TY - JOUR AU - Kalup, Csilla AU - Kiss, Csaba TI - Radiative transfer modelling of Haumea's dust ring JF - BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY J2 - BULL AM ASTRON SOC VL - 55 PY - 2023 IS - 8 SN - 0002-7537 UR - https://m2.mtmt.hu/api/publication/34493622 ID - 34493622 AB - Over the past decade, a number of ring systems around small bodies in the Solar System have been revealed by stellar occultations. On 21 January 2017, Haumea was discovered to have a ∼ 70 km-wide ring with a radius of 2285 ± 80 km. While the dimensions, orientation and certain optical properties of the ring systems have been inferred from occultation measurements, they do not provide direct information about the material of the ring itself. Simple models applied previously use condensed parameters like the reflectivity I/F, the visible range optical depth τ, and the radius and width of the ring to estimate the reflected light and thermal emission of the ring. Naturally, in these models the optical properties of the grains are not considered. To give a most plausible description of the Haumea ring we use radiative transfer simulations with the radmc3d code and investigate how different physical properties, size distributions and various compositions (e.g. pure water ice, amorphous carbon, a mixture of pyroxene and olivine) would affect the ring properties. By modelling the thermal radiation of the ring at visible, infrared, submillimetre and millimetre wavelengths, we can make predictions that can be directly compared with ongoing and planned ground- and space-based observations especially with ALMA and the James Webb Space Telescope that are now able to spatially resolve the ring and detect its emission and reflected light separated from the main body of Haumea. LA - English DB - MTMT ER - TY - JOUR AU - Kiss, Csaba AU - Takacs, Nora AU - Szakáts, Róbert AU - Pál, András TI - Light curves of Jovian Trojan asteroids from the TESS mission JF - BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY J2 - BULL AM ASTRON SOC VL - 55 PY - 2023 IS - 8 SN - 0002-7537 UR - https://m2.mtmt.hu/api/publication/34493621 ID - 34493621 AB - Jovian Trojans are of particular importance because they are touchstones for solar system evolution models. Despite their large number, rotational characteristics are known for a relatively limited sample of targets from ground-based observations. Rotation period and amplitude distributions derived from this sample are strongly affected by ground-based biases, as it was shown by recent studies using data from the K2 mission of the Kepler Space Telescope. The main result of these investigations is that there are a significantly larger number of slow rotators than previously thought. Month-long, uninterrupted light curve data, in many cases spanning over multiple sectors are provided by the TESS mission for a large number of Jovian Trojans. Here we present the first results of our study that could derive accurate light curves for more than 500 Jovian Trojans and provide amplitude upper limits for another three thousand. Our results are compared with the previous investigations of ground based observations and K2 measurements. We also investigate the difference between the rotational characteristics of the 'red' and 'less red' groups and between collisional families and the background population of Jovian Trojans. LA - English DB - MTMT ER - TY - JOUR AU - Szakáts, Róbert AU - Kiss, Csaba TI - Rotational Phase Dependent J − H Colour of the Dwarf Planet Eris JF - PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC J2 - PUBL ASTRON SOC PAC VL - 135 PY - 2023 IS - 1054 SN - 0004-6280 DO - 10.1088/1538-3873/ad0b31 UR - https://m2.mtmt.hu/api/publication/34477101 ID - 34477101 N1 - Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, HUN-REN, Konkoly Thege 15-17, Budapest, 1121, Hungary CSFK, MTA Centre of Excellence, Budapest, Hungary Institute of Physics and Astronomy, ELTE Eötvös Loránd University, Budapest, Hungary Export Date: 04 January 2024; Cited By: 0 LA - English DB - MTMT ER - TY - JOUR AU - Takácsné Farkas, Anikó AU - Kiss, Csaba TI - The Impact of Serpentinization on the Initial Conditions of Satellite Forming Collisions of Large Kuiper Belt Objects JF - PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC J2 - PUBL ASTRON SOC PAC VL - 135 PY - 2023 IS - 1054 SN - 0004-6280 DO - 10.1088/1538-3873/ad0f9a UR - https://m2.mtmt.hu/api/publication/34436348 ID - 34436348 N1 - Funding Agency and Grant Number: Nemzeti Kutatsi Fejlesztsi s Innovcis Hivatalhttps://doi.org/10.13039/501100011019 [K-138962]; National Research, Development and Innovation Office (NKFIH, Hungary) Funding text: This research has been supported by the K-138962 project of the National Research, Development and Innovation Office (NKFIH, Hungary). We are indebted to our referee for the thorough review and the useful comments which have improved the paper considerably. AB - Kuiper Belt objects are thought to be formed at least a few million years after the formation of calcium–aluminum-rich inclusions (CAIs), at a time when the 26 Al isotope—the major source of radiogenic heat in the early solar system—had significantly depleted. The internal structure of these objects is highly dependent on any additional source that can produce extra heat in addition to that produced by the remaining, long-lasting radioactive isotopes. In this paper, we explore how serpentinization, the hydration of silicate minerals, can contribute to the heat budget and to what extent it can modify the internal structure of large Kuiper Belt objects. We find that the extent of restructuring depends very strongly on the start time of the formation process, the size of the object, and the starting ice-to-rock ratio. Serpentinization is able to restructure most of the interior of all objects in the whole size range (400–1200 km) and ice-to-rock ratio range investigated if the process starts early, ∼3 Myr after CAI formation, potentially leading to a predominantly serpentine core much earlier than previously thought (≤5 Myr versus several tens of million years). While the ratio of serpentinized material gradually decreases with the increasing formation time, the increasing ice-to-rock ratio, and the increasing start time of planetesimal formation in the outer solar system, in the case of the largest objects a significant part of the interior will be serpentinized even if the formation starts relatively late, ∼5 Myr after CAI formation. Therefore it is feasible that the interior of planetesimals may have contained a significant amount of serpentine, and in some cases, it could have been a dominant constituent, at the time of satellite-forming impacts. LA - English DB - MTMT ER - TY - JOUR AU - Kalup, Csilla AU - Kiss, Csaba TI - ALMA Band-7 Flux Density Prediction of the Haumea Ring System for Ongoing Observations JF - RESEARCH NOTES OF THE AMERICAN ASTRONOMICAL SOCIETY J2 - RES NOTES AM ASTRO SOC; RN AAS VL - 7 PY - 2023 IS - 9 SN - 2515-5172 DO - 10.3847/2515-5172/acf4f7 UR - https://m2.mtmt.hu/api/publication/34352762 ID - 34352762 AB - In 2017, multi-chord occultation observations found a ring around the dwarf planet (136108) Haumea, and provided direct measurements of the size and an estimate of the apparent opacity of the ring system. Based on these properties, Müller et al. estimated the thermal contribution of Haumea's ring at 20-500 μm. Here, we predict the flux densities of the ring of Haumea at ~870 μm for ongoing measurements with ALMA. LA - English DB - MTMT ER - TY - JOUR AU - Kővári, Emese AU - Forgácsné Dajka, Emese AU - Kovács, Tamás AU - Kiss, Csaba AU - Sándor, Zsolt TI - A dynamical survey of the trans-Neptunian region II.: On the nature of chaotic diffusion JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY: LETTERS J2 - MON NOT ROY ASTRON SOC LETT VL - 524 PY - 2023 IS - 1 SP - L26 EP - L31 PG - 6 SN - 1745-3925 DO - 10.1093/mnrasl/slad063 UR - https://m2.mtmt.hu/api/publication/34015720 ID - 34015720 N1 - Funding Agency and Grant Number: New National Excellence Program of the Ministry for Culture and Innovation from the National Research, Development, and Innovation Fund [uNKP-22-3]; National Research Development and Innovation Office (NKFIH), Hungary [K-138962] Funding text: We acknowledge the computational resources of the GPU Laboratory of the Wigner Research Centre for Physics. Furthermore, EK acknowledges the support of the uNKP-22-3 New National Excellence Program of the Ministry for Culture and Innovation from the source of the National Research, Development, and Innovation Fund. CK was supported by the National Research Development and Innovation Office (NKFIH), Hungary through the grant K-138962. We also thank the reviewer for the valuable comments and suggestions that helped us improve the manuscript. AB - On long enough timescales, chaotic diffusion has the potential to significantly alter the appearance of a dynamical system. The solar system is no exception: diffusive processes take part in the transportation of small bodies and provide dynamical pathways even for the distant trans-Neptunian objects to reach the inner solar system. In this Letter, we carry out a thorough investigation of the nature of chaotic diffusion. We analyze the temporal evolution of the mean squared displacement of ten thousand ensembles of test particles and quantify in each case the diffusion exponent (enabling the classification between normal, sub-, and super-diffusion), the generalized diffusion coefficient, and a characteristic diffusion timescale, too. This latter quantity is compared with an entropy-based timescale, and the two approaches are studied in light of direct computations as well. Our results are given in the context of two-dimensional maps, thereby facilitating the understanding of the relationship between the typical phase space structures and the properties of chaotic diffusion. LA - English DB - MTMT ER - TY - JOUR AU - Forgácsné Dajka, Emese AU - Kővári, Emese AU - Kovács, Tamás AU - Kiss, Csaba AU - Sándor, Zsolt TI - A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune JF - ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES J2 - ASTROPHYS J SUPPL S VL - 266 PY - 2023 IS - 1 PG - 12 SN - 0067-0049 DO - 10.3847/1538-4365/acc4c8 UR - https://m2.mtmt.hu/api/publication/34015359 ID - 34015359 N1 - Kővári E. Wigner FK affiliáció LA - English DB - MTMT ER - TY - JOUR AU - Kecskemethy, Viktoria AU - Kiss, Csaba AU - Szakáts, Róbert AU - Pál, András AU - Szabó M., Gyula AU - Molnár, László AU - Sárneczky, Krisztián AU - Vinkó, József AU - Szabó, Róbert AU - Marton, Gábor AU - Takácsné Farkas, Anikó AU - Kalup, Csilla AU - Kiss, L. László TI - Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope JF - ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES J2 - ASTROPHYS J SUPPL S VL - 264 PY - 2023 IS - 1 PG - 20 SN - 0067-0049 DO - 10.3847/1538-4365/ac9c67 UR - https://m2.mtmt.hu/api/publication/33603304 ID - 33603304 N1 - Funding Agency and Grant Number: National Research, Development and Innovation Office (NKFIH, Hungary) [K-115709, K-138962, PD-116175, KKP-137523, GINOP-2.3.2-15-2016-00003]; Hungarian Academy of Sciences [LP2012-31, LP2018-7/2021]; New National Excellence Programs of the Ministry of Innovation and Technology from the source of the National Research, Development and Innovation Fund [UNKP-19-2, UNKP-20-2, UNKP-21-2]; NASA Science Mission Directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] Funding text: The research leading to these results has received funding from grants K-115709, K-138962, PD-116175, KKP-137523, and GINOP-2.3.2-15-2016-00003 of the National Research, Development and Innovation Office (NKFIH, Hungary) and grants LP2012-31 and LP2018-7/2021 Lendulet of the Hungarian Academy of Sciences. The research leading to these results has been supported by the UNKP-19-2, UNKP-20-2, and UNKP-21-2 New National Excellence Programs of the Ministry of Innovation and Technology from the source of the National Research, Development and Innovation Fund. Funding for the Kepler and K2 missions is provided by the NASA Science Mission Directorate. The data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). The STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has made use of data and services provided by the International Astronomical Union's Minor Planet Center. The authors are thankful for the hospitality of the Veszprem Regional Centre of the Hungarian Academy of Sciences (MTA VEAB), where part of this project was carried out. We are also thankful to our reviewers for their fair and balanced reports. AB - The K2 mission of the Kepler Space Telescope allowed the observations of light curves of small solar system bodies throughout the whole solar system. In this paper, we present the results of a collection of K2 trans-Neptunian object observations between campaigns C03 (2014 November-2015 February) and C19 (2018 August-September), which includes 66 targets. Due to the faintness of our targets, the detectability rate of a light-curve period is similar to 56%, notably lower than in the case of other small-body populations, like Hildas or Jovian Trojans. We managed to obtain light-curve periods with an acceptable confidence for 37 targets; the majority of these cases are new identifications. We were able to give light-curve amplitude upper limits for the other 29 targets. Several of the newly detected light-curve periods are longer than similar to 24 hr, in many cases close to similar to 80 hr; i.e., these targets are slow rotators. This relative abundance of slowly rotating objects is similar to that observed among Hildas, Jovian Trojans, and Centaurs in the K2 mission, as well as among main belt asteroids measured with the TESS space telescope. Trans-Neptunian objects show notably higher light-curve amplitudes at large (D greater than or similar to 300 km) sizes than found among large main belt asteroids, in contrast to the general expectation that due to their lower compressive strength, they reach hydrostatic equilibrium at smaller sizes than their inner solar system counterparts. LA - English DB - MTMT ER - TY - JOUR AU - Szakáts, Róbert AU - Kiss, Csaba AU - Ortiz, J. L. AU - Morales, N. AU - Pál, András AU - Müller, T. G. AU - Greiner, J. AU - Santos-Sanz, P. AU - Marton, Gábor AU - Duffard, R. AU - Sági, P. AU - Forgácsné Dajka, Emese TI - Tidally locked rotation of the dwarf planet (136199) Eris discovered via long-term ground-based and space photometry JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 669 PY - 2023 PG - 13 SN - 0004-6361 DO - 10.1051/0004-6361/202245234 UR - https://m2.mtmt.hu/api/publication/33565585 ID - 33565585 N1 - Export Date: 08 March 2024; CODEN: AAEJA AB - The rotational states of the members in the dwarf planet-satellite systems in the trans-Neptunian region are determined by formation conditions and the tidal interaction between the components. These rotational characteristics serve as prime tracers of their evolution. A number of authors have claimed a very broad range of values for the rotation period for the dwarf planet Eris, ranging from a few hours to a rotation that is (nearly) synchronous with the orbital period (15.8 d) of its satellite, Dysnomia. In this Letter, we present new light curve data for Eris, taken with ∼1–2 m-class ground based telescopes and with the TESS and Gaia space telescopes. The TESS data did not provide a well-defined light curve period, but it could be used to constrain light curve variations to a maximum possible light curve amplitude of Δ m ≤ 0.03 mag (1- σ ) for P ≤ 24 h periods. Both the combined ground-based data and Gaia measurements unambiguously point to a light curve period equal to the orbital period of Dysnomia, P = 15.8 d, with a light curve amplitude of Δ m ≈ 0.03 mag, indicating that the rotation of Eris is tidally locked. Assuming that Dysnomia has a collisional origin, calculations with a simple tidal evolution model show that Dysnomia must be relatively massive (mass ratio of q = 0.01–0.03) and large (radius of R s ≥ 300 km) to have the potential to slow Eris down to a synchronised rotation. These simulations also indicate that (assuming tidal parameters usually considered for trans-Neptunian objects) the density of Dysnomia should be 1.8–2.4 g cm −3 . This is an exceptionally high value among similarly sized trans-Neptunian objects, setting important constraints on their formation conditions. LA - English DB - MTMT ER - TY - CHAP AU - Nagy, Zsófia AU - Ábrahám, Péter AU - Kóspál, Ágnes AU - Szabados, László AU - Fernando, Cruz-Saenz de Miera AU - Fiorellino, Elenonora AU - Kiss, Csaba AU - Kun, Mária AU - Marton, Gábor AU - Park, Sunkyung AU - Siwak, Michal AU - Szabó, Zsófia AU - Szegedi-Elek, Elza ED - Frey, Sándor TI - Fiatal csillagok vizsgálata a Gaia űrtávcső adatai alapján T2 - Űrtan Évkönyv 2021 PB - Magyar Asztronautikai Társaság CY - Budapest T3 - Asztronautikai Tájékoztató, ISSN 1788-7771 ; 73. PY - 2022 SP - 63 EP - 68 PG - 6 UR - https://m2.mtmt.hu/api/publication/33561129 ID - 33561129 LA - Hungarian DB - MTMT ER -