TY  - JOUR
AU  - Tagliente, G.
AU  - Milazzo, P. M.
AU  - Paradela, C.
AU  - Kopecky, S.
AU  - Vescovi, D.
AU  - Alaerts, G.
AU  - Damone, L. A.
AU  - Heyse, J.
AU  - Krtička, M.
AU  - Schillebeeckx, P.
AU  - Mengoni, A.
AU  - Wynants, R.
AU  - Valenta, S.
AU  - Aberle, O.
AU  - Alcayne, V.
AU  - Amaducci, S.
AU  - Andrzejewski, J.
AU  - Audouin, L.
AU  - Babiano-Suarez, V.
AU  - Bacak, M.
AU  - Barbagallo, M.
AU  - Bécares, V.
AU  - Bečvář, F.
AU  - Bellia, G.
AU  - Berthoumieux, E.
AU  - Billowes, J.
AU  - Bosnar, D.
AU  - Brown, A. S.
AU  - Busso, M.
AU  - Caamaño, M.
AU  - Caballero, L.
AU  - Calviani, M.
AU  - Calviño, F.
AU  - Cano-Ott, D.
AU  - Casanovas, A.
AU  - Cerutti, F.
AU  - Chen, Y. H.
AU  - Chiaveri, E.
AU  - Colonna, N.
AU  - Cortés, G. P.
AU  - Cortés-Giraldo, M. A.
AU  - Cosentino, L.
AU  - Cristallo, S.
AU  - Diakaki, M.
AU  - Dietz, M.
AU  - Domingo-Pardo, C.
AU  - Dressler, R.
AU  - Dupont, E.
AU  - Durán, I.
AU  - Eleme, Z.
AU  - Fernández-Domíngez, B.
AU  - Ferrari, A.
AU  - Ferro-Gonçalves, I.
AU  - Finocchiaro, P.
AU  - Furman, V.
AU  - Garg, R.
AU  - Gawlik, A.
AU  - Gilardoni, S.
AU  - Glodariu, T.
AU  - Göbel, K.
AU  - González-Romero, E.
AU  - Guerrero, C.
AU  - Gunsing, F.
AU  - Heinitz, S.
AU  - Jenkins, D. G.
AU  - Jericha, E.
AU  - Kadi, Y.
AU  - Käppeler, F.
AU  - Kimura, A.
AU  - Kivel, N.
AU  - Kokkoris, M.
AU  - Kopatch, Y.
AU  - Kurtulgil, D.
AU  - Ladarescu, I.
AU  - Larsen, A. C.
AU  - Lederer-Woods, C.
AU  - Lerendegui-Marco, J.
AU  - Lo, Meo S.
AU  - Lonsdale, S. J.
AU  - Lugaro, Maria
AU  - Macina, D.
AU  - Manna, A.
AU  - Martínez, T.
AU  - Masi, A.
AU  - Massimi, C.
AU  - Mastinu, P. F.
AU  - Mastromarco, M.
AU  - Matteucci, F.
AU  - Maugeri, E.
AU  - Mazzone, A.
AU  - Mendoza, E.
AU  - Michalopoulou, V.
AU  - Mingrone, F.
AU  - Musumarra, A.
AU  - Negret, A.
AU  - Nolte, R.
AU  - Ogállar, F.
AU  - Oprea, A.
AU  - Patronis, N.
AU  - Pavlik, A.
AU  - Perkowski, J.
AU  - Piersanti, L.
AU  - Porras, I.
AU  - Praena, J.
AU  - Quesada, J. M.
AU  - Radeck, D.
AU  - Ramos, Doval D.
AU  - Reifarth, R.
AU  - Rochman, D.
AU  - Rubbia, C.
AU  - Sabaté-Gilarte, M.
AU  - Saxena, A.
AU  - Schumann, D.
AU  - Smith, A. G.
AU  - Spelta, M.
AU  - Sosnin, N.
AU  - Stamatopoulos, A.
AU  - Tain, J. L.
AU  - Talip, Z.
AU  - Tarifeño-Saldivia, A. E.
AU  - Tassan-Got, L.
AU  - Torres-Sánchez, P.
AU  - Tsinganis, A.
AU  - Ulrich, J.
AU  - Urlass, S.
AU  - Vannini, G.
AU  - Variale, V.
AU  - Vaz, P.
AU  - Ventura, A.
AU  - Vlachoudis, V.
AU  - Vlastou, R.
AU  - Wallner, A.
AU  - Woods, P. J.
AU  - Wright, T. J.
AU  - Žugec, P.
TI  - High-resolution cross section measurements for neutron interactions on 89Y with incident neutron energies up to 95 keV
JF  - EUROPEAN PHYSICAL JOURNAL A: HADRONS AND NUCLEI
J2  - EUR PHYS J A
VL  - 60
PY  - 2024
IS  - 1
SN  - 1434-6001
DO  - 10.1140/epja/s10050-024-01243-4
UR  - https://m2.mtmt.hu/api/publication/34749880
ID  - 34749880
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Deka, Mami
AU  - Kanbur, Shashi M.
AU  - Deb, Sukanta
AU  - Das, Susmita
TI  - A study of the stellar photosphere-hydrogen ionization front interaction in δ Scuti stars
JF  - PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION
J2  - PROC IAU
VL  - 18
PY  - 2024
IS  - S376
SP  - 98
EP  - 104
PG  - 7
SN  - 1743-9213
DO  - 10.1017/S1743921323002697
UR  - https://m2.mtmt.hu/api/publication/34749879
ID  - 34749879
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Das, Susmita
AU  - Molnár, László
AU  - Kanbur, S. M.
AU  - Joyce, Meridith
AU  - Bhardwaj, A.
AU  - Singh, H. P.
AU  - Marconi, M.
AU  - Ripepi, V.
AU  - Smolec, R.
TI  - A multi-wavelength analysis of BL Her stars: Models versus Observations
JF  - PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION
J2  - PROC IAU
VL  - 18
PY  - 2024
IS  - S376
SP  - 105
EP  - 114
PG  - 10
SN  - 1743-9213
DO  - 10.1017/S1743921323002612
UR  - https://m2.mtmt.hu/api/publication/34749877
ID  - 34749877
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Kurbah, Kerdaris
AU  - Kanbur, Shashi M.
AU  - Deb, Sukanta
AU  - Das, Susmita
AU  - Deka, Mami
AU  - Bhardwaj, Anupam
AU  - Randal, Hugh Riley
AU  - Kalici, Selim
TI  - A multiphase study of classical Cepheids in the Magellanic Clouds- Models and Observations
JF  - PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION
J2  - PROC IAU
VL  - 18
PY  - 2024
IS  - S376
SP  - 267
EP  - 274
PG  - 8
SN  - 1743-9213
DO  - 10.1017/S1743921323003563
UR  - https://m2.mtmt.hu/api/publication/34749876
ID  - 34749876
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Szabó, Zsófia Marianna
AU  - Gong, Yan
AU  - Yang, Wenjin
AU  - Menten, Karl M.
AU  - Bayandina, Olga S.
AU  - Cyganowski, Claudia J.
AU  - Kóspál, Ágnes
AU  - Ábrahám, Péter
AU  - Belloche, Arnaud
AU  - Wyrowski, Friedrich
TI  - H2O masers and host environments of FU Orionis and EX Lupi type low-mass eruptive YSOs
JF  - PROCEEDINGS OF THE INTERNATIONAL ASTRONOMICAL UNION
J2  - PROC IAU
VL  - 18
PY  - 2024
IS  - S380
SP  - 246
EP  - 248
PG  - 3
SN  - 1743-9213
DO  - 10.1017/S1743921323003174
UR  - https://m2.mtmt.hu/api/publication/34749874
ID  - 34749874
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Flaherty, Kevin
AU  - Hughes, A. Meredith
AU  - Simon, Jacob
AU  - Diop, Amina
AU  - Tosolini, Anna
AU  - Dhahbi, Achref
AU  - Olsson, Berit
AU  - Qi, Chunhua
AU  - Bai, Xue-Ning
AU  - Andrews, Sean
AU  - Wilner, David
AU  - Kóspál, Ágnes
TI  - Surveying Turbulence in Protoplanetary Disks with ALMA
JF  - BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY
J2  - BULL AM ASTRON SOC
VL  - 56
PY  - 2024
IS  - 2
SN  - 0002-7537
UR  - https://m2.mtmt.hu/api/publication/34749871
ID  - 34749871
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Smith, Sarah
AU  - Banzatti, Andrea
AU  - Ábrahám, Péter
TI  - Chemical changes produced by accretion outbursts in planet-forming regions, observed with the James Webb Space Telescope
JF  - BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY
J2  - BULL AM ASTRON SOC
VL  - 56
PY  - 2024
IS  - 2
SN  - 0002-7537
UR  - https://m2.mtmt.hu/api/publication/34749870
ID  - 34749870
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Ji, Alexander
AU  - Curtis, Sanjana
AU  - Storm, Nicholas
AU  - Chandra, Vedant
AU  - Schlaufman, Kevin
AU  - Stassun, Keivan
AU  - Heger, Alexander
AU  - Pignatari, Marco
AU  - Price-Whelan, Adrian
AU  - Bergemann, Maria
AU  - Stringfellow, Guy
AU  - Frohlich, Carla
AU  - Reggiani, Henrique
AU  - Holmbeck, Erika
AU  - Tayar, Jamie
AU  - Shah, Shivani
AU  - Griffith, Emily
AU  - Laporte, Chervin
AU  - Casey, Andrew
AU  - Hawkins, Keith
AU  - Horta, Darrington Daniel
AU  - Cerny, William
AU  - Thibodeaux, Pierre
AU  - Usman, Sam
AU  - Amarante, Joao
AU  - Beaton, Rachael
AU  - Cargile, Phillip
AU  - Chiappini, Cristina
AU  - Conroy, Charlie
AU  - Johnson, Jennifer
AU  - Kollmeier, Juna
AU  - Li, Haining
AU  - Loebman, Sarah
AU  - Meynet, Georges
AU  - Rix, Hans-Walter
TI  - Spectacular nucleosynthesis from early massive stars
JF  - BULLETIN OF THE AMERICAN ASTRONOMICAL SOCIETY
J2  - BULL AM ASTRON SOC
VL  - 56
PY  - 2024
IS  - 2
SN  - 0002-7537
UR  - https://m2.mtmt.hu/api/publication/34749869
ID  - 34749869
AB  - 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.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Krtička, Jiří
AU  - Benáček, Jan
AU  - Budaj, Jan
AU  - Korčáková, Daniela
AU  - Pál, András
AU  - Piecka, Martin
AU  - Zejda, Miloslav
AU  - Bakış, Volkan
AU  - Brož, Miroslav
AU  - Chang, Hsiang-Kuang
AU  - Faltová, Nikola
AU  - Gális, Rudolf
AU  - Jadlovský, Daniel
AU  - Janík, Jan
AU  - Kára, Jan
AU  - Kolář, Jakub
AU  - Krtičková, Iva
AU  - Kubát, Jiří
AU  - Kubátová, Brankica
AU  - Kurfürst, Petr
AU  - Labaj, Matúš
AU  - Merc, Jaroslav
AU  - Mikulášek, Zdeněk
AU  - Münz, Filip
AU  - Paunzen, Ernst
AU  - Prišegen, Michal
AU  - Ramezani, Tahereh
AU  - Rievajová, Tatiana
AU  - Řípa, Jakub
AU  - Schmidtobreick, Linda
AU  - Skarka, Marek
AU  - Szász, Gabriel
AU  - Weiss, Werner
AU  - Zajaček, Michal
AU  - Werner, Norbert
TI  - Science with a Small Two-Band UV-Photometry Mission II: Observations of Stars and Stellar Systems
JF  - SPACE SCIENCE REVIEWS
J2  - SPACE SCI REV
VL  - 220
PY  - 2024
IS  - 2
SN  - 0038-6308
DO  - 10.1007/s11214-024-01058-1
UR  - https://m2.mtmt.hu/api/publication/34749867
ID  - 34749867
AB  - We outline the impact of a small two-band UV-photometry satellite mission on the field of stellar physics, magnetospheres of stars, binaries, stellar clusters, interstellar matter, and exoplanets. On specific examples of different types of stars and stellar systems, we discuss particular requirements for such a satellite mission in terms of specific mission parameters such as bandpass, precision, cadence, and mission duration. We show that such a mission may provide crucial data not only for hot stars that emit most of their light in UV, but also for cool stars, where UV traces their activity. This is important, for instance, for exoplanetary studies, because the level of stellar activity influences habitability. While the main asset of the two-band UV mission rests in time-domain astronomy, an example of open clusters proves that such a mission would be important also for the study of stellar populations. Properties of the interstellar dust are best explored when combining optical and IR information with observations in UV.
LA  - English
DB  - MTMT
ER  - 

TY  - JOUR
AU  - Royer, P.
AU  - Merle, T.
AU  - Dsilva, K.
AU  - Sekaran, S.
AU  - Van, Winckel H.
AU  - Frémat, Y.
AU  - Van, der Swaelmen M.
AU  - Gebruers, S.
AU  - Tkachenko, A.
AU  - Laverick, M.
AU  - Dirickx, M.
AU  - Raskin, G.
AU  - Hensberge, H.
AU  - Abdul-Masih, M.
AU  - Acke, B.
AU  - Alonso, M. L.
AU  - Bandhu, Mahato S.
AU  - Beck, P. G.
AU  - Behara, N.
AU  - Bloemen, S.
AU  - Buysschaert, B.
AU  - Cox, N.
AU  - Debosscher, J.
AU  - De, Cat P.
AU  - Degroote, P.
AU  - De, Nutte R.
AU  - De, Smedt K.
AU  - de, Vries B.
AU  - Dumortier, L.
AU  - Escorza, A.
AU  - Exter, K.
AU  - Goriely, S.
AU  - Gorlova, N.
AU  - Hillen, M.
AU  - Homan, W.
AU  - Jorissen, A.
AU  - Kamath, D.
AU  - Karjalainen, M.
AU  - Karjalainen, R.
AU  - Lampens, P.
AU  - Lobel, A.
AU  - Lombaert, R.
AU  - Marcos-Arenal, P.
AU  - Menu, J.
AU  - Merges, F.
AU  - Moravveji, E.
AU  - Nemeth, P.
AU  - Neyskens, P.
AU  - Ostensen, R.
AU  - Pápics, P. I.
AU  - Perez, J.
AU  - Prins, S.
AU  - Royer, S.
AU  - Samadi-Ghadim, A.
AU  - Sana, H.
AU  - Sans, Fuentes A.
AU  - Scaringi, S.
AU  - Schmid, V.
AU  - Siess, L.
AU  - Siopis, C.
AU  - Smolders, K.
AU  - Sódor, Ádám
AU  - Thoul, A.
AU  - Triana, S.
AU  - Vandenbussche, B.
AU  - Van, de Sande M.
AU  - Van, De Steene G.
AU  - Van, Eck S.
AU  - van, Hoof P. A. M.
AU  - Van, Marle A. J.
AU  - Van, Reeth T.
AU  - Vermeylen, L.
AU  - Volpi, D.
AU  - Vos, J.
AU  - Waelkens, C.
TI  - MELCHIORS. The Mercator Library of High Resolution Stellar Spectroscopy
JF  - ASTRONOMY & ASTROPHYSICS
J2  - ASTRON ASTROPHYS
VL  - 681
PY  - 2024
SN  - 0004-6361
DO  - 10.1051/0004-6361/202346847
UR  - https://m2.mtmt.hu/api/publication/34749560
ID  - 34749560
AB  - Aims: Over the past decades, libraries of stellar spectra have been used in a large variety of science cases, including as sources of reference spectra for a given object or a given spectral type. Despite the existence of large libraries and the increasing number of projects of large-scale spectral surveys, there is to date only one very high-resolution spectral library offering spectra from a few hundred objects from the southern hemisphere (UVES-POP). We aim to extend the sample, offering a finer coverage of effective temperatures and surface gravity with a uniform collection of spectra obtained in the northern hemisphere. Methods: Between 2010 and 2020, we acquired several thousand echelle spectra of bright stars with the Mercator-HERMES spectrograph located in the Roque de Los Muchachos Observatory in La Palma, whose pipeline offers high-quality data reduction products. We have also developed methods to correct for the instrumental response in order to approach the true shape of the spectral continuum. Additionally, we have devised a normalisation process to provide a homogeneous normalisation of the full spectral range for most of the objects. Results: We present a new spectral library consisting of 3256 spectra covering 2043 stars. It combines high signal-to-noise and high spectral resolution over the entire range of effective temperatures and luminosity classes. The spectra are presented in four versions: raw, corrected from the instrumental response, with and without correction from the atmospheric molecular absorption, and normalised (including the telluric correction). The dataset described in Appendix A is available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/681/A107 and at www.royer.se/melchiors.html
LA  - English
DB  - MTMT
ER  -