Abstrakta příspěvků

Abstrakta přihlášených příspěvků jsou průběžně doplňována dle zaslaných přihlášek.

Plenární přednášky

Soňa Ehlerová (Astronomický ústav AV ČR, v.v.i., Praha-Spořilov)

Kam směřuje astronomie

TBD

Petr Kabáth (Astronomický ústav AV ČR, Ondřejov)

Exoplanet research in the era of PLATO space mission

End of the 2026 will be marked by the launch of PLATO space mission. PLATO will have one of the main goals to detect small habitable planets around Sun-like stars. Detection of the second Earth is an extremely complex task and an extensive follow-up observations from the ground are required. My presentation will introduce Czech contribution to the PLATO mission and to the detection process of the second Earth. In more detail, the current landscape of exoplanetary research will be summarised and some latest results with instrumentation like PLATOSpec but also upcoming projects will be shown.

Kamil Bicz (Uniwersytet Wroclawski, Poland)

Modern Challenges in Detecting and Analysing Stellar Flares: From Photometry to Spectroscopy

Stellar flares, from short impulsive bursts to multi-hour superflares, are powerful manifestations of stellar magnetic activity. High-precision space photometry combined with ground-based multi-colour photometric and spectroscopic observations now reveals their morphology and energetics in unprecedented detail and exposes the limitations of traditional approaches.

I will present recent results that illustrate both the progress and the challenges. On a K-type star, the analysis of a 27-hour flare revealed the underlying starspot distribution through rotational modulation. After correcting for this modulation, the bolometric energy estimate increased from about 1×10^35 erg to 4×10^35 erg, showing how essential such corrections are for long-duration events. During the same flare, repeated occultations indicated the presence of an extended, cool magnetic structure above the active area. Its geometry and physical parameters, derived for the first time on a star other than the Sun, show that photometric data alone can hint at flare-associated loops or arcades.

Multi-colour observations of fifteen flares on M- and K-dwarfs further demonstrate that the emitting area typically varies only by 10–30 % during most of the event, while the temperature can increase by a factor of 2.5, reaching 5 700–17 500 K. Combining these results with stellar parameters led to a semi-empirical grid relating effective temperature and flare amplitude to peak flare temperature. Applying it to over 42 000 TESS flares yields peak blackbody temperatures from 5 700 to 38 300 K, with a median around 11 000 K.

In addition to these published results, I will present upcoming findings from new photometric and spectroscopic analyses that further refine flare temperature and area estimates and provide fresh insight into the link between active regions and flare emission.

Ondřej Pejcha (Ústav teoretické fyzicky, MFF Univerzity Karlovy, Praha)

Zářivě hydrodynamické simulace splynutí dvojhvězdy

Splynutí dvou hvězd je doprovázeno zjasněním trvajícím desítky až stovky dnů, které nazýváme Luminous Red Nova (LRN). Mezi nejznámější zástupce této kategorie patří V838 Mon a V1309 Sco. Studiem LRN můžeme lépe pochopit tuto dosud neúplně objasněnou fázi dvojhvězdného vývoje, která má kritickou roli i v mnoha jiných situacích včetně vývoje zdrojů gravitačních vln. Dosud ale není jasné, co je hlavním zdrojem energie v pozorovaných LRN. V přednášce představíme výsledky osově symetrických zářivě hydrodynamických simulací LRN, které ukazují, že rázové vlny jsou schopné vysvětlit ty nejjasnější pozorované extragalaktické LRN.

Pavol A. Dubovský & Karel Kolomazník (Sekcia premenných hviezd a exoplanét Slovenskej astronomickej spoločnosti a Slovenského zväzu astronómov)

Search for the Nova Super-Remnants - Physical background and future progress of the campaign

In recent years, aesthetic astrophotography and scientific exploration of the universe have increasingly converged. By combining numerous wide-field images taken with narrowband filters into extremely long total exposures, it has become possible to reveal previously unseen extended structures in the night sky with very low surface brightness. These include faint nebulae, stellar streams around galaxies, supernova remnants, and similar objects. Nova super-remnants—the diffuse shells created by repeated nova explosions—represent another promising area of study. Unlike the expanding shell produced by a single, recent nova event, a nova super-remnant is the cumulative result of multiple eruptions over time.

Gas from successive explosions interacts and heats the surrounding low-density medium, producing faint emission spectra with a peak at the Halpha wavelength of 656.3 nm. The first successful detections have already been reported. Research has naturally begun with recurrent novae, which erupt most frequently. Notable examples include the recurrent nova M31N 2008-12a in the Andromeda Galaxy and KT Eri, which was previously only suspected of being recurrent. Extended structures around the cataclysmic variable Z Cam have also been imaged. The *Condor Telescope Array* in New Mexico, specifically designed for detecting low surface brightness objects, has played a key role in this effort.

However, comparable results can also be achieved with the equipment of advanced amateur astrophotographers. To accumulate sufficient total exposure time, the coordinated effort of multiple telescopes operating in an automated regime is essential. At present, nine Slovak and Czech astrophotographers are participating in this campaign. We have already completed a pilot project targeting the known nebulosity around Z Cam, serving as a test of our capabilities. In the summer of 2025, several additional candidate objects were observed with relatively short total exposure times. The next step is to select the most promising targets for deep, long-term imaging.

The scientific significance of this work lies in the potential confirmation that all novae are recurrent, though not all erupt frequently enough for us to witness more than one outburst. Equally valuable will be data on eruption frequency, expansion velocities, interaction with the interstellar medium, and motion of the progenitor star. Even a negative result—such as determining a limiting detectable surface brightness — would provide important constraints. Furthermore, the images obtained will yield extensive photometric data on stars within each field of view.

The main challenge for our campaign is the limited observing time caused by adverse weather in Central Europe. One of our telescopes is already operated remotely from a hosting site in Spain, and we plan to establish our own telescope-hosting facility in southern Spain to ensure more consistent observing conditions.

Abstrakta přihlášených příspěvků

Vojtěch Šimon (Astronomický ústav AV ČR, Ondřejov)

Aktivita kataklyzmických proměnných po skončení erupce klasické novy

Kataklyzmické proměnné jsou objekty, v nichž na bílého trpaslíka proudí hmota z jeho průvodce. Tento proces způsobuje mohutná zjasnění (tzv. výbuchy klasických nov), která ovlivňují aktivitu těchto objektů i dlouho (roky, desetiletí) po skončení vzplanutí. Tuto aktivitu je možné pozorovat a monitorovat i amatérskými prostředky a metodami (CCD i vizuálně). Představujeme příklady dlouhodobé aktivity několika takových objektů.

Petr Zasche (Astronomický ústav, MFF Univerzity Karlovy, Praha)

Dvojzákrytové systémy: Když nastanou komplikace

Standardní dvojzákrytové systémy vykazující dvě periody zákrytů jsou již rutinně zkoumány. V této přednášce bude ale kladen důraz na ty soustavy, které vykazují jisté abnormality, komplikace, a jednoduchý standardní postup nelze jednoduše použít. Co když je hvězd více? Co když se křivky deformují? Co když nelze zanedbat dynamické efekty? Co když O-C diagram neukazuje nic?

Miloslav Zejda (Ústav teoretické fyziky a astrofyziky, PřF Masarykova univerzita, Brno)

30 let mé křemíkové astronomie

Stručný průvodce vývojem techniky i cílů pro má CCD pozorování proměnných hvězd v letech 1995-2025.

Ladislav Šmelcer (Hvězdárna ve Valašském Meziříčí)

Eruptivní hvězdy kontra exoplanety

New observations reveal a possible interaction between chromospherically active stars and their exoplanets in close orbits. High-energy eruptions can have a direct impact on the atmospheres of exoplanets, and it is not impossible that they could be blown away. In connection with the ARIEL project, another interesting observation program is being proposed.

Martin Vrašťák (Liptovská Štiavnica Observatory)

Newton 508/1900, f/3.8, part II.

I will present a new telescope of my own construction, which I use in my observatory in Liptovská Štiavnica, and the first results obtained with this telescope. I will follow up on the previous presentation given at the 56th conference in Litomyšl 2024.

Martin Vrašťák (Liptovská Štiavnica Observatory)

Príklad pro-am spolupráce – práca o prvých hodinách a dňoch vzplanutia rekurentnej symbiotickej novy RS Ophiuchii v roku 2021

An example of pro-am colaboration - The first hours and days of the 2021 explosion of the recurrent symbiotic nova RS Ophiuchii.

A. Skopal, M. Vrašt’ák, F. Teyssier, M. Fujii, S. Shugarov, M. Šlechta, and M. Wolf

Data obtained by amateur astronomers from different parts of the world can very well complement observations by professional astronomers and large telescopes. Such pro-am collaboration can be targeted and lead to very interesting results. A paper about the first hours and days of the explosion of the recurring symbiotic nova RS Oph in 2021 was created in a similar way.

Ivo Peretto (MarSEC, Italy)

The revision of CzeV variable stars by the SSV-UAI-GRAV

While the discovery of new variable stars by amateur astronomers is becoming increasingly difficult due to automated surveys, there is one area where it is still possible to actively contribute to scientific research: the review of variable stars that are already known but whose characteristics can be refined. The SSV-UAI-GRAV, the variable stars section of the Italian Amateur Astronomers Union, has undertaken such work by refining some stars in the Czev catalog.

Martin Jelínek (Astronomický ústav AV ČR, Ondřejov)

Nátroje pro automatizaci astronomických pozorování v Linuxu

Linux je prima. Vzdálená práce je přirozenou součástí systému a tak se nabízí jako logická volba pro vzdálené ovládání astronomických observatoří. Ukážu co všechno je potřeba udělat, aby se z té představy stala realita včetně automatizace plánování pozorování a jejich zpracování a demonstruji to na příkladech jako D50, SBT, FRAM, BOOTES atd.

Jan Štrobl (Astronomický ústav AV ČR, Ondřejov)

Systém pro autonomní robotické observatoře RTS2

Pokročilý pozorovatel proměnných hvězd může časem dojít ke zjištění, že noční bdění nad dalekohledem je sice ohromná zábava, přesto ve větších dávkách může být tak trochu únavné a vlastně se ani moc dobře neslučuje se životem (biologickým, natož pak společenským/rodinným). A že by se občas docela hodilo, kdyby "to" třeba mohlo pozorovat i úplně samo. Pokusíme se zde představit naše řešení (této základní otázky života, vesmíru a vůbec), kterým je systém RTS(4)2, tedy, pardon, RTS2 :-).

Představíme samotný systém RTS2, jeho základní filozofii a také zmíníme některé dalekohledy, na kterých je úspěšně používán (na Astronomickém ústavu v Ondřejově i mimo něj).

Miracle Chibuzor Marcel (Pan-African Citizen Science e-Laboratory)

Exploring Statistical Correlations in Exoplanet Transit Parameters: A Study of Over 400 Light Curves by Citizen Scientists from Developing Countries

This study investigates statistical correlations among key transit parameters in 409 exoplanet light curves contributed by citizen scientists participating in the NASA Exoplanet Watch project. Conducted through the Pan-African Citizen Science e-Laboratory (PACS e-Lab), the research examines how observational variables, such as transit depth, duration, stellar brightness (Vmag), number of images, residual scatter, and detection significance, interact to affect the quality and detectability of transits captured with small telescopes. A standardized analysis was applied, including logarithmic transformations and Pearson correlation assessments, to evaluate twelve parameter pairs. The results confirm several theoretical expectations: detection significance increases with deeper and longer transits, brighter host stars, lower scatter, and more exposures, consistent with established signal-to-noise models. Residual scatter emerged as the strongest predictor of detection confidence, highlighting the importance of careful calibration and noise reduction. Some parameter pairs, such as transit depth versus duration, showed weak or no correlation, reflecting the diversity of planetary system architectures. This work demonstrates that citizen-led, small-telescope observations can yield robust scientific insights when processed with standardized tools and collaborative validation. The findings offer practical guidance for improving future data quality and underscore the potential of citizen science as a valuable contributor to exoplanet research, particularly in underserved regions.

Marek Skarka (Astronomický ústav AV ČR, Ondřejov)

Klasifikace proměnných hvězd v datech z TESS

Fotometrické časové řady produkované vesmírnými misemi nabízejí unikátní možnost k odhalování nových proměnných hvězd a k jejich klasifikaci. Bohužel ne vždy je tato klasifikace jednoduchá a jednoznačná. Zaměřím se na potíže, které je nutné překonávat a brát v potaz při klasifikaci proměnných hvězd na základě dat z družice TESS.

Jan Soldán (Astrosoft, Ondřejov)

Astrosoft Double Telescope

We would like to present the current state of hardware and software development of our new double telescope. The telescope is in the final stage of its hardware & software development.

Studentská sekce

Michal Zummer (Astronomický ústav, MFF Univerzity Karlovy, Praha)

Unique quadruple HD 135160

After analyzing four years of high-resolution echelle spectroscopy and photometric data from the TESS mission, we have discovered that HD 135160 is a unique 2+2 quadruple system. It consists of a massive eccentric ellipsoidal binary and an eclipsing binary exhibiting a strong reflection effect. Both pairs are gravitationally bound and orbit each other with a period between 4.4 and 6 years. The system also exhibits small periodic flux variations of unknown origin.

Rebecca Szabó (Astronomický ústav MFF Univerzity Karlovy, Praha)

Architecture of planetary systems and their effects on the occurrence of stellar flares

Flares occur on stars that are magnetically active and present themselves as a large increase in the flux emitted from a star. Many stars have planets orbiting around them, with the existence of over 6000 exoplanets confirmed so far and even more exoplanet candidates. Many planets have their own magnetic field, which possibly interferes with the star's magnetic field, inducing flares. If this were to be the case, Jupiter-sized exoplanets orbiting near their host star should have the most significant effect, considering the architecture of planetary systems. Predominantly using data gathered from the satellite TESS, it is possible to determine the occurrences of stellar flares. The main focus of this work is analysing stars (with known exoplanets) with a high rate of flares by examining the distribution of occurred flares. By reconstructing the orbits of their exoplanets, I therefore aim to statistically determine whether there is a relation between the period with which the flares occur on a specific star and the orbital elements of its exoplanets. The conclusion may then be extended to our own solar system, where the length of the main cycle of the Sun's activity is suspiciously similar to Jupiter's orbital period. The purpose of this work is to prove whether the architecture of a planetary system truly has an effect on the occurrence of stellar flares or whether it is purely a coincidence.

Jana Bušovská (Astronomický ústav MFF Univerzity Karlovy, Praha)

Accuracy of exoplanet parameters from transit observations

Using data obtained from an observing campaign coordinated by SPHE ČAS and collected by amateur astronomers, two modeling approaches — Pylightcurve and the Exoplanet Transit Database (ETD) — were compared in terms of accuracy and consistency. The analysis highlights the contribution of amateur observations to refining exoplanetary parameters such as the planet-to-star radius ratio and the mid-transit time.

Alžběta Maleňáková (Olomouc)

GRB afterglows with observed maxima: what can we say of them?

Thanks to rapid follow up of FRAM, D50 and SBT telescopes, we obtained a collection of GRB afterglow lightcurves that present early maxima. I will present my thesis that deals with fitting of these rare events.

Prokop Ohlídal (Masarykova univerzita, Brno)

Eclipsing binaries with period changes

Some eclipsing binary systems exhibit variations in their orbital periods. Three such systems — V366 Cyg, S Cnc, and DX Vel — were selected for further analysis. Data from space-based surveys, TESS and K2, the ground-based survey ASAS-SN, and, in the case of V366 Cyg, our own photometric observations were used to construct and analyze O-C diagrams. Archival data from the Krakow Timing Database and VarAstro were also incorporated. Physical models for each system were created using the PHOEBE software to determine their key parameters. This presentation introduces the methods used, the analysis process, and the main findings, providing insight into the period variations observed in these systems.

Jan Kříž (Ústav teoretické fyzicky, MFF Univerzity Karlovy, Praha)

Souřadnicové systémy pro Rocheův potenciál

Binární systémy jsou jedním z nejtypičtějších a nejstudovanějších vesmírných objektů. Jsou zodpovědné za mnoho zajímavých astrofyzikálních jevů, od rekurentních nov až po emisi gravitačních vln. Fyzika kolem binárních systémů je do velké míry popsána Rocheovým potenciálem, který svou formou zachycuje gravitační interakci společně s odstředivými silami.

Jelikož je (nejen v numerických simulacích) výhodné pracovat v adaptovaných souřadnicích, stalo se studium Rocheova potenciálu disciplínou s dlouhou tradicí. Jedním z hlavních cílů této snahy bylo právě zavedení globálních 3D souřadnic adaptovaných na ekvipotenciální plochy. Ukázalo se však, že takovýto výsledek není matematicky možný.

Ondřej Marek (Masarykova univerzita)

AstroCollector - web application for downloading & plotting variable star data

In order to study the variability of stellar objects, it is essential to obtain as many measurements as possible, ideally covering the longest time interval possible. Numerous star surveys produce large amounts of photometric data, which are stored in their respective archives.

However, each project typically uses its own data format. For astrophysicists, searching through these archives and converting the data into a unified format can be time-consuming.

AstroCollector is a web application designed to address this issue. Its main purpose is to search for photometric data across various star survey projects. The collected data can be visualized as a light curve or a phase curve. It is also possible to download the data in both processed and original formats for further use.

Průmyslové aplikace a technologie v astronomii

Carlos Guirao & Gerardo Avila (Baader Planetarium)

Baader spectrographs - testing the WHAPOS spectrograph in the 1m Vega (Salzburg) and in the 1.5m Sierra Nevada (Granada) observatories

Pavel Cagaš (Moravské přístroje)

Astronomické kamery Moravské přístroje -- novinky 2025-2026

Martin Myslivec (2EL, spol. s r.o.)

2EL, spol. s r.o. - Deset let výroby dalekohledů

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