A5039274669- Stellar, planetary, and galactic studies
- Astro and Planetary Science
- Astronomical Observations and Instrumentation
- Astronomy and Astrophysical Research
- Astrophysical Phenomena and Observations
- History and Developments in Astronomy
- Astrophysics and Star Formation Studies
- Gamma-ray bursts and supernovae
- Historical Astronomy and Related Studies
- Hydraulic and Pneumatic Systems
- Solar and Space Plasma Dynamics
- Vehicle Dynamics and Control Systems
- Astrophysics and Cosmic Phenomena
- Spacecraft Design and Technology
- Mechanical Engineering and Vibrations Research
- Engineering and Test Systems
- Model Reduction and Neural Networks
- Real-time simulation and control systems
- Advanced Frequency and Time Standards
- Space Satellite Systems and Control
- Satellite Image Processing and Photogrammetry
- Particle Accelerators and Free-Electron Lasers
- History of Science and Natural History
- Nuclear physics research studies
- Material Science and Thermodynamics
Institute for Computer Science and Control
2024
University of Szeged
2016-2023
Astronomical Observatory
1998-2015
Eötvös József Főiskola
1996-2011
MTA-SZTE Research Group on Artificial Intelligence
1996
We present extensive optical ($UBVRI$, $g'r'i'z'$, and open CCD) near-infrared ($ZYJH$) photometry for the very nearby Type IIP SN ~2013ej extending from +1 to +461 days after shock breakout, estimated be MJD $56496.9\pm0.3$. Substantial time series ultraviolet spectroscopy obtained +8 +135 are also presented. Considering well-observed SNe literature, we derive $UBVRIJHK$ bolometric calibrations $UBVRI$ unfiltered measurements that potentially reach 2\% precision with a $B-V$ color-dependent...
Context . Since the discovery of first exoplanet almost three decades ago, number known exoplanets has increased dramatically. By beginning 2000s it was clear that dedicated facilities to advance our studies in this field were needed. The CHaracterising ExOPlanet Satellite (CHEOPS) is a space telescope specifically designed monitor transiting orbiting bright stars. In September 2023, CHEOPS completed its nominal mission duration 3.5 yr and remains excellent operational conditions. As...
The aim of this paper is to search for evidences the presence unseen companions in some eclipsing binary systems using their O–C diagrams. A total 8507 times minima (6890 visual and 1617 photographic or photoelectric ones) 18 have been collected from remarkable database late Dieter Lichtenknecker (Lichtenknecker 1988) other more recent papers. Assuming that light-time effect (LITE) responsible periodic components on diagrams sets orbital parameters were derived Kopal's (1978) method. In...
We study the long-term time-scale (i.e. period comaprable to orbital of outer perturber object) transit timing variations in transiting exoplanetary systems which contain a further, more distant (a_2>>a_1) either planetary, or stellar companion. give an analytical form O-C diagram (which describes such TTV-s) trigonometric series, valid for arbitrary mutual inclinations, up sixth order inner eccentricity. show that dependence on and physical parameters can be separated into three parts. Two...
The nearby, bright, almost completely unreddened Type Ia supernova 2011fe in M101 provides a unique opportunity to test both the precision and accuracy of extragalactic distances derived from SNe light curve fitters. We apply current, public versions independent fitting codes MLCS2k2 SALT2 compute distance modulus SN high-precision, multi-color (BVRI) curves. results two confirm that is "normal" (not peculiar) only slightly reddened Ia. New moduli are as 29.21 +/- 0.07 mag (D ~ 6.95 0.23$...
Abstract In dancing sprite events, entities and groups appear in rapid succession together with a corresponding series of parent lightning strokes. Dancing including case possible rebrightening, were recorded on video simultaneously from two observation sites above mesoscale convective system Central Europe the night 6 August 2013. Joint analysis triangulated locations elements, position, type, peak current strokes LINET detection network database moment waveforms deduced at Hylaty station,...
We report the discovery with $TESS$ of a third set eclipses from V994 Herculis (TIC 424508303), previously only known as doubly-eclipsing system. The key implication this and our analyses is that Her second fully-characterized (2+2) + 2 sextuple system, in which all three binaries eclipse. In work, we use combination ground-based observations data to analyze A B order update parameters inner quadruple's orbit (with derived period 1062 $\pm$ 2d). binary C were detected also found older...
Complex period variations of five W UMa type binaries (AB And, OO Aql, DK Cyg, V566 Oph, U Peg) were investigated by analyzing their O--C diagrams, and several common features found. Four the systems show secular at a constant rate on order |dP / dt 1/P | ~ 10E-7 1/yr. In case AB Peg high-amplitude, nearly one-century long quasi-sinusoidal pattern was also It might be explained as light-time effect, or some magnetic phenomena, although mathematical, consequently physical, parameters these...
We present a comparative study of absolute distances to sample very nearby, bright Type Ia supernovae (SNe) derived from high cadence, signal-to-noise, multi-band photometric data. Our consists four SNe: 2012cg, 2012ht, 2013dy and 2014J. new homogeneous, high-cadence data in Johnson–Cousins BVRI Sloan g'r'i'z' bands taken two sites (Piszkesteto Baja, Hungary), the light curves are analyzed with publicly available curve fitters (MLCS2k2, SNooPy2 SALT2.4). When comparing best-fit parameters...
CHEOPS is a space telescope specifically designed to monitor transiting exoplanets orbiting bright stars. In September 2023, completed its nominal mission and remains in excellent operational conditions. The has been extended until the end of 2026. Scientific instrumental data have collected throughout in-orbit commissioning operations, enabling comprehensive analysis mission's performance. this article, we present results with twofold goal. First, aim inform scientific community about...
Results of a new light-curve analysis and period variation study the eclipsing binary IM Aur are presented. Four solutions given according to different spectral types primary, available in literature. Multicolour photometry both indicate close (≈ ) third physical member. If it is considered as main-sequence star, then its type A2V–A8V, with mass . The light-time effect modelled by authors' simultaneous secular periodic terms fitting code. Clear evidence change also revealed. detailed effects...
Physical parameters of the W UMa-type eclipsing binaries UZ Leo and CV Cyg are presented based on light-curve analysis. Modified Lucy models (containing either a temperature excess secondary component or spots surface primary) were fitted to V B light curves. Both systems show positive (indicating hot secondary) one large dark spot near pole primary — it is not possible decide which solution real from present data sets only. The average density both less than that most other known UMa stars;...
Context. Despite the fact that VW Cephei is one of well-studied contact binaries in literature, there no fully consistent model available can explain every observed property this system. Aims. Our motivation to obtain new spectra along with photometric measurements, analyze what kind changes may have happened system past two decades, and propose ideas for explaining them. Methods. For period analysis we determined 10 times minima from our light curves, constructed a O$-$C diagram Radial...
Abstract EM Cygni is a Z Cam‐subtype eclipsing dwarf nova. Its orbital period variations were reported in the past but results conflict to each other while studies allowed possibility of no variation. In this study we report accurate new times minima binary and update its O – C diagram.We also estimate mass transfer rate system conclude that far from critical value. The determined eclipse timings agreement with spectroscopically (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
We present the results of photometric CCD observations magnetic cataclysmic variable V405 Aurigae (RX J0558.0+5353= 1RXS J055800.7+535358)obtained using different instruments.We analysed variability spin period white dwarf in Aur J0558.0+5353)system our and previously published maxima timings.The system 2010-2012 is P = 545.4558163(94)s.As we have gaps observational data, 2 hypotheses this a cubic ephemeris which may be interpreted by precession or periodic change with 6.2 years...
The types of instability in the interacting binary stars are reviewed. project "Inter-Longitude Astronomy" is a series smaller projects on concrete or groups stars. It has no special funds, and supported from resources grants participating organizations, when informal working created. Totally we studied 1900+ variable different types. characteristic timescale seconds to decades (extrapolating) even more. monitoring first star our sample AM Her was initiated by Prof. V.P. Tsesevich...