@article{MTMT:34817487, title = {European VLBI Network observations of the peculiar radio source 4C 35.06 overlapping with a compact group of nine galaxies}, url = {https://m2.mtmt.hu/api/publication/34817487}, author = {Veres, P. M. and Gabányi, Krisztina Éva and Frey, Sándor and Paragi, Z. and An, T. and Bagchi, J. and Bogdán, Á. and Biju, K. G. and Kun, Emma and Jacob, J. and Adebahr, B.}, doi = {10.1051/0004-6361/202348729}, journal-iso = {ASTRON ASTROPHYS}, journal = {ASTRONOMY & ASTROPHYSICS}, volume = {684}, unique-id = {34817487}, issn = {0004-6361}, abstract = {Context. According to the hierarchical structure formation model, brightest cluster galaxies (BCGs) evolve into the most luminous and massive galaxies in the Universe through multiple merger events. The peculiar radio source 4C 35.06 is located at the core of the galaxy cluster Abell 407, overlapping with a compact group of nine galaxies. Low-frequency radio observations have revealed a helical, steep-spectrum, kiloparsec-scale jet structure and inner lobes with less steep spectra, compatible with a recurring active galactic nucleus (AGN) activity scenario. However, the host galaxy of the AGN responsible for the detected radio emission remained unclear.}, year = {2024}, eissn = {1432-0746}, orcid-numbers = {Veres, P. M./0000-0002-9553-2987; Gabányi, Krisztina Éva/0000-0003-1020-1597; Frey, Sándor/0000-0003-3079-1889; Paragi, Z./0000-0002-5195-335X; An, T./0000-0003-4341-0029; Kun, Emma/0000-0003-2769-3591; Jacob, J./0000-0002-0413-1855; Adebahr, B./0000-0002-5447-6878} } @article{MTMT:34762210, title = {Raman–Infrared Spectral Correlation of an Artificially Space-Weathered Carbonaceous Chondrite Meteorite}, url = {https://m2.mtmt.hu/api/publication/34762210}, author = {Gyollai, Ildikó and Biri, Sándor and Juhász, Zoltán and Király, Csilla and Rácz, Richárd Péter and Rezes, Dániel and Sulik, Béla and Szabó, Máté Zoltán and Szalai, Zoltán and Szávai, P and Szklenár, Tamás and Kereszturi, Ákos}, doi = {10.3390/min14030288}, journal-iso = {MINERALS-BASEL}, journal = {MINERALS}, volume = {14}, unique-id = {34762210}, abstract = {Raman and infrared measurements of the same locations were conducted on a northwest African (NWA) 10580 CO3 meteorite sample, before and after three proton irradiations (1 keV ion energy using 1011, 1014, and 1017 ion/cm2 fluent values), to simulate space weathering effects. In the case of Raman spectroscopy, both FWHM and peak positions of the major olivine and pyroxene bands changed after the irradiation, and the minor bands disappeared. In the FTIR spectra, the minor bands of olivine and pyroxene also disappeared; meanwhile, major IR bands of pyroxene remained visible, demonstrating both positive and negative peak shifts, and the olivines were characterised only by negative peak shifts. The olivines were characterised by negative FWHM changes for major bands, but positive FWHM changes for minor bands. The pyroxenes were characterised by elevated FWHM changes for minor bands after the irradiation. The disappearance of minor bands both of IR and Raman spectra indicates the amorphization of minerals. The negative peak shift in IR spectra indicates Mg loss for olivine and pyroxene, in agreement with the literature. The Raman spectra are characterised by positive peak shift and positive FWHM changes; the IR spectra are characterised by a negative peak shift. The Mg loss, which was detected by negative peak shifts of FTIR bands, may be caused by distortion of the crystal structure, which could be detected by a positive peak shift in Raman spectra. This joint observation and interpretation has not been formulated in the literature, but indicates further possibilities in the confirmation of mineral changes by different instruments. Shock alteration-based observations by other researchers could be used as a reference for irradiation experiments as irradiation makes a similar structural alteration, like a low-grade shock metamorphism.}, year = {2024}, eissn = {2075-163X}, orcid-numbers = {Gyollai, Ildikó/0000-0001-8576-0196; Rezes, Dániel/0000-0003-0730-2418; Szalai, Zoltán/0000-0001-5267-411X} } @article{MTMT:34749880, title = {High-resolution cross section measurements for neutron interactions on 89Y with incident neutron energies up to 95 keV}, url = {https://m2.mtmt.hu/api/publication/34749880}, author = {Tagliente, G. and Milazzo, P. M. and Paradela, C. and Kopecky, S. and Vescovi, D. and Alaerts, G. and Damone, L. A. and Heyse, J. and Krtička, M. and Schillebeeckx, P. and Mengoni, A. and Wynants, R. and Valenta, S. and Aberle, O. and Alcayne, V. and Amaducci, S. and Andrzejewski, J. and Audouin, L. and Babiano-Suarez, V. and Bacak, M. and Barbagallo, M. and Bécares, V. and Bečvář, F. and Bellia, G. and Berthoumieux, E. and Billowes, J. and Bosnar, D. and Brown, A. S. and Busso, M. and Caamaño, M. and Caballero, L. and Calviani, M. and Calviño, F. and Cano-Ott, D. and Casanovas, A. and Cerutti, F. and Chen, Y. H. and Chiaveri, E. and Colonna, N. and Cortés, G. P. and Cortés-Giraldo, M. A. and Cosentino, L. and Cristallo, S. and Diakaki, M. and Dietz, M. and Domingo-Pardo, C. and Dressler, R. and Dupont, E. and Durán, I. and Eleme, Z. and Fernández-Domíngez, B. and Ferrari, A. and Ferro-Gonçalves, I. and Finocchiaro, P. and Furman, V. and Garg, R. and Gawlik, A. and Gilardoni, S. and Glodariu, T. and Göbel, K. and González-Romero, E. and Guerrero, C. and Gunsing, F. and Heinitz, S. and Jenkins, D. G. and Jericha, E. and Kadi, Y. and Käppeler, F. and Kimura, A. and Kivel, N. and Kokkoris, M. and Kopatch, Y. and Kurtulgil, D. and Ladarescu, I. and Larsen, A. C. and Lederer-Woods, C. and Lerendegui-Marco, J. and Lo, Meo S. and Lonsdale, S. J. and Lugaro, Maria and Macina, D. and Manna, A. and Martínez, T. and Masi, A. and Massimi, C. and Mastinu, P. F. and Mastromarco, M. and Matteucci, F. and Maugeri, E. and Mazzone, A. and Mendoza, E. and Michalopoulou, V. and Mingrone, F. and Musumarra, A. and Negret, A. and Nolte, R. and Ogállar, F. and Oprea, A. and Patronis, N. and Pavlik, A. and Perkowski, J. and Piersanti, L. and Porras, I. and Praena, J. and Quesada, J. M. and Radeck, D. and Ramos, Doval D. and Reifarth, R. and Rochman, D. and Rubbia, C. and Sabaté-Gilarte, M. and Saxena, A. and Schumann, D. and Smith, A. G. and Spelta, M. and Sosnin, N. and Stamatopoulos, A. and Tain, J. L. and Talip, Z. and Tarifeño-Saldivia, A. E. and Tassan-Got, L. and Torres-Sánchez, P. and Tsinganis, A. and Ulrich, J. and Urlass, S. and Vannini, G. and Variale, V. and Vaz, P. and Ventura, A. and Vlachoudis, V. and Vlastou, R. and Wallner, A. and Woods, P. J. and Wright, T. J. and Žugec, P.}, doi = {10.1140/epja/s10050-024-01243-4}, journal-iso = {EUR PHYS J A}, journal = {EUROPEAN PHYSICAL JOURNAL A: HADRONS AND NUCLEI}, volume = {60}, unique-id = {34749880}, issn = {1434-6001}, abstract = {The cross section of the 89Y(n, γ ) reaction has important implications in nuclear astrophysics and for advanced nuclear technology. Given its neutron magic number N = 50 and a consequent small neutron capture cross section, 89Y represents one of the key nuclides for the stellar s-process. It acts as a bottleneck in the neutron capture chain between the Fe seed and the heavier elements. Moreover, it is located at the overlapping region, where both the weak and main s-process components take place. 89Y, the only stable yttrium isotope, is also used in innovative nuclear reactors. Neutron capture and transmission measurements were performed at the time-of-flight facilities n_TOF at CERN and GELINA at JRC-Geel. Resonance parameters of individual resonances were extracted from a resonance analysis of the experimental transmission and capture yields, up to a neutron incident energy of 95 keV. Even though a comparison with results reported in the literature shows differences in resonance parameters, the present data are consistent with the Maxwellian averaged cross section suggested by the astrophysical database KADONIS.}, year = {2024}, eissn = {1434-601X} } @article{MTMT:34749879, title = {A study of the stellar photosphere-hydrogen ionization front interaction in δ Scuti stars}, url = {https://m2.mtmt.hu/api/publication/34749879}, author = {Deka, Mami and Kanbur, Shashi M. and Deb, Sukanta and Das, Susmita}, doi = {10.1017/S1743921323002697}, journal-iso = {PROC IAU}, journal = {PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION}, volume = {18}, unique-id = {34749879}, issn = {1743-9213}, abstract = {Pulsating variable δ Scuti stars are intermediate-mass stars with masses in the range of 1-3 δ and spectral types between A2 and F2. They can be found at the intersection of the Cepheid instability strip with the main sequence. They can be used as astrophysical laboratories to test theories of stellar evolution and pulsation. In this contribution, we investigate the observed period-colour and amplitude-colour (PCAC) relations at maximum/mean/minimum light of Galactic bulge and Large Magellanic Cloud δ Scuti stars for the first time and test the hydrogen ionization front (HIF)-photosphere interaction theory using the mesa-rsp code. The PCAC relations, as a function of pulsation phase, are crucial probes of the structure of the outer stellar envelope and provide insight into the physics of stellar pulsation and evolution. The observed behaviour of the δ Scuti PCAC relations is consistent with the theory of the interaction between the HIF and the stellar photosphere.}, keywords = {variables; STARS; Astrophysics - Solar and Stellar Astrophysics; MAGELLANIC CLOUDS; delta Scuti; GALACTIC BULGE}, year = {2024}, eissn = {1743-9221}, pages = {98-104} } @article{MTMT:34749877, title = {A multi-wavelength analysis of BL Her stars: Models versus Observations}, url = {https://m2.mtmt.hu/api/publication/34749877}, author = {Das, Susmita and Molnár, László and Kanbur, S. M. and Joyce, Meridith and Bhardwaj, A. and Singh, H. P. and Marconi, M. and Ripepi, V. and Smolec, R.}, doi = {10.1017/S1743921323002612}, journal-iso = {PROC IAU}, journal = {PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION}, volume = {18}, unique-id = {34749877}, issn = {1743-9213}, abstract = {We present new theoretical period-luminosity (PL) and period-radius (PR) relations at multiple wavelengths (Johnson-Cousins-Glass and Gaia passbands) for a fine grid of BL Herculis models computed using mesa-rsp. The non-linear models were computed for periods typical of BL Her stars, i.e. 1 ≤ P(days) ≤ 4, covering a wide range of input parameters: metallicity (−2.0 dex ≤ [Fe/H] ≤ 0.0 dex), stellar mass (0.5-0.8 ), luminosity (50-300 ) and effective temperature (full extent of the instability strip; in steps of 50K). We investigate the impact of four sets of convection parameters on multi-wavelength properties. Most empirical relations match well with theoretical relations from the BL Her models computed using the four sets of convection parameters. No significant metallicity effects are seen in the PR relations. Another important result from our grid of BL Her models is that it supports combining PL relations of RR Lyrae and Type II Cepheids together as an alternative to classical Cepheids for the extragalactic distance scale calibration.}, keywords = {Astrophysics - Solar and Stellar Astrophysics; Stars: population II; stars: low-mass; stars: variables: Cepheids; stars: oscillations (including pulsations)}, year = {2024}, eissn = {1743-9221}, pages = {105-114} } @article{MTMT:34749876, title = {A multiphase study of classical Cepheids in the Magellanic Clouds- Models and Observations}, url = {https://m2.mtmt.hu/api/publication/34749876}, author = {Kurbah, Kerdaris and Kanbur, Shashi M. and Deb, Sukanta and Das, Susmita and Deka, Mami and Bhardwaj, Anupam and Randal, Hugh Riley and Kalici, Selim}, doi = {10.1017/S1743921323003563}, journal-iso = {PROC IAU}, journal = {PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION}, volume = {18}, unique-id = {34749876}, issn = {1743-9213}, abstract = {This work presents the study of multiphase relations of classical Cepheids in the Magellanic Clouds for short periods (log P < 1) and long periods (log P > 1). From the analysis, it has been found that the multiphase relations obtained using the models as well as observations are highly dynamic with pulsational phase. The multiphase relations for short and long periods are found to display contrasting behaviour for both LMC and SMC. It has been observed that the multiphase relations obtained using the models agree better with the observations in the PC plane in most phases in comparison to the PL plane. Multiphase relations obtained using the models display a clear distinction among different convection sets in most phases. Comparison of models and observations in the multiphase plane is one way to test the models with the observations and to constrain the theory of stellar pulsation.}, keywords = {STARS; statistical; Astrophysics - Astrophysics of Galaxies; Variable; Data analysis-methods; Cepheids-galaxies; Magellanic Clouds-methods}, year = {2024}, eissn = {1743-9221}, pages = {267-274} } @article{MTMT:34749874, title = {H2O masers and host environments of FU Orionis and EX Lupi type low-mass eruptive YSOs}, url = {https://m2.mtmt.hu/api/publication/34749874}, author = {Szabó, Zsófia Marianna and Gong, Yan and Yang, Wenjin and Menten, Karl M. and Bayandina, Olga S. and Cyganowski, Claudia J. and Kóspál, Ágnes and Ábrahám, Péter and Belloche, Arnaud and Wyrowski, Friedrich}, doi = {10.1017/S1743921323003174}, journal-iso = {PROC IAU}, journal = {PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION}, volume = {18}, unique-id = {34749874}, issn = {1743-9213}, abstract = {The FU Orionis (FUor) and EX Lupi (EXor) type objects are rare pre-main sequence low-mass stars undergoing accretion outbursts. Maser emission is widespread and is a powerful probe of mass accretion and ejection on small scales in star forming region. However, very little is known about the overall prevalence of water masers towards FUors/Exors. We present results from our survey using the Effelsberg 100-m telescope to observe the largest sample of FUors and EXors, plus additional Gaia alerted sources (with the potential nature of being eruptive stars), a total of 51 targets, observing the 22.2 GHz H2O maser, while simultaneously covering the NH3 23 GHz.}, keywords = {stars: pre-main sequence; stars: low-mass; MASERS}, year = {2024}, eissn = {1743-9221}, pages = {246-248} } @article{MTMT:34749871, title = {Surveying Turbulence in Protoplanetary Disks with ALMA}, url = {https://m2.mtmt.hu/api/publication/34749871}, author = {Flaherty, Kevin and Hughes, A. Meredith and Simon, Jacob and Diop, Amina and Tosolini, Anna and Dhahbi, Achref and Olsson, Berit and Qi, Chunhua and Bai, Xue-Ning and Andrews, Sean and Wilner, David and Kóspál, Ágnes}, journal-iso = {BULL AM ASTRON SOC}, journal = {BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY}, volume = {56}, unique-id = {34749871}, issn = {0002-7537}, abstract = {Turbulence within protoplanetary disks plays a crucial role in the formation and evolution of planets, through its influence on processes ranging from the collisional velocity of small dust grains to the ability of gas-giant planets to open gaps in the disk. Because of this importance, more observational constraints are needed. Molecular line observations provide the most direct method for measuring gas motion, and ALMA has provided the sensitivity and resolution needed to constrain turbulence. I will discuss our recent detections of turbulence around DM Tau and IM Lup, recent efforts to expand this sample, as well as the prospects for measuring radial and vertical variations in the turbulence using CO/13CO/C18O/N2H+/DCO+ emission.}, year = {2024} } @article{MTMT:34749870, title = {Chemical changes produced by accretion outbursts in planet-forming regions, observed with the James Webb Space Telescope}, url = {https://m2.mtmt.hu/api/publication/34749870}, author = {Smith, Sarah and Banzatti, Andrea and Ábrahám, Péter}, journal-iso = {BULL AM ASTRON SOC}, journal = {BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY}, volume = {56}, unique-id = {34749870}, issn = {0002-7537}, abstract = {The James Webb Space Telescope (JWST) is currently giving access to the chemistry of planet-forming regions in protoplanetary disks around pre-main-sequence stars in an unprecedented way, thanks to its high sensitivity and resolution. Young stars with circumstellar disks have variable accretion outbursts that give flares of high energy radiation to the planet-forming regions in inner disks within < 10 au. In this work, we use molecular spectra from MIRI (the mid-infrared instrument on JWST) to study the effects of episodic accretion flares on the chemistry of H2O, C2H2, HCN, CO2, OH, CO. We compare two epochs of MIRI spectra taken in August 2022 and April 2023 after a recent accretion outburst that happened in March 2022. We also compare the new MIRI data to previous Spitzer spectra that measured large chemical changes during a previous, strong outburst that happened in 2008. Our goal is to understand the long-term effects of accretion flares on the chemistry of planet formation in inner disks.}, year = {2024} } @article{MTMT:34749869, title = {Spectacular nucleosynthesis from early massive stars}, url = {https://m2.mtmt.hu/api/publication/34749869}, author = {Ji, Alexander and Curtis, Sanjana and Storm, Nicholas and Chandra, Vedant and Schlaufman, Kevin and Stassun, Keivan and Heger, Alexander and Pignatari, Marco and Price-Whelan, Adrian and Bergemann, Maria and Stringfellow, Guy and Frohlich, Carla and Reggiani, Henrique and Holmbeck, Erika and Tayar, Jamie and Shah, Shivani and Griffith, Emily and Laporte, Chervin and Casey, Andrew and Hawkins, Keith and Horta, Darrington Daniel and Cerny, William and Thibodeaux, Pierre and Usman, Sam and Amarante, Joao and Beaton, Rachael and Cargile, Phillip and Chiappini, Cristina and Conroy, Charlie and Johnson, Jennifer and Kollmeier, Juna and Li, Haining and Loebman, Sarah and Meynet, Georges and Rix, Hans-Walter}, journal-iso = {BULL AM ASTRON SOC}, journal = {BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY}, volume = {56}, unique-id = {34749869}, issn = {0002-7537}, abstract = {Stars formed with initial mass over 50 solar masses are very rare today, but they are thought to be more common in the early universe. The fates of those early, metal-poor, massive stars are highly uncertain. Most are expected to directly collapse to black holes, while some may explode as a result of rotationally powered engines or the pair-creation instability. We present the discovery and chemical abundances of J0931+0038, a nearby low-mass star that preserves the signature of unusual nucleosynthesis from a massive star in the early universe. J0931+0038 has relatively high metallicity ([Fe/H] = −1.76 ± 0.13) but an extreme odd-even abundance pattern, with some of the lowest known abundance ratios of [N/Fe], [Na/Fe], [K/Fe], [Sc/Fe], and [Ba/Fe] known. The implication is that a majority of its metals originated in a single extremely metal-poor nucleosynthetic source. An extensive search through models of nucleosynthesis in single, spherically symmetric, and metal-poor massive stars yielded no existing models able to explain the full abundance pattern, though there is a clear preference for progenitors with initial mass over 50 solar masses. J0931+0038 thus reaffirms the possible importance of jets, three-dimensional treatments of convection, and/or binary companions in models of supernova nucleosynthesis, especially at high initial masses. Though rare, more examples of unusual early nucleosynthesis in metal-poor stars should be found in upcoming large spectroscopic surveys.}, year = {2024}, orcid-numbers = {Pignatari, Marco/0000-0002-9048-6010} }