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174 results on '"KÓSPÁL, ÁGNES"'

152. A multiwavelength study of the debris disc around 49 Cet

Author

Pawellek, Nicole, primary, Moór, Attila, additional, Milli, Julien, additional, Kóspál, Ágnes, additional, Olofsson, Johan, additional, Ábrahám, Péter, additional, Keppler, Miriam, additional, Kral, Quentin, additional, Pohl, Adriana, additional, Augereau, Jean-Charles, additional, Boccaletti, Anthony, additional, Chauvin, Gaël, additional, Choquet, Élodie, additional, Engler, Natalia, additional, Henning, Thomas, additional, Langlois, Maud, additional, Lee, Eve J, additional, Ménard, François, additional, Thébault, Philippe, additional, and Zurlo, Alice, additional

Published
2019
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153. Chemical Signatures of the FU Ori Outbursts

Author

Molyarova, Tamara, primary, Akimkin, Vitaly, additional, Semenov, Dmitry, additional, Ábrahám, Péter, additional, Henning, Thomas, additional, Kóspál, Ágnes, additional, Vorobyov, Eduard, additional, and Wiebe, Dmitri, additional

Published
2018
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154. Near-infrared High-resolution Imaging Polarimetry of FU Ori-type Objects: Toward a Unified Scheme for Low-mass Protostellar Evolution

Author

Takami, Michihiro, primary, Fu, Guangwei, additional, Liu, Hauyu Baobab, additional, Karr, Jennifer L., additional, Hashimoto, Jun, additional, Kudo, Tomoyuki, additional, Vorobyov, Eduard I., additional, Kóspál, Ágnes, additional, Scicluna, Peter, additional, Dong, Ruobing, additional, Tamura, Motohide, additional, Pyo, Tae-Soo, additional, Fukagawa, Misato, additional, Tsuribe, Toru, additional, Dunham, Michael M., additional, Henning, Thomas, additional, and Leon, Jerome de, additional

Published
2018
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156. Chemical modeling of FU Ori protoplanetary disks

Author

Molyarova, Tamara, primary, Akimkin, Vitaly, additional, Semenov, Dmitry, additional, Ábrahám, Péter, additional, Henning, Thomas, additional, Kóspál, Ágnes, additional, Vorobyov, Eduard, additional, and Wiebe, Dmitri, additional

Published
2018
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157. A 1.3 mm SMA survey of 29 variable young stellar objects

Author

Liu, Hauyu Baobab, primary, Dunham, Michael M., additional, Pascucci, Ilaria, additional, Bourke, Tyler L., additional, Hirano, Naomi, additional, Longmore, Steven, additional, Andrews, Sean, additional, Carrasco-González, Carlos, additional, Forbrich, Jan, additional, Galván-Madrid, Roberto, additional, Girart, Josep M., additional, Green, Joel D., additional, Juárez, Carmen, additional, Kóspál, Ágnes, additional, Manara, Carlo F., additional, Palau, Aina, additional, Takami, Michihiro, additional, Testi, Leonardo, additional, and Vorobyov, Eduard I., additional

Published
2018
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158. Molecular Gas in Debris Disks around Young A-type Stars

Author

Moór, Attila, primary, Curé, Michel, additional, Kóspál, Ágnes, additional, Ábrahám, Péter, additional, Csengeri, Timea, additional, Eiroa, Carlos, additional, Gunawan, Diah, additional, Henning, Thomas, additional, Hughes, A. Meredith, additional, Juhász, Attila, additional, Pawellek, Nicole, additional, and Wyatt, Mark, additional

Published
2017
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159. A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+

Author

Flaherty, Kevin M., primary, Hughes, A. Meredith, additional, Rose, Sanaea C., additional, Simon, Jacob B., additional, Qi, Chunhua, additional, Andrews, Sean M., additional, Kóspál, Ágnes, additional, Wilner, David J., additional, Chiang, Eugene, additional, Armitage, Philip J., additional, and Bai, Xue-ning, additional

Published
2017
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160. A concordant scenario to explain FU Orionis from deep centimeter and millimeter interferometric observations

Author

Liu, Hauyu Baobab, primary, Vorobyov, Eduard I., additional, Dong, Ruobing, additional, Dunham, Michael M., additional, Takami, Michihiro, additional, Galván-Madrid, Roberto, additional, Hashimoto, Jun, additional, Kóspál, Ágnes, additional, Henning, Thomas, additional, Tamura, Motohide, additional, Rodríguez, Luis F., additional, Hirano, Naomi, additional, Hasegawa, Yasuhiro, additional, Fukagawa, Misato, additional, Carrasco-Gonzalez, Carlos, additional, and Tazzari, Marco, additional

Published
2017
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161. Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

Author

Hughes, A. Meredith, primary, Lieman-Sifry, Jesse, additional, Flaherty, Kevin M., additional, Daley, Cail M., additional, Roberge, Aki, additional, Kóspál, Ágnes, additional, Moór, Attila, additional, Kamp, Inga, additional, Wilner, David J., additional, Andrews, Sean M., additional, Kastner, Joel H., additional, and Ábrahám, Peter, additional

Published
2017
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162. Resolving the Radio Complexity of EXor and FUor-type Systems with the ngVLA.

Author

White, Jacob Aaron, Audard, Marc, Ábrahám, Péter, Cieza, Lucas, Cruz-Sáenz de Miera, Fernando, Dunham, Michael M., Green, Joel D., Güdel, Manuel, Grosso, Nicolas, Hales, Antonio, Hartmann, Lee, Kadam, Kundan, Kastner, Joel H., Kóspál, Ágnes, Perez, Sebastian, Postel, Andreas, Ruiz-Rodriguez, Dary, Rab, Christian, Vorobyov, Eduard I., and Zhaohuan Zhu

Published
2018

163. Accretion dynamics of EX Lupi in quiescence

Author

Sicilia-Aguilar, Aurora, Fang, Min, Roccatagliata, Veronica, Cameron, Andrew Collier, Kóspál, Ágnes, Henning, Thomas, Ábrahám, Peter, and Sipos, Nikoletta

Published
2015

165. ABSENCE OF SIGNIFICANT COOL DISKS IN YOUNG STELLAR OBJECTS EXHIBITING REPETITIVE OPTICAL OUTBURSTS

Author

Liu, Hauyu Baobab, primary, Galván-Madrid, Roberto, additional, Vorobyov, Eduard I., additional, Kóspál, Ágnes, additional, Rodríguez, Luis F., additional, Dunham, Michael M., additional, Hirano, Naomi, additional, Henning, Thomas, additional, Takami, Michihiro, additional, Dong, Ruobing, additional, Hashimoto, Jun, additional, Hasegawa, Yasuhiro, additional, and Carrasco-González, Carlos, additional

Published
2016
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166. Accretion dynamics of EX Lupi in quiescence

Author

Sicilia-Aguilar, Aurora, primary, Fang, Min, additional, Roccatagliata, Veronica, additional, Cameron, Andrew Collier, additional, Kóspál, Ágnes, additional, Henning, Thomas, additional, Ábrahám, Peter, additional, and Sipos, Nikoletta, additional

Published
2015
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167. A concordant scenario to explain FU Orionis from deep centimeter and millimeter interferometric observations.

Author

Hauyu Baobab Liu, Vorobyov, Eduard I., Ruobing Dong, Dunham, Michael M., Michihiro Takami, Galván-Madrid, Roberto, Hashimoto, Jun, Kóspál, Ágnes, Henning, Thomas, Tamura, Motohide, Rodríguez, Luis F., Naomi Hirano, Yasuhiro Hasegawa, Misato Fukagawa, Carrasco-Gonzalez, Carlos, and Tazzari, Marco

Subjects
SPECTRAL energy distribution, GRAVITATIONAL interactions, GRAVITATIONAL instability, THERMAL instability, IONIZED gases, EXPECTED returns
Abstract

Aims: The aim of this work is to constrain properties of the disk around the archetype FU Orionis object, FU Ori, with as good as ~25 au resolution. Methods. We resolved FU Ori at 29-37 GHz using the Karl G. Jansky Very Large Array (JVLA) in the A-array configuration, which provided the highest possible angular resolution to date at this frequency band (~007). We also performed complementary JVLA 8-10 GHz observations, Submillimeter Array (SMA) 224 GHz and 272 GHz observations, and compared these with archival Atacama Large Millimeter Array (ALMA) 346 GHz observations to obtain the spectral energy distributions (SEDs). Results: Our 8-10 GHz observations do not find evidence for the presence of thermal radio jets, and constrain the radio jet/wind flux to at least 90 times lower than the expected value from the previously reported bolometric luminosity-radio luminosity correlation. The emission at frequencies higher than 29 GHz may be dominated by the two spatially unresolved sources, which are located immediately around FU Ori and its companion FU Ori S, respectively. Their deconvolved radii at 33 GHz are only a few au, which is two orders of magnitude smaller in linear scale than the gaseous disk revealed by the previous Subaru-HiCIAO 1.6 µm coronagraphic polarization imaging observations. We are struck by the fact that these two spatially compact sources contribute to over 50% of the observed fluxes at 224 GHz, 272 GHz, and 346 GHz. The 8-346 GHz SEDs of FU Ori and FU Ori S cannot be fit by constant spectral indices (over frequency), although we cannot rule out that it is due to the time variability of their (sub)millimeter fluxes. Conclusions: The more sophisticated models for SEDs considering the details of the observed spectral indices in the millimeter bands suggest that the >29 GHz emission is contributed by a combination of free-free emission from ionized gas and thermal emission from optically thick and optically thin dust components. We hypothesize that dust in the innermost parts of the disks (≤0.1 au) has been sublimated, and thus the disks are no longer well shielded against the ionizing photons. The estimated overall gas and dust mass based on SED modeling, can be as high as a fraction of a solar mass, which is adequate for developing disk gravitational instability. Our present explanation for the observational data is that the massive inflow of gas and dust due to disk gravitational instability or interaction with a companion/intruder, was piled up at the few-au scale due to the development of a deadzone with negligible ionization. The piled up material subsequently triggered the thermal instability and the magnetorotational instability when the ionization fraction in the inner sub-au scale region exceeded a threshold value, leading to the high protostellar accretion rate. [ABSTRACT FROM AUTHOR]

Published
2017
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168. AN ANALYSIS OF THE ENVIRONMENTS OF FU ORIONIS OBJECTS WITHHERSCHEL

Author

Green, Joel D., primary, Evans, Neal J., additional, Kóspál, Ágnes, additional, Herczeg, Gregory, additional, Quanz, Sascha P., additional, Henning, Thomas, additional, van Kempen, Tim A., additional, Lee, Jeong-Eun, additional, Dunham, Michael M., additional, Meeus, Gwendolyn, additional, Bouwman, Jeroen, additional, Chen, Jo-hsin, additional, Güdel, Manuel, additional, Skinner, Stephen L., additional, Liebhart, Armin, additional, and Merello, Manuel, additional

Published
2013
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170. DISENTANGLING THE ENVIRONMENT OF THE FU ORIONIS CANDIDATE HBC 722 WITH HERSCHEL

Author

Green, Joel D., primary, Evans II, Neal J., additional, Kóspál, Ágnes, additional, van Kempen, Tim A., additional, Herczeg, Gregory, additional, Quanz, Sascha P., additional, Henning, Thomas, additional, Lee, Jeong-Eun, additional, Dunham, Michael M., additional, Meeus, Gwendolyn, additional, Bouwman, Jeroen, additional, van Dishoeck, Ewine, additional, Chen, Jo-Hsin, additional, Güdel, Manuel, additional, Skinner, Stephen L., additional, Merello, Manuel, additional, Pooley, David, additional, Rebull, Luisa M., additional, and Guieu, Sylvain, additional

Published
2011
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172. Disks around young stars with VLTI/MIDI

Author

van Boekel, Roy, primary, Ábrahám, Péter, additional, Correia, Serge, additional, de Koter, Alex, additional, Dominik, Carsten, additional, Dutrey, Anne, additional, Henning, Thomas, additional, Kóspál, Ágnes, additional, Lachaume, Régis, additional, Leinert, Christoph, additional, Linz, Hendrik, additional, Min, Michiel, additional, Mosoni, László, additional, Preibisch, Thomas, additional, Quanz, Sascha, additional, Ratzka, Thorsten, additional, Schegerer, Alexander, additional, Waters, Rens, additional, Wolf, Sebastian, additional, and Zinnecker, Hans, additional

Published
2006
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173. The inner disks of EXor-type eruptive stars

Author

Sipos, Nikoletta, Kóspál, Ágnes, Sipos, Nikoletta, and Kóspál, Ágnes

Abstract

EX Lupi-type young stars (EXors) show sporadic brightenings of several magnitudes, caused by the episodic increase in the accretion rate of the circumstellar matter onto the young star. As the inner disk plays a crucial role during the onset of the outburst, we examined the quiescent properties of the circumstellar environment of EXors, focusing on the inner regions. We found that in case of three EXors (VY Tau, V1143 Ori and EX Lup) the spectral energy distributions show no or weak excess above the stellar photosphere at NIR-MIR wavelengths, indicative of inner disk clearing. A detailed radiative transfer modeling of the sources revealed that the inner regions of these disks had to go through significant evolution, either the inner radius of the dusty disk is beyond the sublimation radius and/or the inner disks are flattened

174. The accretion variability in the young multiple system WX Cha

Author

Fiorellino, Eleonora, Zsidi ,Gabriella, Kóspál, Ágnes, and Ábrahám, Péter

Subjects
Stellar Astrophysics, Accretion, Astrophysics::High Energy Astrophysical Phenomena, Star formation, Multiple systems, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Variability, Astrophysics::Galaxy Astrophysics, Young stellar objects
Abstract

One of the main contributor to the photometric variability of pre-main sequence stars is the mass accretion rate, which regulates the interplay between the forming star and the protoplanetary disk. In multiple systems, the accretion scenario is furthermore complicated by the interaction of the components, and by the eventual presence of a circumbinary disk. The multiple system WX Cha, composed of three young stellar objects, is one of the best candidates to investigate the accretion rates to study how the photometric variability is related to the accretion process in multiple systems. We collected high resolution spectroscopy (ESO2.2/FEROS + VLT/ESPRESSO) in 7 different epochs, as well as ground-based and spaceborne (TESS) multi-epoch VIS/IR photometry of the young multiple system WXCha. The multi-wavelength light curves exhibit quasi-periodic variability of about 0.5 mag. Analysing the TESS light curve, we found a significant period of 9.6 days, which we assign to one of the orbital periods in the system (Fig. 1). We studied the variability of selected emission lines (Fig. 2) that trace the accretion, to compute the accretion luminosity with empirical relations (Alcalà+2017). We computed accretion luminosity and mass accretion rate for each epoch (Fig. 3) by measuring our flux calibrated spectra, taking stellar parameters from the literature (Daemgen+13). Our preliminary data show that WX Cha is accreting as a rate typical of TTauri stars system. Daily changes in the accretion luminosity can explain the photometric variability, and the extinction can be considered constant. The relative contributions of the three stellar components to the accretion will be the topic of further studies. &nbsp

Published
2021
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