@article{MTMT:34493622,
	title = {Radiative transfer modelling of Haumea's dust ring},
	url = {https://m2.mtmt.hu/api/publication/34493622},
	author = {Kalup, Csilla and Kiss, Csaba},
	journal-iso = {BULL AM ASTRON SOC},
	journal = {BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY},
	volume = {55},
	unique-id = {34493622},
	issn = {0002-7537},
	abstract = {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.},
	year = {2023}
}

@article{MTMT:34493621,
	title = {Light curves of Jovian Trojan asteroids from the TESS mission},
	url = {https://m2.mtmt.hu/api/publication/34493621},
	author = {Kiss, Csaba and Takacs, Nora and Szakáts, Róbert and Pál, András},
	journal-iso = {BULL AM ASTRON SOC},
	journal = {BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY},
	volume = {55},
	unique-id = {34493621},
	issn = {0002-7537},
	abstract = {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.},
	year = {2023}
}

@article{MTMT:34477101,
	title = {Rotational Phase Dependent J − H Colour of the Dwarf Planet Eris},
	url = {https://m2.mtmt.hu/api/publication/34477101},
	author = {Szakáts, Róbert and Kiss, Csaba},
	doi = {10.1088/1538-3873/ad0b31},
	journal-iso = {PUBL ASTRON SOC PAC},
	journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC},
	volume = {135},
	unique-id = {34477101},
	issn = {0004-6280},
	year = {2023},
	eissn = {1538-3873}
}

@article{MTMT:34436348,
	title = {The Impact of Serpentinization on the Initial Conditions of Satellite Forming Collisions of Large Kuiper Belt Objects},
	url = {https://m2.mtmt.hu/api/publication/34436348},
	author = {Takácsné Farkas, Anikó and Kiss, Csaba},
	doi = {10.1088/1538-3873/ad0f9a},
	journal-iso = {PUBL ASTRON SOC PAC},
	journal = {PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC},
	volume = {135},
	unique-id = {34436348},
	issn = {0004-6280},
	abstract = {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.},
	year = {2023},
	eissn = {1538-3873}
}

@article{MTMT:34352762,
	title = {ALMA Band-7 Flux Density Prediction of the Haumea Ring System for Ongoing Observations},
	url = {https://m2.mtmt.hu/api/publication/34352762},
	author = {Kalup, Csilla and Kiss, Csaba},
	doi = {10.3847/2515-5172/acf4f7},
	journal-iso = {RES NOTES AM ASTRO SOC; RN AAS},
	journal = {RESEARCH NOTES OF THE AMERICAN ASTRONOMICAL SOCIETY},
	volume = {7},
	unique-id = {34352762},
	issn = {2515-5172},
	abstract = {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.},
	keywords = {Small solar system bodies; 1469},
	year = {2023},
	eissn = {2515-5172}
}

@article{MTMT:34015720,
	title = {A dynamical survey of the trans-Neptunian region II.: On the nature of chaotic diffusion},
	url = {https://m2.mtmt.hu/api/publication/34015720},
	author = {Kővári, Emese and Forgácsné Dajka, Emese and Kovács, Tamás and Kiss, Csaba and Sándor, Zsolt},
	doi = {10.1093/mnrasl/slad063},
	journal-iso = {MON NOT ROY ASTRON SOC LETT},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY: LETTERS},
	volume = {524},
	unique-id = {34015720},
	issn = {1745-3925},
	abstract = {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.},
	year = {2023},
	eissn = {1745-3933},
	pages = {L26-L31},
	orcid-numbers = {Forgácsné Dajka, Emese/0000-0002-5735-6273; Kovács, Tamás/0000-0002-0697-6050; Sándor, Zsolt/0000-0003-1216-913X}
}

@article{MTMT:34015359,
	title = {A Dynamical Survey of the Trans-Neptunian Region. I. Mean-motion Resonances with Neptune},
	url = {https://m2.mtmt.hu/api/publication/34015359},
	author = {Forgácsné Dajka, Emese and Kővári, Emese and Kovács, Tamás and Kiss, Csaba and Sándor, Zsolt},
	doi = {10.3847/1538-4365/acc4c8},
	journal-iso = {ASTROPHYS J SUPPL S},
	journal = {ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES},
	volume = {266},
	unique-id = {34015359},
	issn = {0067-0049},
	year = {2023},
	eissn = {1538-4365},
	orcid-numbers = {Forgácsné Dajka, Emese/0000-0002-5735-6273; Kovács, Tamás/0000-0002-0697-6050; Sándor, Zsolt/0000-0003-1216-913X}
}

@article{MTMT:33603304,
	title = {Light Curves of Trans-Neptunian Objects from the K2 Mission of the Kepler Space Telescope},
	url = {https://m2.mtmt.hu/api/publication/33603304},
	author = {Kecskemethy, Viktoria and Kiss, Csaba and Szakáts, Róbert and Pál, András and Szabó M., Gyula and Molnár, László and Sárneczky, Krisztián and Vinkó, József and Szabó, Róbert and Marton, Gábor and Takácsné Farkas, Anikó and Kalup, Csilla and Kiss, L. László},
	doi = {10.3847/1538-4365/ac9c67},
	journal-iso = {ASTROPHYS J SUPPL S},
	journal = {ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES},
	volume = {264},
	unique-id = {33603304},
	issn = {0067-0049},
	abstract = {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.},
	year = {2023},
	eissn = {1538-4365},
	orcid-numbers = {Szabó M., Gyula/0000-0002-0606-7930; Vinkó, József/0000-0001-8764-7832; Szabó, Róbert/0000-0002-3258-1909; Kiss, L. László/0000-0002-3234-1374}
}

@article{MTMT:33565585,
	title = {Tidally locked rotation of the dwarf planet (136199) Eris discovered via long-term ground-based and space photometry},
	url = {https://m2.mtmt.hu/api/publication/33565585},
	author = {Szakáts, Róbert and Kiss, Csaba and Ortiz, J. L. and Morales, N. and Pál, András and Müller, T. G. and Greiner, J. and Santos-Sanz, P. and Marton, Gábor and Duffard, R. and Sági, P. and Forgácsné Dajka, Emese},
	doi = {10.1051/0004-6361/202245234},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {669},
	unique-id = {33565585},
	issn = {0004-6361},
	abstract = {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.},
	year = {2023},
	eissn = {1432-0746},
	orcid-numbers = {Ortiz, J. L./0000-0002-8690-2413; Morales, N./0000-0003-0419-1599; Müller, T. G./0000-0002-0717-0462; Greiner, J./0000-0002-9875-426X; Santos-Sanz, P./0000-0002-1123-983X; Duffard, R./0000-0001-5963-5850; Sági, P./0000-0001-7549-0348; Forgácsné Dajka, Emese/0000-0002-5735-6273}
}

@{MTMT:33561129,
	title = {Fiatal csillagok vizsgálata a Gaia űrtávcső adatai alapján},
	url = {https://m2.mtmt.hu/api/publication/33561129},
	author = {Nagy, Zsófia and Ábrahám, Péter and Kóspál, Ágnes and Szabados, László and Fernando, Cruz-Saenz de Miera and Fiorellino, Elenonora and Kiss, Csaba and Kun, Mária and Marton, Gábor and Park, Sunkyung and Siwak, Michal and Szabó, Zsófia and Szegedi-Elek, Elza},
	booktitle = {Űrtan Évkönyv 2021},
	unique-id = {33561129},
	year = {2022},
	pages = {63-68}
}