TY - JOUR AU - Könyves-Tóth, Réka AU - Seli, Bálint Attila TI - Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity? JF - ASTROPHYSICAL JOURNAL J2 - ASTROPHYS J VL - 954 PY - 2023 IS - 1 PG - 16 SN - 1538-4357 DO - 10.3847/1538-4357/ace787 UR - https://m2.mtmt.hu/api/publication/34125272 ID - 34125272 AB - In this study, we analyze the postmaximum spectra of a sample of 27 Type I superluminous supernovae (SLSNe-I) in order to search for physical differences between the so-called Type W and Type 15bn subtypes. This paper is a continuation of Konyves-Toth & Vinko and Konyves-Toth. In the former, it was revealed that not all SLSNe-I show the W-shaped absorption feature between 4000 and 5000 & ANGS; in the premaximum spectra, and two new SLSN subgroups were disclosed. In the latter, physical differences in the premaximum phases were studied. For completeness, postmaximum data are analyzed in this paper. It is concluded that in terms of photospheric temperature and velocity, Type W and Type 15bn SLSNe-I decrease to a similar value by the postmaximum phases, and their pseudo-nebular spectra are nearly uniform. The relation between the photometric and spectroscopic phases (& phi;) between the two subgroups was examined, and it was found that the & phi; of Type W SLSNe-I increases monotonically with time, while Type 15bn objects tend to show larger & phi; before peak brightness, which evolves slowly. Pseudo-equivalent width (pEW) calculations show that the pEWs of the wavelength range between 4166 and 5266 & ANGS; evolve differently in the cases of the two subtypes, while the other parts of the spectra seem to evolve similarly. It was found that the host galaxies of the studied objects do not differ significantly in their star formation rate, morphology, stellar mass, and absolute brightness. The main difference behind the bimodality of Type W and Type 15bn SLSNe-I therefore is in their premaximum evolution. LA - English DB - MTMT ER - TY - JOUR AU - Kriskovics, Levente AU - Kővári, Zsolt AU - Seli, Bálint Attila AU - Oláh, Katalin Ilona AU - Vida, Krisztián AU - Henry, G. W. AU - Granzer, T. AU - Görgei, A. TI - EI Eridani: A star under the influence. The effect of magnetic activity in the short and long term JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 674 PY - 2023 SN - 0004-6361 DO - 10.1051/0004-6361/202245767 UR - https://m2.mtmt.hu/api/publication/34053151 ID - 34053151 N1 - Funding Agency and Grant Number: Hungarian National Research, Development and Innovation Office [OTKA K-131508, KKP-143986, 2019-2.1.11-TeT-2019-00056]; Bolyai+ [UNKP-22-5-ELTE-1093]; DNew National Excellence Program of the Ministry for Culture and Innovation from the source of the National Research, Development and Innovation Fund; NASA; NSF; State of Tennessee through its Centers of Excellence Program Funding text: The authors would like to thank Albert Washuettl and the original MUSICOS team for organizing and gathering the data used in this work. The authors acknowledge the Hungarian National Research, Development and Innovation Office grants OTKA K-131508, KKP-143986 (Elvonal), and 2019-2.1.11-TeT-2019-00056. L.K. acknowledges the Hungarian National Research, Development and Innovation Office grant OTKA PD-134784. L.K. and K.V. are Bolyai Janos research Fellows. K.V. is supported by the Bolyai+ grant UNKP-22-5-ELTE-1093, BS is supported by 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. G.W.K. acknowledges long-term support from NASA, NSF, and the State of Tennessee through its Centers of Excellence Program. AB - Context. Homogeneous photometric time series spanning decades provide a unique opportunity to study the long-term cyclic behavior of active spotted stars such as our target EI Eridani. In addition, with ultraprecise space photometry data, it is possible to investigate the accompanying flare activity in detail. However, the rotation period of ≈2 days for EI Eri makes it impossible to achieve time-resolved surface images from a single ground-based observing site. Therefore, for this purpose, spectroscopic data from a multi-site observing campaign are needed. LA - English DB - MTMT ER - TY - JOUR AU - Oláh, Katalin Ilona AU - Seli, Bálint Attila AU - Kővári, Zsolt AU - Kriskovics, Levente AU - Vida, Krisztián TI - Characteristics of flares on giant stars JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 668 PY - 2022 SN - 0004-6361 DO - 10.1051/0004-6361/202243789 UR - https://m2.mtmt.hu/api/publication/33538419 ID - 33538419 N1 - Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklós út 15-17, Budapest, 1121, Hungary Csfk, Mta Centre of Excellence, Budapest, Konkoly Thege Miklós út 15-17, Budapest, 1121, Hungary Eötvös University, Department of Astronomy, Pf. 32, Budapest, 1518, Hungary Cited By :1 Export Date: 13 October 2023 CODEN: AAEJA AB - Context. Although late-type dwarfs and giant stars are substantially different, their flares are thought to originate in similar physical processes and differ only by a scale factor in the energy levels. We study the validity of this approach. LA - English DB - MTMT ER - TY - JOUR AU - Moór, Attila AU - Ábrahám, Péter AU - Szabó M., Gyula AU - Vida, Krisztián AU - Cataldi, Gianni AU - Derekas, Alíz AU - Henning, Thomas AU - Kinemuchi, Karen AU - Kóspál, Ágnes AU - Kovács, József AU - Pál, András AU - Sarkis, Paula AU - Seli, Bálint Attila AU - Szabó, Zsófia M. AU - Takáts, Katalin TI - Erratum: “A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog” (2021, ApJ, 910, 27) JF - ASTROPHYSICAL JOURNAL J2 - ASTROPHYS J VL - 940 PY - 2022 IS - 2 SN - 1538-4357 DO - 10.3847/1538-4357/aca280 UR - https://m2.mtmt.hu/api/publication/33535919 ID - 33535919 LA - English DB - MTMT ER - TY - JOUR AU - Moór, Attila AU - Ábrahám, Péter AU - Kóspál, Ágnes AU - Su, Kate Y. L. AU - Rieke, George H. AU - Vida, Krisztián AU - Cataldi, Gianni AU - Bódi, Attila AU - Sódorné Bognár, Zsófia AU - Cseh, Borbála AU - Csörnyei, Géza AU - Egei, Nóra AU - Farkas, Anikó AU - Hanyecz, Ottó AU - Ignácz, Bernadett AU - Kalup, Csilla AU - Könyves-Tóth, Réka AU - Kriskovics, Levente AU - Mészáros, László AU - Pál, András AU - Ordasi, András AU - Sárneczky, Krisztián AU - Seli, Bálint Attila AU - Sódor, Ádám AU - Szakáts, Róbert AU - Vinkó, József AU - Zsidi, Gabriella TI - Mid-infrared time-domain study of recent dust production events in the extreme debris disc of TYC 4209-1322-1 JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY J2 - MON NOT R ASTRON SOC VL - 516 PY - 2022 IS - 4 SP - 5684 EP - 5701 PG - 18 SN - 0035-8711 DO - 10.1093/mnras/stac2595 UR - https://m2.mtmt.hu/api/publication/33108812 ID - 33108812 N1 - Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network (ELKH), Konkoly-Thege Miklós út 15-17, Budapest, H-1121, Hungary CSFK, MTA Centre of Excellence, Konkoly Thege Miklós út 15-17, Budapest, H-1121, Hungary ELTE Eötvös Loránd University, Institute of Physics, Pázmány Péter sétány 1/A, Budapest, H-1117, Hungary Max-Planck-Institut für Astronomie, Königstuhl 17, Heidelberg, D-69117, Germany Department of Astronomy, Steward Observatory, The University of Arizona, Tucson, AZ 85721-0009, United States Department of Planetary Sciences, Lunar & Planetary Laboratory, The University of Arizona, 1629 E University Blvd, Tucson, AZ 85721-0092, United States National Astronomical Observatory of Japan, Osawa 2-21-1, , Tokyo, Mitaka, 181-8588, Japan Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo, 113-0033, Japan MTA, CSFK, Lendület Near-Field Cosmology Research Group, Hungary MTA-ELTE, Lendület 'Momentum' Milky Way Research Group, Hungary Faculty of Informatics, Eötvös Loránd University, Pázmány Péter sétány 1/A, Budapest, H-1117, Hungary Department of Astronomy, Eötvös Loránd University, Pázmány Péter sétány 1/A, Budapest, H-1117, Hungary Department of Optics and Quantum Electronics, University of Szeged, Dóm tér 9, Szeged, H-6720, Hungary Export Date: 16 June 2023 CODEN: MNRAA Correspondence Address: Moór, A.; Konkoly Observatory, Konkoly-Thege Miklós út 15-17, Hungary; email: moor@konkoly.hu AB - 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. LA - English DB - MTMT ER - TY - CONF AU - Seli, Bálint Attila AU - Van Driel Gesztelyi, Lídia AU - Baker, Deborah AU - Laming, J. Martin AU - Kővári, Zsolt AU - Oláh, Katalin Ilona AU - Kriskovics, Levente AU - Vida, Krisztián AU - Balázs, Lajos TI - Stellar FIP effect from the empirical side T2 - 44th COSPAR Scientific Assembly. Held 16-24 July PY - 2022 UR - https://m2.mtmt.hu/api/publication/33087071 ID - 33087071 AB - The difference between the elemental abundances of the corona and the photosphere is an apparently common feature of stellar atmospheres. The abundance difference depends on the first ionization potential of the given element, so the phenomenon is known as the FIP effect. Here we explore the variation of the strength of the FIP effect for different types of stars, through the FIP bias parameter. Using a sample of 59 main sequence and evolved stars with known coronal abundances from the literature, we look for macroscopic, measurable parameters that affect the stellar FIP bias, and also re-evaluate the simple dependence on the effective temperature. LA - English DB - MTMT ER - TY - JOUR AU - Szabó, Zs. M. AU - Kóspál, Ágnes AU - Ábrahám, Péter AU - Park, Sunkyung AU - Siwak, Michal AU - Green, J. D. AU - Pál, András AU - Acosta-Pulido, J. A. AU - Lee, J. -E. AU - Ibrahimov, M. AU - Grankin, K. AU - Kovács, B. AU - Bora, Zs. AU - Bódi, Attila AU - Cseh, Borbála AU - Csörnyei, Géza AU - Dróżdż, Marek AU - Hanyecz, O. AU - Ignácz, B. AU - Kalup, Csilla AU - Könyves-Tóth, Réka AU - Krezinger, Máté AU - Kriskovics, Levente AU - Ogłoza, Waldemar AU - Ordasi, A. AU - Sárneczky, Krisztián AU - Seli, Bálint Attila AU - Szakáts, Róbert AU - Sódor, Ádám AU - Szing, A. AU - Vida, Krisztián AU - Vinkó, József TI - A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence JF - ASTROPHYSICAL JOURNAL J2 - ASTROPHYS J VL - 936 PY - 2022 IS - 1 SN - 1538-4357 DO - 10.3847/1538-4357/ac82f5 UR - https://m2.mtmt.hu/api/publication/33087067 ID - 33087067 N1 - Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Eötvös Loránd Research Network (ELKH), Konkoly-Thege Miklós út 15-17, Budapest, 1121, Hungary CSFK, MTA Centre of Excellence, Konkoly Thege Miklós út 15-17., Budapest, H-1121, Hungary Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, Bonn, D-53121, Germany Scottish Universities Physics Alliance (SUPA), School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, United Kingdom Eötvös Loránd University, Department of Astronomy, Pázmány Péter sétány 1/A, Budapest, 1117, Hungary Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, D-69117, Germany ELTE Eötvös Loránd University, Institute of Physics, Pázmány Péter sétány 1/A, Budapest, H-1117, Hungary Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, United States MIT Kavli Institute for Astrophysics and Space Research, 70 Vassar Street, Cambridge, MA 02109, United States Instituto de Astrofísica de Canarias, Avenida Vía Láctea, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, Tenerife, Spain School of Space Research, Kyung Hee University, 1732, Deogyeong-daero, Giheung-gu, Yongin-si, Gyeonggi-do, 17104, South Korea Institute of Astronomy, Russian Academy of Sciences, 48 Pyatnitskaya st., Moscow, 119017, Russian Federation Crimean Astrophysical Observatory, p/o Nauchny298409 MTA CSFK Lendület Near-Field Cosmology Research Group, 1121 Konkoly Thege Miklós út, Budapest, 15-17, Hungary MTA-ELTE Lendület “Momentum” Milky Way Research Group, Hungary Mount Suhora Astronomical Observatory, Cracow Pedagogical University, ul. Podchorazych 2, Kraków, 30-084, Poland Department of Optics & Quantum Electronics, University of Szeged, Dóm tér 9, Szeged, 6720, Hungary Cited By :1 Export Date: 15 February 2023 Correspondence Address: Szabó, Zs.M.; Konkoly Observatory, Konkoly-Thege Miklós út 15-17, Hungary; email: szabo.zsofia@csfk.org AB - Historically, FU Orionis-type stars are low-mass, pre-main-sequence stars. The members of this class experience powerful accretion outbursts and remain in an enhanced accretion state for decades or centuries. V1515 Cyg, a classical FUor, started brightening in the 1940s and reached its peak brightness in the late 1970s. Following a sudden decrease in brightness, it stayed in a minimum state for a few months, then started brightening for several years. We present the results of our ground-based photometric monitoring complemented with optical/near-infrared spectroscopic monitoring. Our light curves show a long-term fading with strong variability on weekly and monthly timescales. The optical spectra show P Cygni profiles and broad blueshifted absorption lines, common properties of FUors. However, V1515 Cyg lacks the P Cygni profile in the Ca II 8498 Å line, a part of the Ca infrared triplet, formed by an outflowing wind, suggesting that the absorbing gas in the wind is optically thin. The newly obtained near-infrared spectrum shows the strengthening of the CO bandhead and the FeH molecular band, indicating that the disk has become cooler since the last spectroscopic observation in 2015. The current luminosity of the accretion disk dropped from the peak value of 138 L ⊙ to about 45 L ⊙, suggesting that the long-term fading is also partly caused by the dropping of the accretion rate. LA - English DB - MTMT ER - TY - JOUR AU - Günther, Maximilian N. AU - Berardo, David A. AU - Ducrot, Elsa AU - Murray, Catriona A. AU - Stassun, Keivan G. AU - Oláh, Katalin Ilona AU - Bouma, L. G. AU - Rappaport, Saul AU - Winn, Joshua N. AU - Feinstein, Adina D. AU - Matthews, Elisabeth C. AU - Sebastian, Daniel AU - Rackham, Benjamin V. AU - Seli, Bálint Attila AU - Triaud, Amaury H. M. J. AU - Gillen, Edward AU - Levine, Alan M. AU - Demory, Brice-Olivier AU - Gillon, Michaël AU - Queloz, Didier AU - Ricker, George R. AU - Vanderspek, Roland K. AU - Seager, Sara AU - Latham, David W. AU - Jenkins, Jon M. AU - Brasseur, C. E. AU - Colón, Knicole D. AU - Daylan, Tansu AU - Delrez, Laetitia AU - Fausnaugh, Michael AU - Garcia, Lionel J. AU - Jayaraman, Rahul AU - Jehin, Emmanuel AU - Kristiansen, Martti H. AU - Kruijssen, J. M. Diederik AU - Pedersen, Peter Pihlmann AU - Pozuelos, Francisco J. AU - Rodriguez, Joseph E. AU - Wohler, Bill AU - Zhan, Zhuchang TI - Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle JF - ASTRONOMICAL JOURNAL J2 - ASTRON J VL - 163 PY - 2022 IS - 4 SN - 0004-6256 DO - 10.3847/1538-3881/ac503c UR - https://m2.mtmt.hu/api/publication/32732997 ID - 32732997 N1 - Department of Physics, Kavli Institute for Astrophysics and Space Research, Mit, 77 Massachusetts Avenue, Cambridge, MA 02139, United States European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Keplerlaan 1, Noordwijk, 2201 AZ, Netherlands Astrobiology Research Unit, Université de Liège, 19C Allée du 6 Aout, Liège, B-4000, Belgium Cavendish Laboratory, JJ Thomson Avenue, Cambridge, CB3 0HE, United Kingdom Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, United States Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungary Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, United States Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, United States Department of Earth, Atmospheric and Planetary Sciences, Mit, 77 Massachusetts Avenue, Cambridge, MA 02139, United States School of Physics and Astronomy, University of Birmingham, Birmingham, Edgbaston, B15 2TT, United Kingdom Astronomy Unit, Queen Mary University of London, Mile End Road, London, E1 4NS, United Kingdom University of Bern, Center for Space and Habitability, Bern, Switzerland Observatoire Astronomique de l'Université de Genève, 51 chemin de Pégase, Sauverny, 1290, Switzerland Department of Aeronautics and Astronautics, Mit, 77 Massachusetts Avenue, Cambridge, MA 02139, United States Center for Astrophysics Harvard and Smithsonian, 60 Garden Street, Cambridge, MA 02138, United States Nasa Ames Research Center, Moffett FieldCA 94035, United States Mikulski Archive for Space Telescopes, United States Nasa Goddard Space Flight Center, Exoplanets and Stellar Astrophysics Laboratory (Code 667), Greenbelt, MD 20771, United States Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, 19C Allée du 6 Aout, Liège, B-4000, Belgium Brorfelde Observatory, Observator Gyldenkernes Vej 7DK-4340, Denmark Dtu Space, National Space Institute, Technical University of Denmark, Elektrovej 327, Lyngby, DK-2800, Denmark Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, Heidelberg, D-69120, Germany Seti Institute/NASA Ames Research Center, United States Cited By :1 Export Date: 29 June 2022 Correspondence Address: Günther, M.N.; Department of Physics, 77 Massachusetts Avenue, United States; email: maximilian.guenther@esa.int Funding details: T010920F Funding details: KR4801/2-1 Funding details: National Science Foundation, NSF, DGE-1746045 Funding details: National Aeronautics and Space Administration, NASA, NAS 5-26555 Funding details: Simons Foundation, SF Funding details: Automotive Research Center, ARC Funding details: Horizon 2020 Framework Programme, H2020, 714907, 803193/BEBOP Funding details: Seventh Framework Programme, FP7, FP/2007–2013 Funding details: Heising-Simons Foundation, HSF Funding details: Engineering Research Centers, ERC, 336480 Funding details: Science and Technology Facilities Council, STFC, ST/S00193X/1 Funding details: European Research Council, ERC Funding details: European Space Agency, ESA Funding details: Deutsche Forschungsgemeinschaft, DFG, KR4801/1-1 Funding details: Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, SNF, PP00P2-163967 Funding details: Nemzeti Kutatási Fejlesztési és Innovációs Hivatal, NKFIH, OTKA K131508 Funding details: Fondation Merac, MERAC Funding details: Innovációs és Technológiai Minisztérium Funding text 1: M.N.G. acknowledges support from MIT’s Kavli Institute as a Juan Carlos Torres Fellow and from the European Space Agency (ESA) as an ESA Research Fellow. K.O. and B.S. acknowledge support from the Hungarian National Research, Development and Innovation Office grant OTKA K131508. B.S. is supported by the ÚNKP-19-3 New National Excellence Program of the Ministry for Innovation and Technology. J.N.W. and B.V.R. thank the Heising-Simons Foundation for support. A.D.F. acknowledges the support from the National Science Foundation Graduate Research Fellowship Program under grant No. (DGE-1746045). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a Winton Exoplanet Fellowship. M.G. is F.R.S.-FNRS Senior Research Associate. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-163967). J.M.D.K. gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) through an Emmy Noether Research Group (grant number KR4801/1-1), the DFG Sachbeihilfe (grant number KR4801/2-1), and the SFB 881 “The Milky Way System” (subproject B2), as well as from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program via the ERC Starting Grant MUSTANG (grant agreement number 714907). Funding text 2: Funding for the TESS mission is provided by NASA’s Science Mission directorate. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007–2013) ERC Grant Agreement n° 336480, from the European Union’s Horizon 2020 research and innovation program (grant agreement n° 803193/BEBOP), from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation, from the Balzan Prize Foundation, from F.R.S-FNRS (Research Project ID T010920F), from the Simons Foundation, from the MERAC foundation, and from STFC, under grant number ST/S00193X/1. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. LA - English DB - MTMT ER - TY - JOUR AU - Seli, Bálint Attila AU - Oláh, Katalin Ilona AU - Kriskovics, Levente AU - Kővári, Zsolt AU - Vida, Krisztián AU - Balázs, Lajos AU - Laming, J. M. AU - Van Driel Gesztelyi, Lídia AU - Baker, D. TI - Extending the FIP bias sample to magnetically active stars JF - ASTRONOMY & ASTROPHYSICS J2 - ASTRON ASTROPHYS VL - 659 PY - 2022 SN - 0004-6361 DO - 10.1051/0004-6361/202141493 UR - https://m2.mtmt.hu/api/publication/32726535 ID - 32726535 N1 - Konkoly Observatory, Research Centre for Astronomy and Earth Sciences (ELKH), Budapest, Hungary Eotvos University, Department of Astronomy, Pf. 32, Budapest, 1518, Hungary Space Science Division, Code 7684, Naval Research Laboratory, Washington, DC 20375, United States University College London, Mullard Space Science Laboratory, Holmbury St. Mary, Surrey, RH5 6NT, United Kingdom LESIA, Observatoire de Paris, Universite PSL, CNRS, Sorbonne Universite, Univ. Paris Diderot, Sorbonne Paris Cite, 5 place Jules Janssen, Meudon, 92195, France Export Date: 29 June 2022 CODEN: AAEJA Correspondence Address: Seli, B.; Konkoly Observatory, Hungary; email: seli.balint@csfk.org Funding details: 101öu13, 104öu2, NKFIH PD-134784 Funding details: Office of Naval Research, ONR Funding details: National Aeronautics and Space Administration, NASA, 80HQTR19T0029, 80HQTR20T0076 Funding details: Science and Technology Facilities Council, STFC, ST/S000240/1 Funding details: Hungarian Scientific Research Fund, OTKA, 2019-2.1.11-TÉT-2019-00056, K-131508, K129249, KH-130526, NN129075 Funding details: Nemzeti Kutatási Fejlesztési és Innovációs Hivatal, NKFIH Funding text 1: cA knolw edgements. We thank the referee for the useful suggestion concerning the connection between the (I)FIP and the heating of the stellar coronae. Konkoly Observatory, Budapest, Hungary hosted two workshops on Elemental Composition in Solar and Stellar Atmospheres (IFIPWS-1, 13-15 Feb, 2017 and IFIPWS-2, 27 Feb-1 Mar, 2018). The workshops have fostered collaboration by exploiting synergies in solar and stellar magnetic activity studies and exchanging experience and knowledge in both research fields. We thank G. Csörnyei for the useful discussions and enlightening ideas regarding statistical methods. This work was supported by the Hungarian National Research, Development and Innovation Office grants NKFIH (OTKA) K-131508, KH-130526, NN129075, K129249 and by the NKFIH grant 2019-2.1.11-TÉT-2019-00056. Authors acknowledge the financial support of the Austrian-Hungarian Action Foundation (101öu13, 104öu2). L.K. acknowledges the financial support of the Hungarian National Research, Development and Innovation Office grant NKFIH PD-134784. L.K. is a Bolyai János Research Fellow. J.M.L. was supported by the NASA Heliophysics Guest Investigator (80HQTR19T0029) and Supporting Research (80HQTR20T0076) programs, and by Basic Research FUnds of the Office of Naval Research. D.B. is funded under STFC consolidated grant number ST/S000240/1 and LvDG is partially funded under the same grant. Software: python (Van Rossum & Drake 2009), matplotlib (Hunter 2007), numpy (van der Walt et al. 2011), scipy (Virtanen et al. 2020), pandas (McKinney 2010), sklearn (Pedregosa et al. 2011). AB - Context. The different elemental abundances of the photosphere and the corona are striking features of not only the Sun, but of other stars as well. This phenomenon is known as the first ionisation potential (FIP) effect, and its strength can be characterized by the FIP bias, the logarithmic abundance difference between low- and high-FIP elements in the corona, compared to the photosphere. The FIP bias was shown to depend on the surface temperature of the star. Aims: We aim to extend the Teff−FIP bias relationship to a larger stellar sample and analyse the effect of other astrophysical parameters on the relation (e.g. surface gravity, age, activity indicators). Methods: We compiled FIP bias and other parameters for 59 stars for which coronal composition is available, now including evolved stars. Using principal component analysis and linear discriminant analysis, we searched for correlations with other astrophysical parameters within the sample that may influence the stellar FIP bias. Results: Adding stars to the Teff−FIP bias diagram unveiled new features in its structure. In addition to the previously known relationship, there appears to be a second branch: a parallel sequence about 0.5 dex above it. While the Teff remains the main determinant of the FIP bias, other parameters such as stellar activity indicators also have influence. We find three clusters in the FIP bias determinant parameter space. One distinct group is formed by the evolved stars. Two groups contain main sequence stars in continuation separated roughly by the sign change of the FIP-bias value. Conclusions: The new branch of the Teff−FIP bias diagram contains stars with higher activity level, in terms of X-ray flux and rotational velocity. The Rossby number also seems to be important, indicating possible dependence on the type of dynamo operating in these stars influencing their FIP bias. The two main-sequence clusters run from the earliest spectral types of A-F with shallow convection zones through G-K-early-M stars with gradually deeper convection zones, and they end with the fully convective M dwarf stars, depicting the change of the dynamo type with the internal differences of the main sequence stars in connection with the FIP-bias values. LA - English DB - MTMT ER - TY - JOUR AU - Borkovits, Tamás AU - Mitnyan, Tibor AU - Rappaport, S A AU - Pribulla, T AU - Powell, B P AU - Kostov, V B AU - Bíró, Imre Barna AU - Csányi, István AU - Garai, Zoltán AU - Gary, B L AU - Kaye, T G AU - Komžík, R AU - Terentev, I AU - Omohundro, M AU - Gagliano, R AU - Jacobs, T AU - Kristiansen, M H AU - LaCourse, D AU - Schwengeler, H M AU - Czavalinga, Donát Róbert AU - Seli, Bálint Attila AU - Huang, C X AU - Pál, András AU - Vanderburg, A AU - Rodriguez, J E AU - Stevens, D J TI - Triply eclipsing triple stars in the northern TESS fields: TICs 193993801, 388459317, and 52041148 JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY J2 - MON NOT R ASTRON SOC VL - 510 PY - 2022 IS - 1 SP - 1352 EP - 1374 PG - 23 SN - 0035-8711 DO - 10.1093/mnras/stab3397 UR - https://m2.mtmt.hu/api/publication/32559296 ID - 32559296 N1 - Baja Astronomical Observatory of University of Szeged, Szegediút, Kt. 766, Baja, H-6500, Hungary Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklósút 15-17, Budapest, H-1121, Hungary ELTE Gothard Astrophysical Observatory, Szent Imre h. u. 112, Szombathely, H-9700, Hungary Department of Physics, Kavli Institute for Astrophysics and Space Research, M.I.T., Cambridge, MA 02139, United States Astronomical Institute of the Slovak Academy of Sciences, Tatranská Lomnica, Slovakia NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, United States SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, United States MTA-ELTEExoplanet Research Group, Szent Imre h. u. 112, Szombathely, H-9700, Hungary MTA-ELTE Lendület Milky Way Research Group, Szent Imre h. u. 112, Szombathely, H-9700, Hungary Amateur Astronomer, Her Efor D Arizona Observatory, Hereford, AZ 85615, United States Amateur Astronomer, Foundation for Scientific Advancement, Patterson ObservatoryAZ 85650, United States Citizen Scientist, Department of Physics, Univer Sity of Oxford, Denys Wilkinson Building, c/o Zooniver se, Keble Road, Oxford, OX1 3RH, United Kingdom Amateur Astronomer, Glendale, AZ 85308, United States Amateur Astronomer, 12812 SE 69th Place, Bellevue, WA 98006, United States Brorfelde Observatory, Observator Gyldenkernes Vej 7 TølløseDK-4340, Denmark DTU Space, National Space Institute, Technical Univer Sity of Denmark, Elektrovej 327, Lyngby, DK-2800, Denmark Amateur Astronomer, 7507 52nd Place NE, Marysville, WA 98270, United States Eötvös University, Department of Astronomy, Pf. 32, Budapest, 1518, Hungary Department of Astronomy, The University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53706, United States Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, United States Department of Astronomy & Astrophysics, The Pennsylvania State Univer- Sity, 525 Davey Lab, University Park, PA 16802, United States Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, United States Cited By :7 Export Date: 14 December 2022 CODEN: MNRAA Correspondence Address: Borkovits, T.; Baja Astronomical Observatory of University of Szeged, Szegediút, Kt. 766, Hungary; email: borko@electra.bajaobs.hu AB - In this work we report the discovery and analysis of three new triply eclipsing triple star systems found with the TESS mission during its observations of the northern skies: TICs 193993801, 388459317, and 52041148. We utilized the TESS precision photometry of the binary eclipses and third-body eclipsing events, ground-based archival and follow-up photometric data, eclipse timing variations, archival spectral energy distributions, as well as theoretical evolution tracks in a joint photodynamical analysis to deduce the system masses and orbital parameters of both the inner and outer orbits. In one case (TIC 193993801) we also obtained radial velocity measurements of all three stars. This enabled us to 'calibrate' our analysis approach with and without 'truth' (i.e. RV) data. We find that the masses are good to 1-3 per cent accuracy with RV data and 3-10 per cent without the use of RV data. In all three systems we were able to find the outer orbital period before doing any detailed analysis by searching for a longer-term periodicity in the ASAS-SN archival photometry data - just a few thousand ASAS-SN points enabled us to find the outer periods of 49.28 d, 89.86 d, and 177.0 d, respectively. From our full photodynamical analysis we find that all three systems are coplanar to within 1 degrees-3 degrees. The outer eccentricities of the three systems are 0.003, 0.10, and 0.62, respectively (i.e. spanning a factor of 200). The masses of the three stars {Aa, Ab, and B} in the three systems are: {1.31, 1.19, 1.34}, {1.82, 1.73, 2.19}, and {1.62, 1.48, 2.74} M-circle dot, respectively. LA - English DB - MTMT ER -