@article{MTMT:34566634,
	title = {Abundant sub-micron grains revealed in newly discovered extreme debris discs},
	url = {https://m2.mtmt.hu/api/publication/34566634},
	author = {Moór, Attila and Ábrahám, Péter and Su, K Y L and Henning, T and Marino, S and Chen, Lei and Kóspál, Ágnes and Pawellek, Nicole and Varga, József and Vida, Krisztián},
	doi = {10.1093/mnras/stae155},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {528},
	unique-id = {34566634},
	issn = {0035-8711},
	abstract = {Extreme debris discs (EDDs) are bright and warm circumstellar dusty structures around main sequence stars. They may represent the outcome of giant collisions occuring in the terrestrial region between large planetesimals or planetary bodies, and thus provide a rare opportunity to peer into the aftermaths of these events. Here, we report on results of a mini-survey we conducted with the aim to increase the number of known EDDs, investigate the presence of solid-state features around 10 μm in eight EDDs, and classify them into the silica or silicate dominated groups. We identify four new EDDs and derive their fundamental properties. For these, and for four other previously known discs, we study the spectral energy distribution around 10 μm by means of VLT/VISIR photometryin three narrow-band filters and conclude that all eight objects likely exhibit solid-state emission features from sub-micron grains. We find that four discs probably belong to the silicate dominated subgroup. Considering the age distribution of the entire EDD sample, we find that their incidence begins to decrease only after 300 Myr, suggesting that the earlier common picture that these objects are related to the formation of rocky planets may not be exclusive, and that other processes may be involved for older objects (≳100 Myr). Because most of the older EDD systems have wide, eccentric companions, we suggest that binarity may play a role in triggering late giant collisions.},
	year = {2024},
	eissn = {1365-2966},
	pages = {4528-4546},
	orcid-numbers = {Marino, S/0000-0002-5352-2924}
}

@article{MTMT:34498310,
	title = {Mid-infrared evidence for iron-rich dust in the multi-ringed inner disk of HD 144432},
	url = {https://m2.mtmt.hu/api/publication/34498310},
	author = {Varga, József and Waters, L. B. F. M. and Hogerheijde, M. and van Boekel, R. and Matter, A. and Lopez, B. and Perraut, K. and Chen, Lei and Nadella, D. and Wolf, S. and Dominik, C. and Kóspál, Ágnes and Ábrahám, Péter and Augereau, J.-C. and Boley, P. and Bourdarot, G. and Caratti o Garatti, A. and Fernando, Cruz-Saenz de Miera and Danchi, W. C. and Gámez Rosas, V. and Henning, Th. and Hofmann, K.-H. and Houllé, M. and Isbell, J. W. and Jaffe, W. and Juhász, T. and Kecskeméthy, V. and Kobus, J. and Kokoulina, E. and Labadie, L. and Lykou, Foteini and Millour, F. and Moór, Attila and Morujão, N. and Pantin, E. and Schertl, D. and Scheuck, M. and van Haastere, L. and Weigelt, G. and Woillez, J. and Woitke, P.},
	doi = {10.1051/0004-6361/202347535},
	journal-iso = {ASTRON ASTROPHYS},
	journal = {ASTRONOMY & ASTROPHYSICS},
	volume = {681},
	unique-id = {34498310},
	issn = {0004-6361},
	abstract = {Context. Rocky planets form by the concentration of solid particles in the inner few au regions of planet-forming disks. Their chemical composition reflects the materials in the disk available in the solid phase at the time the planets were forming. Studying the dust before it gets incorporated in planets provides a valuable diagnostic for the material composition.},
	year = {2024},
	eissn = {1432-0746},
	orcid-numbers = {Dominik, C./0000-0002-3393-2459; Boley, P./0000-0001-7923-2979; Caratti o Garatti, A./0000-0001-8876-6614; Isbell, J. W./0000-0002-1272-6322; Kecskeméthy, V./0000-0002-9511-0901}
}

@article{MTMT:34435056,
	title = {The debris disc of HD 131488: bringing together thermal emission and scattered light},
	url = {https://m2.mtmt.hu/api/publication/34435056},
	author = {Pawellek, Nicole and Moór, Attila and Kirchschlager, F. and Milli, J. and Kóspál, Ágnes and Ábrahám, Péter and Marino, S. and Wyatt, M. and Rebollido, I. and Hughes, A.M. and Cantalloube, F. and Henning, T.},
	doi = {10.1093/mnras/stad3455},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {527},
	unique-id = {34435056},
	issn = {0035-8711},
	year = {2024},
	eissn = {1365-2966},
	pages = {3559-3584}
}

@article{MTMT:34079891,
	title = {Gaia21bty: An EXor lightcurve exhibiting an FUor spectrum},
	url = {https://m2.mtmt.hu/api/publication/34079891},
	author = {Siwak, Michal and Hillenbrand, Lynne A. and Kóspál, Ágnes and Ábrahám, Péter and Giannini, Teresa and De, Kishalay and Moór, Attila and Szilágyi, Máté and Janík, Jan and Koen, Chris and Park, Sunkyung and Nagy, Zsófia and Fernando, Cruz-Saenz de Miera and Fiorellino, Elenonora and Marton, Gábor and Kun, Mária and Lucas, Philip W. and Udalski, Andrzej and Szabó, Zsófia Marianna},
	doi = {10.1093/mnras/stad2135},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {524},
	unique-id = {34079891},
	issn = {0035-8711},
	abstract = {Gaia21bty, a pre-main sequence star that previously had shown aperiodic dips in its light curve, underwent a considerable ΔG ≈ 2.9 mag brightening that occurred over a few months between 2020 October - 2021 February. The Gaia lightcurve shows that the star remained near maximum brightness for about 4 - 6 months, and then started slowly fading over the next 2 years, with at least three superimposed ~1 mag sudden rebrightening events. Whereas the amplitude and duration of the maximum is typical for EXors, optical and near-infrared spectra obtained at the maximum are dominated by features which are typical for FUors. Modelling of the accretion disc at the maximum indicates that the disc bolometric luminosity is 43 L⊙ and the mass accretion rate is 2.5 × 10-5 M⊙ yr-1, which are typical values for FUors even considering the large uncertainty in the distance ($1.7_{-0.4}^{+0.8}$ kpc). Further monitoring is necessary to understand the cause of the quick brightness decline, the rebrightening, and the other post-outburst light changes, as our multi-colour photometric data suggest that they could be caused by a long and discontinuous obscuration event. We speculate that the outburst might have induced large-scale inhomogeneous dust condensations in the line of sight leading to such phenomena, whilst the FUor outburst continues behind the opaque screen.},
	keywords = {ACCRETION; Astrophysics - Solar and Stellar Astrophysics; stars: pre-main-sequence; stars: formation; accretion discs; Astrophysics - Earth and Planetary Astrophysics; Herbig Ae/Be; stars: variables: T Tauri},
	year = {2023},
	eissn = {1365-2966},
	pages = {5548-5565},
	orcid-numbers = {Szilágyi, Máté/0000-0002-3648-433X}
}

@article{MTMT:34070188,
	title = {Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*},
	url = {https://m2.mtmt.hu/api/publication/34070188},
	author = {Cataldi, Gianni and Aikawa, Yuri and Iwasaki, Kazunari and Marino, Sebastian and Brandeker, Alexis and Hales, Antonio and Henning, Thomas and Higuchi, Aya E. and Hughes, A. Meredith and Janson, Markus and Kral, Quentin and Matrà, Luca and Moór, Attila and Olofsson, Göran and Redfield, Seth and Roberge, Aki},
	doi = {10.3847/1538-4357/acd6f3},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {951},
	unique-id = {34070188},
	issn = {1538-4357},
	abstract = {The origin and evolution of gas in debris disks are still not well understood. Secondary gas production from cometary material or a primordial origin have been proposed. So far, observations have mostly concentrated on CO, with only a few C observations available. We overview the C and CO content of debris disk gas and test state-of-the-art models. We use new and archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO and C i emission, complemented by C ii data from Herschel, for a sample of 14 debris disks. This expands the number of disks with ALMA measurements of both CO and C i by 10 disks. We present new detections of C i emission toward three disks: HD 21997, HD 121191, and HD 121617. We use a simple disk model to derive gas masses and column densities. We find that current state-of-the-art models of secondary gas production overpredict the C 0 content of debris disk gas. This does not rule out a secondary origin, but might indicate that the models require an additional C removal process. Alternatively, the gas might be produced in transient events rather than a steady-state collisional cascade. We also test a primordial gas origin by comparing our results to a simplified thermochemical model. This yields promising results, but more detailed work is required before a conclusion can be reached. Our work demonstrates that the combination of C and CO data is a powerful tool to advance our understanding of debris disk gas.},
	year = {2023},
	eissn = {0004-637X},
	orcid-numbers = {Cataldi, Gianni/0000-0002-2700-9676; Aikawa, Yuri/0000-0003-3283-6884; Iwasaki, Kazunari/0000-0002-2707-7548; Marino, Sebastian/0000-0002-5352-2924; Brandeker, Alexis/0000-0002-7201-7536; Hales, Antonio/0000-0001-5073-2849; Henning, Thomas/0000-0002-1493-300X; Higuchi, Aya E./0000-0002-9221-2910; Hughes, A. Meredith/0000-0002-4803-6200; Janson, Markus/0000-0001-8345-593X; Kral, Quentin/0000-0001-6527-4684; Matrà, Luca/0000-0003-4705-3188; Olofsson, Göran/0000-0003-3747-7120; Redfield, Seth/0000-0003-3786-3486; Roberge, Aki/0000-0002-2989-3725}
}

@article{MTMT:33758671,
	title = {The Detection of a Compact Radio Feature in a Seyfert Galaxy After an Accretion Rate Change},
	url = {https://m2.mtmt.hu/api/publication/33758671},
	author = {Gabányi, Krisztina Éva and Smith, K. and Frey, Sándor and Paragi, Zsolt and An, T. and Moór, Attila},
	doi = {10.22323/1.428.0006},
	journal-iso = {POS - PROCEEDINGS OF SCIENCE},
	journal = {POS - PROCEEDINGS OF SCIENCE},
	volume = {428},
	unique-id = {33758671},
	issn = {1824-8039},
	year = {2023},
	orcid-numbers = {Gabányi, Krisztina Éva/0000-0003-1020-1597; Frey, Sándor/0000-0003-3079-1889}
}

@misc{MTMT:33729197,
	title = {VizieR Online Data Catalog: Opt-to-IR monitoring obs. of V1057 Cyg (Szabo+, 2021)},
	url = {https://m2.mtmt.hu/api/publication/33729197},
	author = {Szabo, Z. M. and Kóspál, Ágnes and Ábrahám, Péter and Park, Sunkyung and Siwak, Michal and Green, J. D. and Moór, Attila and Pál, András and Acosta-Pulido, J. A. and Lee, J. -E. and Cseh, B. and Csornyei, G. and Hanyecz, O. and Könyves-Tóth, Réka and Krezinger, M. and Kriskovics, Levente and Ordasi, A. and Sárneczky, Krisztián and Seli, B. and Szakáts, Róbert and Szing, A. and Vida, Krisztián},
	unique-id = {33729197},
	abstract = {We performed the majority of our photometric observations in B, V, RC, IC , g', r', and i' filters at the Piszkesteto Mountain Station of Konkoly Observatory (Hungary) between 2005 and 2021. Three telescopes with three slightly different optical systems were used: the 1m Ritchey-Chretien-coude (RCC) telescope, the 60/90/180cm Schmidt telescope and the Astro Systeme Austria AZ800 alt-azimuth direct drive 80cm Ritchey-Chretien (RC80) telescope; see Section 2.1. In addition to our national facilities, we occasionally used other telescopes. On 2006 July 20 and 2012 October 13 we obtained B, V, RJ, and IJ images of V1057 Cyg with the IAC80 telescope of the Instituto de Astrofisica de Canarias located at Teide Observatory (Canary Islands, Spain). During 2019 August-September, in parallel with TESS, we additionally observed V1057 Cyg at the Northern Skies Observatory (NSO). We used the 0.4m telescope equipped with BVI filters. We also observed V1057 Cyg with the 2.56m Nordic Optical Telescope (NOT) at the Roque de los Muchachos Observatory, La Palma, in the Canary Islands (Plan ID 61-414, PI: Zs. M. Szabo). For optical imaging we used the Alhambra Faint Object Spectrograph and Camera (ALFOSC) on 2020 August 17. The Bessel BVR filter set was supplemented by an i interference filter, which is similar to the SLOAN i', but with a slightly longer effective wavelength of λeff=0.789um. We obtained NIR images in the J, H, and Ks bands at six epochs between 2006 July 15 and 2012 October 13 using the 1.52m Telescopio Carlos Sanchez (TCS) at the Teide Observatory. We also used the NOTCam instrument on the NOT on 2020 August 29. See Section 2.3. We obtained a new optical spectrum of V1057 Cyg with the high-resolution FIbre-fed Echelle Spectrograph (FIES) instrument on the NOT on 2020 August 17. We used a fiber with a larger entrance aperture of 2.5", which provided a spectral resolution R=25000, covering the 370-900nm wavelength range. V1057 Cyg was also observed with the Bohyunsan Optical Echelle Spectrograph (BOES) installed on the 1.8m telescope at the Bohyunsan Optical Astronomy Observatory (BOAO). It provides R=30000 in the wavelength range ~400-900nm. The first spectrum was obtained on 2012-September-11 and the last on 2018-December-18. See Section 2.4. On 2020 August 29, we used the NOTCam on the NOT to obtain new NIR spectra of V1057 Cyg and Iot Cyg (A5 V) as our telluric standard star in the JHKs bands. We used the low-resolution camera mode (R=2500). See Section 2.5. On 2018 September 6, we observed V1057 Cyg with the Stratospheric Observatory for Infrared Astronomy (SOFIA) using the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST). We obtained mid-infrared imaging in a series of short exposures in band F111 (10.6-11.6um) totaling ~30s, a single exposure in F056 (5.6um) for 37s and F077 (7.5-8um) for 42s, and R~100-200 spectra with G063 (5-8um) and G227 (17-27um) (Plan ID 06_062, PI: J. D. Green). See Section 2.6. (2 data files).},
	keywords = {stars: pre-main sequence; Photometry: UBVRI; Spectra: infrared},
	year = {2023}
}

@article{MTMT:33535919,
	title = {Erratum: “A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog” (2021, ApJ, 910, 27)},
	url = {https://m2.mtmt.hu/api/publication/33535919},
	author = {Moór, Attila and Ábrahám, Péter and Szabó M., Gyula and Vida, Krisztián and Cataldi, Gianni and Derekas, Alíz and Henning, Thomas and Kinemuchi, Karen and Kóspál, Ágnes and Kovács, József and Pál, András and Sarkis, Paula and Seli, Bálint Attila and Szabó, Zsófia M. and Takáts, Katalin},
	doi = {10.3847/1538-4357/aca280},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {940},
	unique-id = {33535919},
	issn = {1538-4357},
	year = {2022},
	eissn = {0004-637X},
	orcid-numbers = {Szabó M., Gyula/0000-0002-0606-7930; Cataldi, Gianni/0000-0002-2700-9676; Derekas, Alíz/0000-0002-6526-9444; Henning, Thomas/0000-0002-1493-300X; Kinemuchi, Karen/0000-0001-7908-7724; Sarkis, Paula/0000-0001-8128-3126; Seli, Bálint Attila/0000-0002-3658-2175; Szabó, Zsófia M./0000-0001-9830-3509}
}

@article{MTMT:33108812,
	title = {Mid-infrared time-domain study of recent dust production events in the extreme debris disc of TYC 4209-1322-1},
	url = {https://m2.mtmt.hu/api/publication/33108812},
	author = {Moór, Attila and Ábrahám, Péter and Kóspál, Ágnes and Su, Kate Y. L. and Rieke, George H. and Vida, Krisztián and Cataldi, Gianni and Bódi, Attila and Sódorné Bognár, Zsófia and Cseh, Borbála and Csörnyei, Géza and Egei, Nóra and Farkas, Anikó and Hanyecz, Ottó and Ignácz, Bernadett and Kalup, Csilla and Könyves-Tóth, Réka and Kriskovics, Levente and Mészáros, László and Pál, András and Ordasi, András and Sárneczky, Krisztián and Seli, Bálint Attila and Sódor, Ádám and Szakáts, Róbert and Vinkó, József and Zsidi, Gabriella},
	doi = {10.1093/mnras/stac2595},
	journal-iso = {MON NOT R ASTRON SOC},
	journal = {MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY},
	volume = {516},
	unique-id = {33108812},
	issn = {0035-8711},
	abstract = {Extreme debris discs are characterized by unusually strong mid-infrared excess emission, which often proves to be variable. The warm dust in these discs is of transient nature and is likely related to a recent giant collision occurring close to the star in the terrestrial region. Here we present the results of a 877 days long, gap-free photometric monitoring performed by the Spitzer Space Telescope of the recently discovered extreme debris disc around TYC 4209-1322-1. By combining these observations with other time-domain optical and mid-infrared data, we explore the disc variability of the last four decades, with particular emphasis on the last 12 years. During the latter interval the disc showed substantial changes, the most significant was the brightening and subsequent fading between 2014 and 2018 as outlined in WISE data. The Spitzer light curves outline the fading phase and a subsequent new brightening of the disc after 2018, revealing an additional flux modulation with a period of ~39 days on top of the long-term trend. We found that all these variations can be interpreted as the outcome of a giant collision that happened at an orbital radius of ~0.3 au sometime in 2014. Our analysis implies that a collision on a similar scale could have taken place around 2010, too. The fact that the disc was already peculiarly dust rich 40 years ago, as implied by IRAS data, suggests that these dust production events belong to a chain of large impacts triggered by an earlier even more catastrophic collision.},
	keywords = {infrared: planetary systems; (stars:) circumstellar matter; stars: individual: TYC 4209-1322-1},
	year = {2022},
	eissn = {1365-2966},
	pages = {5684-5701},
	orcid-numbers = {Bódi, Attila/0000-0002-8585-4544; Seli, Bálint Attila/0000-0002-3658-2175; Vinkó, József/0000-0001-8764-7832}
}

@article{MTMT:33076006,
	title = {Multiwavelength Vertical Structure in the AU Mic Debris Disk: Characterizing the Collisional Cascade},
	url = {https://m2.mtmt.hu/api/publication/33076006},
	author = {Vizgan, David and Meredith, Hughes A. and Carter, Evan S. and Flaherty, Kevin M. and Pan, Margaret and Chiang, Eugene and Schlichting, Hilke and Wilner, David J. and Andrews, Sean M. and Carpenter, John M. and Moór, Attila and MacGregor, Meredith A.},
	doi = {10.3847/1538-4357/ac80b8},
	journal-iso = {ASTROPHYS J},
	journal = {ASTROPHYSICAL JOURNAL},
	volume = {935},
	unique-id = {33076006},
	issn = {1538-4357},
	abstract = {Debris disks are scaled-up analogs of the Kuiper Belt in which dust is generated by collisions between planetesimals. In the collisional cascade model of debris disks, the dust lost to radiation pressure and winds is constantly replenished by grinding collisions between planetesimals. The model assumes that collisions are destructive and involve large velocities; this assumption has not been tested beyond our solar system. We present 0.″25 (≍2.4 au) resolution observations of the λ = 450 μm dust continuum emission from the debris disk around the nearby M dwarf AU Microscopii with the Atacama Large Millimeter/submillimeter Array. We use parametric models to describe the disk structure, and a Monte Carlo Markov Chain (MCMC) algorithm to explore the posterior distributions of the model parameters; we fit the structure of the disk to both our data and archival λ = 1.3 mm data (Daley et al. 2019), from which we obtain two aspect ratio measurements at 1.3 mm (h 1300 = ${0.025}_{-0.002}^{+0.008}$ ) and at 450 μm (h 450 = ${0.019}_{-0.001}^{+0.006}$ ), as well as the grain-size distribution index q = 3.03 ± 0.02. Contextualizing our aspect ratio measurements within the modeling framework laid out in Pan & Schlichting (2012), we derive a power-law index of velocity dispersion as a function of grain size p = 0.28 ± 0.06 for the AU Mic debris disk. This result implies that smaller bodies are more easily disrupted than larger bodies by collisions, which is inconsistent with the strength regime usually assumed for such small bodies. Possible explanations for this discrepancy are discussed.},
	keywords = {Astrophysics - Solar and Stellar Astrophysics; CIRCUMSTELLAR DISKS; Astrophysics - Earth and Planetary Astrophysics; Debris disks; M dwarf stars; 982; 363; 235},
	year = {2022},
	eissn = {0004-637X}
}