenomenological conditions for comparing different parametrisations. Deriving the result explicitly from the relativistic continuity equation, I showed that a reversal in the monotonically decreasing trend of the matter density parameter, implying a return to matter dominance, occurs precisely when the equation-of-state parameter transitions from the negative to the positive regime, regardless of the specific parametrisation chosen. This allows for the establishment of a phenomenological upper bound, helping to avoid an otherwise difficult-to-justify return to matter dominance and the loss of the negative pressure associated with dark energy. By adhering to this criterion, along with the lower bound on the equation-of-state parameter ($w \in [-1, 0]$) characteristic of scalar-field quintessence models, I employed a symbolic regression (machine learning) approach to identify a parametrisation that satisfies these boundary conditions within a specific region of the parameter space.

Speaker: Zétény Lőkös-Birdal (Konkoly Observatory / ELTE)

FIKUT_Lőkös-Birdal_Zétény.pdf

49 Laboratory Modeling of Cosmic-Ray-Driven Chemistry in Interstellar Ice Analogs

Dust grains are important components of the interstellar medium (ISM). Their surfaces are typically covered by icy mantles formed through the condensation of gas-phase species of the ISM. Upon exposure to external irradiation, such as cosmic rays, chemical reactions can be initiated within these ice layers. [1] These reactions lead to the formation of new chemical species, some of which can subsequently sublime from the condensed phase into the gas phase, thereby altering the original composition of the gaseous ISM. [1,2]
Interstellar ice analogs containing molecules present in the ISM, including methanol (CH3OH), ethanol (CH3CH2OH), methyl amine (CH3NH2), and ammonia (NH3), have been experimentally studied using the VIZSLA (Versatile Ice Zigzag Sublimation Setup for Laboratory Astrochemistry) setup. [3] First, the ices were condensed onto a cold surface. Then, to simulate the effects of cosmic-ray irradiation, the ices were bombarded with 5 keV electrons. After that, the irradiated samples were heated in a controlled manner. During the temperature-programmed heating, two distinct experiments were performed for each sample. In the first, spectral changes of the processed ices were monitored throughout the entire heating process. In the second, species sublimating from the ice were allowed to recondense onto a second substrate. During this recondensation process, the matrix-isolation technique was employed, enabling the more sensitive identification of the recondensed species, i.e., the molecules sublimating from the ice during the temperature-programmed desorption.
The experiments showed the formation of several reaction products both in electron bombarded CH3OH:CH3NH2 and CH3CH2OH:NH3 astrophysical ice analogs. Collectively, the studied processes contribute to our understanding on the chemical evolution of the ISM and demonstrates that interstellar ices are an important source of chemical complexity in space.
[1] E. F. van Dishoeck, G. A. Blake, Annu. Rev. Astron. Astrophys., 36 (1998), 317.
[2] W. D. Watson, E. E. Salpeter, Astrophys. J., 174 (1972), 321.
[3] Bazsó, G.; et al. Rev. Sci. Instrum. 2021, 92(12), 124104-124143.

Speaker: Barbara Keresztes (ELTE Eötvös Loránd University, Budapest)

FIKUT_Keresztes.pptx

50 Introduction to the dynamics of Haumea’s ring

Recently, several rings were discovered around various minor planets and asteroids. The origin and history of these rings are not well understood yet. We specifically focus on the ring of the dwarf planet Haumea and its perturbed nature. In this project, we are using numerical simulations with a modified version of the REBOUND N-body code to study the dynamical effects occurring in this system. Moreover, we make analytical predictions for the minimum ring width around Haumea, Chariklo, Quaoar, and Chiron. We also aim to construct local simulations of the ring, analogously to the standard shearing sheet model, to study kinetic properties. In this presentation, I will introduce several dynamical features of Haumea’s ring and discuss how the standard local simulations of planetary rings break down in this example.

Speaker: Péter Csernyik (University of Toronto)

Csernyik_Peter_FIKUT_presentation_pauses.pdf

Compact Objects, Relativistic Astrophysics, and Gravitational Waves

Convener: Balázs Kacskovics (HUN-REN Wigner Research Centre for Physics)

51 Volume Concepts in the Thermodynamics of Black Holes

Thermodynamic volume and extensivity in black hole thermodynamics

Black holes lack a coordinate-independent notion of volume, so their thermodynamics is non-extensive. In extended AdS thermodynamics, the mass is treated as enthalpy and the cosmological constant as pressure, but for Schwarzschild-AdS black holes, the resulting volume is fixed by the entropy, leaving the state space degenerate. This degeneracy can be resolved by assuming Euler homogeneity of the entropy through a scaling relation between horizon radius, energy and volume. A generalized pressure then selects a volume consistent with the Christodoulou–Rovelli concept. Within this framework, thermodynamic stability is restored, the concavity of the entropy is recovered, and the stability and evaporation boundaries, including the Hawking–Page temperature, shift relative to the standard treatment. Our results complement the quasi-local, holographic definition of black hole volume recently proposed, where boundary area plays the role of volume and extensivity emerges in a large-system limit. Both approaches resolve the state-space degeneracy, but differ on whether volume is an interior or a boundary property.

Speaker: Réka Somogyfoki

black_holes_volume_beamer_FIKUT2026.pdf

52 Early inspiral higher harmonics and Einstein Telescope geometry

Higher harmonics from asymmetric compact binaries may enter the Einstein Telescope’s observing band before the dominant quadrupole signal. This may extend the interval over which Earth’s rotation changes the detector response. We examine how much noise-weighted signal accumulates during this earlier interval, comparing a triangular detector in the Euregio Meuse–Rhine region with two pairs of L-shaped detectors at Sardinia–Meuse–Rhine and Sardinia–Lusatia. By accounting for Earth’s rotation, we investigate how detector geometry affects the observable early signal. This provides a quantitative starting point for assessing the harmonics’ contribution to early source characterization.

Speaker: Kata Karácsonyi (University of Szeged & HUN-REN Wigner RCP)

Karacsonyi_FIKUT_NEXTGEN_2026.pdf

Closing

Closing.pdf

Visiting the Wigner's Jánossy Lajos Underground Laboratory

Janossy_UndergroundResearchLaboratory_FIKUT_v1.pdf