Search

Your search keyword '"Sódor, Ádám"' showing total 30 results
Start Over Author "Sódor, Ádám"
30 results on '"Sódor, Ádám"'

1. Ejecta masses in Type Ia Supernovae -- Implications for the Progenitor and the Explosion Scenario

Author

Bora, Zsófia, Könyves-Tóth, Réka, Vinkó, József, Bánhidi, Dominik, Bíró, Imre Barna, Bostroem, K. Azalee, Bódi, Attila, Burke, Jamison, Csányi, István, Cseh, Borbála, Farah, Joseph, Filippenko, Alexei V., Hegedűs, Tibor, Hiramatsu, Daichi, Horti-Dávid, Ágoston, Howell, D. Andrew, Jha, Saurabh W., Kalup, Csilla, Krezinger, Máté, Kriskovics, Levente, McCully, Curtis, Newsome, Megan, Ordasi, András, Gonzalez, Estefania Padilla, Pál, András, Pellegrino, Craig, Seli, Bálint, Sódor, Ádám, Szabó, Zsófia Marianna, Szabó, Norton O., Szakáts, Róbert, Szalai, Tamás, Székely, Péter, Terreran, Giacomo, Varga, Vázsony, Vida, Krisztián, Wang, Xiaofeng, and Wheeler, J. Craig

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

The progenitor system(s) as well as the explosion mechanism(s) of thermonuclear (Type Ia) supernovae are long-standing issues in astrophysics. Here we present ejecta masses and other physical parameters for 28 recent Type Ia supernovae inferred from multiband photometric and optical spectroscopic data. Our results confirm that the majority of SNe Ia show {\it observable} ejecta masses below the Chandrasekhar-limit (having a mean $M_{\rm ej} \approx 1.1 \pm 0.3$ M$_\odot$), consistent with the predictions of recent sub-M$_{\rm Ch}$ explosion models. They are compatible with models assuming either single- or double-degenerate progenitor configurations. We also recover a sub-sample of supernovae within $1.2 $ M$_\odot$ $< M_{\rm {ej}} < 1.5$ M$_\odot$ that are consistent with near-Chandrasekhar explosions. Taking into account the uncertainties of the inferred ejecta masses, about half of our SNe are compatible with both explosion models. We compare our results with those in previous studies, and discuss the caveats and concerns regarding the applied methodology.

Published
2024

2. The PLATO Mission

Author

Rauer, Heike, Aerts, Conny, Cabrera, Juan, Deleuil, Magali, Erikson, Anders, Gizon, Laurent, Goupil, Mariejo, Heras, Ana, Lorenzo-Alvarez, Jose, Marliani, Filippo, Martin-Garcia, Cesar, Mas-Hesse, J. Miguel, O'Rourke, Laurence, Osborn, Hugh, Pagano, Isabella, Piotto, Giampaolo, Pollacco, Don, Ragazzoni, Roberto, Ramsay, Gavin, Udry, Stéphane, Appourchaux, Thierry, Benz, Willy, Brandeker, Alexis, Güdel, Manuel, Janot-Pacheco, Eduardo, Kabath, Petr, Kjeldsen, Hans, Min, Michiel, Santos, Nuno, Smith, Alan, Suarez, Juan-Carlos, Werner, Stephanie C., Aboudan, Alessio, Abreu, Manuel, Acuña, Lorena, Adams, Moritz, Adibekyan, Vardan, Affer, Laura, Agneray, François, Agnor, Craig, Børsen-Koch, Victor Aguirre, Ahmed, Saad, Aigrain, Suzanne, Al-Bahlawan, Ashraf, Gil, M de los Angeles Alcacera, Alei, Eleonora, Alencar, Silvia, Alexander, Richard, Alfonso-Garzón, Julia, Alibert, Yann, Prieto, Carlos Allende, Almeida, Leonardo, Sobrino, Roi Alonso, Altavilla, Giuseppe, Althaus, Christian, Trujillo, Luis Alonso Alvarez, Amarsi, Anish, Eiff, Matthias Ammler-von, Amôres, Eduardo, Andrade, Laerte, Antoniadis-Karnavas, Alexandros, António, Carlos, del Moral, Beatriz Aparicio, Appolloni, Matteo, Arena, Claudio, Armstrong, David, Aliaga, Jose Aroca, Asplund, Martin, Audenaert, Jeroen, Auricchio, Natalia, Avelino, Pedro, Baeke, Ann, Baillié, Kevin, Balado, Ana, Balestra, Andrea, Ball, Warrick, Ballans, Herve, Ballot, Jerome, Barban, Caroline, Barbary, Gaële, Barbieri, Mauro, Forteza, Sebastià Barceló, Barker, Adrian, Barklem, Paul, Barnes, Sydney, Navascues, David Barrado, Barragan, Oscar, Baruteau, Clément, Basu, Sarbani, Baudin, Frederic, Baumeister, Philipp, Bayliss, Daniel, Bazot, Michael, Beck, Paul G., Bedding, Tim, Belkacem, Kevin, Bellinger, Earl, Benatti, Serena, Benomar, Othman, Bérard, Diane, Bergemann, Maria, Bergomi, Maria, Bernardo, Pierre, Biazzo, Katia, Bignamini, Andrea, Bigot, Lionel, Billot, Nicolas, Binet, Martin, Biondi, David, Biondi, Federico, Birch, Aaron C., Bitsch, Bertram, Ceballos, Paz Victoria Bluhm, Bódi, Attila, Bognár, Zsófia, Boisse, Isabelle, Bolmont, Emeline, Bonanno, Alfio, Bonavita, Mariangela, Bonfanti, Andrea, Bonfils, Xavier, Bonito, Rosaria, Bonomo, Aldo Stefano, Börner, Anko, Saikia, Sudeshna Boro, Martín, Elisa Borreguero, Borsa, Francesco, Borsato, Luca, Bossini, Diego, Bouchy, Francois, Boué, Gwenaël, Boufleur, Rodrigo, Boumier, Patrick, Bourrier, Vincent, Bowman, Dominic M., Bozzo, Enrico, Bradley, Louisa, Bray, John, Bressan, Alessandro, Breton, Sylvain, Brienza, Daniele, Brito, Ana, Brogi, Matteo, Brown, Beverly, Brown, David, Brun, Allan Sacha, Bruno, Giovanni, Bruns, Michael, Buchhave, Lars A., Bugnet, Lisa, Buldgen, Gaël, Burgess, Patrick, Busatta, Andrea, Busso, Giorgia, Buzasi, Derek, Caballero, José A., Cabral, Alexandre, Calderone, Flavia, Cameron, Robert, Cameron, Andrew, Campante, Tiago, Martins, Bruno Leonardo Canto, Cara, Christophe, Carone, Ludmila, Carrasco, Josep Manel, Casagrande, Luca, Casewell, Sarah L., Cassisi, Santi, Castellani, Marco, Castro, Matthieu, Catala, Claude, Fernández, Irene Catalán, Catelan, Márcio, Cegla, Heather, Cerruti, Chiara, Cessa, Virginie, Chadid, Merieme, Chaplin, William, Charpinet, Stephane, Chiappini, Cristina, Chiarucci, Simone, Chiavassa, Andrea, Chinellato, Simonetta, Chirulli, Giovanni, Christensen-Dalsgaard, Jorgen, Church, Ross, Claret, Antonio, Clarke, Cathie, Claudi, Riccardo, Clermont, Lionel, Coelho, Hugo, Coelho, Joao, Cogato, Fabrizio, Colomé, Josep, Condamin, Mathieu, Conseil, Simon, Corbard, Thierry, Correia, Alexandre C. M., Corsaro, Enrico, Cosentino, Rosario, Costes, Jean, Cottinelli, Andrea, Covone, Giovanni, Creevey, Orlagh L., Crida, Aurelien, Csizmadia, Szilard, Cunha, Margarida, Curry, Patrick, da Costa, Jefferson, da Silva, Francys, Dalal, Shweta, Damasso, Mario, Damiani, Cilia, Damiani, Francesco, Chagas, Maria Liduina das, Davies, Melvyn, Davies, Guy, Davies, Ben, Davison, Gary, de Almeida, Leandro, de Angeli, Francesca, de Barros, Susana Cristina Cabral, Leão, Izan de Castro, de Freitas, Daniel Brito, de Freitas, Marcia Cristina, De Martino, Domitilla, de Medeiros, José Renan, de Paula, Luiz Alberto, de Plaa, Jelle, De Ridder, Joris, Deal, Morgan, Decin, Leen, Deeg, Hans, Degl'Innocenti, Scilla, Deheuvels, Sebastien, del Burgo, Carlos, Del Sordo, Fabio, Delgado-Mena, Elisa, Demangeon, Olivier, Denk, Tilmann, Derekas, Aliz, Desidera, Silvano, Dexet, Marc, Di Criscienzo, Marcella, Di Giorgio, Anna Maria, Di Mauro, Maria Pia, Rial, Federico Jose Diaz, Díaz-García, José-Javier, Dima, Marco, Dinuzzi, Giacomo, Dionatos, Odysseas, Distefano, Elisa, Nascimento Jr., Jose-Dias do, Domingo, Albert, D'Orazi, Valentina, Dorn, Caroline, Doyle, Lauren, Duarte, Elena, Ducellier, Florent, Dumaye, Luc, Dumusque, Xavier, Dupret, Marc-Antoine, Eggenberger, Patrick, Ehrenreich, David, Eigmüller, Philipp, Eising, Johannes, Emilio, Marcelo, Eriksson, Kjell, Ermocida, Marco, Giribaldi, Riano Isidoro Escate, Eschen, Yoshi, Estrela, Inês, Evans, Dafydd Wyn, Fabbian, Damian, Fabrizio, Michele, Faria, João Pedro, Farina, Maria, Farinato, Jacopo, Feliz, Dax, Feltzing, Sofia, Fenouillet, Thomas, Ferrari, Lorenza, Ferraz-Mello, Sylvio, Fialho, Fabio, Fienga, Agnes, Figueira, Pedro, Fiori, Laura, Flaccomio, Ettore, Focardi, Mauro, Foley, Steve, Fontignie, Jean, Ford, Dominic, Fornazier, Karin, Forveille, Thierry, Fossati, Luca, Franca, Rodrigo de Marca, da Silva, Lucas Franco, Frasca, Antonio, Fridlund, Malcolm, Furlan, Marco, Gabler, Sarah-Maria, Gaido, Marco, Gallagher, Andrew, Galli, Emanuele, Garcia, Rafael A., Hernández, Antonio García, Munoz, Antonio Garcia, García-Vázquez, Hugo, Haba, Rafael Garrido, Gaulme, Patrick, Gauthier, Nicolas, Gehan, Charlotte, Gent, Matthew, Georgieva, Iskra, Ghigo, Mauro, Giana, Edoardo, Gill, Samuel, Girardi, Leo, Winter, Silvia Giuliatti, Giusi, Giovanni, da Silva, João Gomes, Zazo, Luis Jorge Gómez, Gomez-Lopez, Juan Manuel, Hernández, Jonay Isai González, Murillo, Kevin Gonzalez, Gorius, Nicolas, Gouel, Pierre-Vincent, Goulty, Duncan, Granata, Valentina, Grenfell, John Lee, Grießbach, Denis, Grolleau, Emmanuel, Grouffal, Salomé, Grziwa, Sascha, Guarcello, Mario Giuseppe, Gueguen, Loïc, Guenther, Eike Wolf, Guilhem, Terrasa, Guillerot, Lucas, Guiot, Pierre, Guterman, Pascal, Gutiérrez, Antonio, Gutiérrez-Canales, Fernando, Hagelberg, Janis, Haldemann, Jonas, Hall, Cassandra, Handberg, Rasmus, Harrison, Ian, Harrison, Diana L., Hasiba, Johann, Haswell, Carole A., Hatalova, Petra, Hatzes, Artie, Haywood, Raphaelle, Hébrard, Guillaume, Heckes, Frank, Heiter, Ulrike, Hekker, Saskia, Heller, René, Helling, Christiane, Helminiak, Krzysztof, Hemsley, Simon, Heng, Kevin, Hermans, Aline, Hermes, JJ, Torres, Nadia Hidalgo, Hinkel, Natalie, Hobbs, David, Hodgkin, Simon, Hofmann, Karl, Hojjatpanah, Saeed, Houdek, Günter, Huber, Daniel, Huesler, Joseph, Hui-Bon-Hoa, Alain, Huygen, Rik, Huynh, Duc-Dat, Iro, Nicolas, Irwin, Jonathan, Irwin, Mike, Izidoro, André, Jacquinod, Sophie, Jannsen, Nicholas Emborg, Janson, Markus, Jeszenszky, Harald, Jiang, Chen, Mancebo, Antonio José Jimenez, Jofre, Paula, Johansen, Anders, Johnston, Cole, Jones, Geraint, Kallinger, Thomas, Kálmán, Szilárd, Kanitz, Thomas, Karjalainen, Marie, Karjalainen, Raine, Karoff, Christoffer, Kawaler, Steven, Kawata, Daisuke, Keereman, Arnoud, Keiderling, David, Kennedy, Tom, Kenworthy, Matthew, Kerschbaum, Franz, Kidger, Mark, Kiefer, Flavien, Kintziger, Christian, Kislyakova, Kristina, Kiss, László, Klagyivik, Peter, Klahr, Hubert, Klevas, Jonas, Kochukhov, Oleg, Köhler, Ulrich, Kolb, Ulrich, Koncz, Alexander, Korth, Judith, Kostogryz, Nadiia, Kovács, Gábor, Kovács, József, Kozhura, Oleg, Krivova, Natalie, Kučinskas, Arunas, Kuhlemann, Ilyas, Kupka, Friedrich, Laauwen, Wouter, Labiano, Alvaro, Lagarde, Nadege, Laget, Philippe, Laky, Gunter, Lam, Kristine Wai Fun, Lambrechts, Michiel, Lammer, Helmut, Lanza, Antonino Francesco, Lanzafame, Alessandro, Martiz, Mariel Lares, Laskar, Jacques, Latter, Henrik, Lavanant, Tony, Lawrenson, Alastair, Lazzoni, Cecilia, Lebre, Agnes, Lebreton, Yveline, Etangs, Alain Lecavelier des, Leinhardt, Zoe, Leleu, Adrien, Lendl, Monika, Leto, Giuseppe, Levillain, Yves, Libert, Anne-Sophie, Lichtenberg, Tim, Ligi, Roxanne, Lignieres, Francois, Lillo-Box, Jorge, Linsky, Jeffrey, Liu, John Scige, Loidolt, Dominik, Longval, Yuying, Lopes, Ilídio, Lorenzani, Andrea, Ludwig, Hans-Guenter, Lund, Mikkel, Lundkvist, Mia Sloth, Luri, Xavier, Maceroni, Carla, Madden, Sean, Madhusudhan, Nikku, Maggio, Antonio, Magliano, Christian, Magrin, Demetrio, Mahy, Laurent, Maibaum, Olaf, Malac-Allain, LeeRoy, Malapert, Jean-Christophe, Malavolta, Luca, Maldonado, Jesus, Mamonova, Elena, Manchon, Louis, Mann, Andrew, Mantovan, Giacomo, Marafatto, Luca, Marconi, Marcella, Mardling, Rosemary, Marigo, Paola, Marinoni, Silvia, Marques, Érico, Marques, Joao Pedro, Marrese, Paola Maria, Marshall, Douglas, Perales, Silvia Martínez, Mary, David, Marzari, Francesco, Masana, Eduard, Mascher, Andrina, Mathis, Stéphane, Mathur, Savita, Figueiredo, Ana Carolina Mattiuci, Maxted, Pierre F. L., Mazeh, Tsevi, Mazevet, Stephane, Mazzei, Francesco, McCormac, James, McMillan, Paul, Menou, Lucas, Merle, Thibault, Meru, Farzana, Mesa, Dino, Messina, Sergio, Mészáros, Szabolcs, Meunier, Nadége, Meunier, Jean-Charles, Micela, Giuseppina, Michaelis, Harald, Michel, Eric, Michielsen, Mathias, Michtchenko, Tatiana, Miglio, Andrea, Miguel, Yamila, Milligan, David, Mirouh, Giovanni, Mitchell, Morgan, Moedas, Nuno, Molendini, Francesca, Molnár, László, Mombarg, Joey, Montalban, Josefina, Montalto, Marco, Monteiro, Mário J. P. F. G., Morales, Juan Carlos, Morales-Calderon, Maria, Morbidelli, Alessandro, Mordasini, Christoph, Moreau, Chrystel, Morel, Thierry, Morello, Guiseppe, Morin, Julien, Mortier, Annelies, Mosser, Benoît, Mourard, Denis, Mousis, Olivier, Moutou, Claire, Mowlavi, Nami, Moya, Andrés, Muehlmann, Prisca, Muirhead, Philip, Munari, Matteo, Musella, Ilaria, Mustill, Alexander James, Nardetto, Nicolas, Nardiello, Domenico, Narita, Norio, Nascimbeni, Valerio, Nash, Anna, Neiner, Coralie, Nelson, Richard P., Nettelmann, Nadine, Nicolini, Gianalfredo, Nielsen, Martin, Niemi, Sami-Matias, Noack, Lena, Noels-Grotsch, Arlette, Noll, Anthony, Norazman, Azib, Norton, Andrew J., Nsamba, Benard, Ofir, Aviv, Ogilvie, Gordon, Olander, Terese, Olivetto, Christian, Olofsson, Göran, Ong, Joel, Ortolani, Sergio, Oshagh, Mahmoudreza, Ottacher, Harald, Ottensamer, Roland, Ouazzani, Rhita-Maria, Paardekooper, Sijme-Jan, Pace, Emanuele, Pajas, Miriam, Palacios, Ana, Palandri, Gaelle, Palle, Enric, Paproth, Carsten, Parro, Vanderlei, Parviainen, Hannu, Granado, Javier Pascual, Passegger, Vera Maria, Pastor-Morales, Carmen, Pätzold, Martin, Pedersen, May Gade, Hidalgo, David Pena, Pepe, Francesco, Pereira, Filipe, Persson, Carina M., Pertenais, Martin, Peter, Gisbert, Petit, Antoine C., Petit, Pascal, Pezzuto, Stefano, Pichierri, Gabriele, Pietrinferni, Adriano, Pinheiro, Fernando, Pinsonneault, Marc, Plachy, Emese, Plasson, Philippe, Plez, Bertrand, Poppenhaeger, Katja, Poretti, Ennio, Portaluri, Elisa, Portell, Jordi, de Mello, Gustavo Frederico Porto, Poyatos, Julien, Pozuelos, Francisco J., Moroni, Pier Giorgio Prada, Pricopi, Dumitru, Prisinzano, Loredana, Quade, Matthias, Quirrenbach160, ndreas, Reina6, Julio Arturo Rabanal, Soares, Maria Cristina Rabello, Raimondo, Gabriella, Rainer, Monica, Rodón, Jose Ramón, Ramón-Ballesta, Alejandro, Zapata, Gonzalo Ramos, Rätz, Stefanie, Rauterberg, Christoph, Redman, Bob, Redmer, Ronald, Reese, Daniel, Regibo, Sara, Reiners, Ansgar, Reinhold, Timo, Renie, Christian, Ribas, Ignasi, Ribeiro, Sergio, Ricciardi, Thiago Pereira, Rice, Ken, Richard, Olivier, Riello, Marco, Rieutord, Michel, Ripepi, Vincenzo, Rixon, Guy, Rockstein, Steve, Rodríguez, María Teresa Rodrigo, Díaz, Luisa Fernanda Rodríguez, Garcia, Juan Pablo Rodriguez, Rodriguez-Gomez, Julio, Roehlly, Yannick, Roig, Fernando, Rojas-Ayala, Bárbara, Rolf, Tobias, Rørsted, Jakob Lysgaard, Rosado, Hugo, Rosotti, Giovanni, Roth, Olivier, Roth, Markus, Rousseau, Alex, Roxburgh, Ian, Roy, Fabrice, Royer, Pierre, Ruane, Kirk, Mastropasqua, Sergio Rufini, de Galarreta, Claudia Ruiz, Russi, Andrea, Saar, Steven, Saillenfest, Melaine, Salaris, Maurizio, Salmon, Sebastien, Saltas, Ippocratis, Samadi, Réza, Samadi, Aunia, Samra, Dominic, da Silva, Tiago Sanches, Carrasco, Miguel Andrés Sánchez, Santerne, Alexandre, Santoli, Francesco, Santos, Ângela R. G., Mesa, Rosario Sanz, Sarro, Luis Manuel, Scandariato, Gaetano, Schäfer, Martin, Schlafly, Edward, Schmider, François-Xavier, Schneider, Jean, Schou, Jesper, Schunker, Hannah, Schwarzkopf, Gabriel Jörg, Serenelli, Aldo, Seynaeve, Dries, Shan, Yutong, Shapiro, Alexander, Shipman, Russel, Sicilia, Daniela, Sanmartin, Maria Angeles Sierra, Sigot, Axelle, Silliman, Kyle, Silvotti, Roberto, Simon, Attila E., Napoli, Ricardo Simoyama, Skarka, Marek, Smalley, Barry, Smiljanic, Rodolfo, Smit, Samuel, Smith, Alexis, Smith, Leigh, Snellen, Ignas, Sódor, Ádám, Sohl, Frank, Solanki, Sami K., Sortino, Francesca, Sousa, Sérgio, Southworth, John, Souto, Diogo, Sozzetti, Alessandro, Stamatellos, Dimitris, Stassun, Keivan, Steller, Manfred, Stello, Dennis, Stelzer, Beate, Stiebeler, Ulrike, Stokholm, Amalie, Storelvmo, Trude, Strassmeier, Klaus, Strøm, Paul Anthony, Strugarek, Antoine, Sulis, Sophia, Švanda, Michal, Szabados, László, Szabó, Róbert, Szabó, Gyula M., Szuszkiewicz, Ewa, Talens, Geert Jan, Teti, Daniele, Theisen, Tom, Thévenin, Frédéric, Thoul, Anne, Tiphene, Didier, Titz-Weider, Ruth, Tkachenko, Andrew, Tomecki, Daniel, Tonfat, Jorge, Tosi, Nicola, Trampedach, Regner, Traven, Gregor, Triaud, Amaury, Trønnes, Reidar, Tsantaki, Maria, Tschentscher, Matthias, Turin, Arnaud, Tvaruzka, Adam, Ulmer, Bernd, Ulmer-Moll, Solène, Ulusoy, Ceren, Umbriaco, Gabriele, Valencia, Diana, Valentini, Marica, Valio, Adriana, Guijarro, Ángel Luis Valverde, Van Eylen, Vincent, Van Grootel, Valerie, van Kempen, Tim A., Van Reeth, Timothy, Van Zelst, Iris, Vandenbussche, Bart, Vasiliou, Konstantinos, Vasilyev, Valeriy, de Mascarenhas, David Vaz, Vazan, Allona, Nunez, Marina Vela, Velloso, Eduardo Nunes, Ventura, Rita, Ventura, Paolo, Venturini, Julia, Trallero, Isabel Vera, Veras, Dimitri, Verdugo, Eva, Verma, Kuldeep, Vibert, Didier, Martinez, Tobias Vicanek, Vida, Krisztián, Vigan, Arthur, Villacorta, Antonio, Villaver, Eva, Aparicio, Marcos Villaverde, Viotto, Valentina, Vorobyov, Eduard, Vorontsov, Sergey, Wagner, Frank W., Walloschek, Thomas, Walton, Nicholas, Walton, Dave, Wang, Haiyang, Waters, Rens, Watson, Christopher, Wedemeyer, Sven, Weeks, Angharad, Weingril, Jörg, Weiss, Annita, Wendler, Belinda, West, Richard, Westerdorff, Karsten, Westphal, Pierre-Amaury, Wheatley, Peter, White, Tim, Whittaker, Amadou, Wickhusen, Kai, Wilson, Thomas, Windsor, James, Winter, Othon, Winther, Mark Lykke, Winton, Alistair, Witteck, Ulrike, Witzke, Veronika, Woitke, Peter, Wolter, David, Wuchterl, Günther, Wyatt, Mark, Yang, Dan, Yu, Jie, Sanchez, Ricardo Zanmar, Osorio, María Rosa Zapatero, Zechmeister, Mathias, Zhou, Yixiao, Ziemke, Claas, and Zwintz, Konstanze

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.

Published
2024

3. The Enigma of Gaia18cjb: a Rare Hybrid of FUor and EXor?

Author

Fiorellino, Eleonora, Abraham, Peter, Kospal, Agnes, Kun, Maria, Alcala, Juan M., Garatti, Alessio Caratti o, de Miera, Fernando Cruz-Saenz, Garcia-Alvarez, David, Giannini, Teresa, Park, Sunkyung, Siwak, Michal, Szilagyi, Mate, Covino, Elvira, Marton, Gabor, Nagy, Zsofia, Nisini, Brunella, Szabo, Zsofia Marianna, Bora, Zsofia, Cseh, Borbala, Kalup, Csilla, Krezinger, Mate, Kriskovics, Levente, Ogloza, Waldemar, Pal, Andras, Sodor, Adam, Sonbas, Eda, Szakats, Robert, Vida, Krisztian, Vinko, Jozsef, Wyrzykowski, Lukasz, and Zielinski, Pawel

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Context. Gaia18cjb is one of the Gaia-alerted eruptive young star candidates which has been experiencing a slow and strong brightening during the last 13 years, similar to some FU Orionis-type objects. Aims. The aim of this work is to derive the young stellar nature of Gaia18cjb, determine its physical and accretion properties to classify its variability. Methods. We conducted monitoring observations using multi-filter optical and near-infrared photometry, as well as near-infrared spectroscopy. We present the analysis of pre-outburst and outburst optical and infrared light curves, color-magnitude diagrams in different bands, the detection of near-IR spectral lines, and estimates of both stellar and accretion parameters during the burst. Results. The optical light curve shows an unusually long (8 years) brightening event of 5 mag in the last 13 years, before reaching a plateau indicating that the burst is still on-going, suggesting a FUor-like nature. The same outburst is less strong in the infrared light curves. The near-infrared spectra, obtained during the outburst, exhibit emission lines typical of highly accreting low-intermediate mass young stars with typical EXor features. The spectral index of Gaia18cjb SED classifies it as a Class I in the pre-burst stage and a Flat Spectrum young stellar object (YSO) during the burst. Conclusions. Gaia18cjb is an eruptive YSO which shows FUor-like photometric features (in terms of brightening amplitude and length of the burst) and EXor-like spectroscopic features and accretion rate, as V350 Cep and V1647 Ori, classified as objects in between FUors and EXors, Comment: 21 pages, 13 figures

Published
2024
Full Text
View/download PDF

4. SN 2022oqm: A Bright and Multi-peaked Calcium-rich Transient

Author

Yadavalli, S. Karthik, Villar, V. Ashley, Izzo, Luca, Zenati, Yossef, Foley, Ryan J., Wheeler, J. Craig, Angus, Charlotte R., Bánhidi, Dominik, Auchettl, Katie, Bíró, Barna Imre, Bódi, Attila, Bodola, Zsófia, de Boer, Thomas, Chambers, Kenneth C., Chornock, Ryan, Coulter, David A., Csányi, István, Cseh, Borbála, Dandu, Srujan, Davis, Kyle W., Dickinson, Connor Braden, Farias, Diego, Farah, Joseph, Gall, Christa, Gao, Hua, Howell, D. Andrew, Jacobson-Galan, Wynn V., Khetan, Nandita, Kilpatrick, Charles D., Könyves-Tóth, Réka, Kriskovics, Levente, LeBaron, Natalie, Loertscher, Kayla, Saux, X. K. Le, Margutti, Rafaella, Magnier, Eugene A., McCully, Curtis, McGill, Peter, Miao, Hao-Yu, Newsome, Megan, Gonzalez, Estefania Padilla, Pál, András, Pál, Boróka H., Pan, Yen-Chen, Politsch, Collin A., Ransome, Conor L., Ramirez-Ruiz, Enrico, Rest, Armin, Rest, Sofia, Robinson, Olivia, Sears, Huei, Scheer, Jackson, Sódor, Ádám, Swift, Jonathan, Székely, Péter, Szakáts, Róbert, Szalai, Tamás, Taggart, Kirsty, Terreran, Giacomo, Venkatraman, Padma, Vinkó, József, Yang, Grace, and Zhou, Henry

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the photometric and spectroscopic evolution of SN 2022oqm, a nearby multi-peaked hydrogen- and helium-weak calcium-rich transient (CaRT). SN 2022oqm was detected 13.1 kpc from its host galaxy, the face-on spiral galaxy NGC 5875. Extensive spectroscopic coverage reveals an early hot (T >= 40,000 K) continuum and carbon features observed $\sim$1~day after discovery, SN Ic-like photospheric-phase spectra, and strong forbidden calcium emission starting 38 days after discovery. SN 2022oqm has a relatively high peak luminosity (MB = -17 mag) for (CaRTs), making it an outlier in the population. We determine that three power sources are necessary to explain the light curve (LC), with each corresponding to a distinct peak. The first peak is powered by an expanding blackbody with a power law luminosity, suggesting shock cooling by circumstellar material (CSM). Subsequent LC evolution is powered by a double radioactive decay model, consistent with two sources of photons diffusing through optically thick ejecta. From the LC, we derive an ejecta mass and 56Ni mass of ~0.6 solar masses and ~0.09 solar masses. Spectroscopic modeling suggests 0.6 solar masses of ejecta, and with well-mixed Fe-peak elements throughout. We discuss several physical origins for SN 2022oqm and find either a surprisingly massive white dwarf progenitor or a peculiar stripped envelope model could explain SN 2022oqm. A stripped envelope explosion inside a dense, hydrogen- and helium-poor CSM, akin to SNe Icn, but with a large 56Ni mass and small CSM mass could explain SN 2022oqm. Alternatively, helium detonation on an unexpectedly massive white dwarf could also explain SN 2022oqm., Comment: 35 pages, 17 figures, 7 tables, Accepted for Publication in ApJ

Published
2023

5. Ground-based observations of the ZZ Ceti star HS 1625+1231

Author

Kalup, Csilla, Bognár, Zsófia, and Sódor, Ádám

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the results of our detailed light curve analysis of the ZZ Ceti star HS 1625+1231. We collected photometric time series data at Konkoly Observatory on 14 nights, and performed Fourier analysis of these data sets. We detected 11 significant frequencies, where six of them are found to be independent pulsation modes in the 514 - 881 s period range. By utilising these frequencies, we performed preliminary asteroseismic investigations to give constraints on the main physical parameters, and to derive seismic distances for the star. Finally, we compared the astrometric distance provided by the Gaia EDR3 data with those seismic distances. Our selected model, considering both the spectroscopic measurements and the distance value provided by Gaia, has $T_{eff}$ = 11 000 K and $M_*$ = 0.60 $M_{\odot}$., Comment: 16 pages, 5 figures, accepted for publication in Acta Astronomica

Published
2021
Full Text
View/download PDF

6. First results on RR Lyrae stars with the TESS space telescope: untangling the connections between mode content, colors and distances

Author

Molnár, László, Bódi, Attila, Pál, András, Bhardwaj, Anupam, Hambsch, Franz-Josef, Benkő, József M., Derekas, Aliz, Ebadi, Mohammad, Joyce, Meridith, Hasanzadeh, Amir, Kolenberg, Katrien, Lund, Michael B., Nemec, James M., Netzel, Henryka, Ngeow, Chow-Choong, Pepper, Joshua, Plachy, Emese, Prudil, Zdeněk, Siverd, Robert J., Skarka, Marek, Smolec, Radosław, Sódor, Ádám, Sylla, Salma, Szabó, Pál, Szabó, Róbert, Kjeldsen, Hans, Christensen-Dalsgaard, Jørgen, and Ricker, George R.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The TESS space telescope is collecting continuous, high-precision optical photometry of stars throughout the sky, including thousands of RR Lyrae stars. In this paper, we present results for an initial sample of 118 nearby RR Lyrae stars observed in TESS Sectors 1 and 2. We use differential-image photometry to generate light curves and analyse their mode content and modulation properties. We combine accurate light curve parameters from TESS with parallax and color information from the Gaia mission to create a comprehensive classification scheme. We build a clean sample, preserving RR Lyrae stars with unusual light curve shapes, while separating other types of pulsating stars. We find that a large fraction of RR Lyrae stars exhibit various low-amplitude modes, but the distribution of those modes is markedly different from those of the bulge stars. This suggests that differences in physical parameters have an observable effect on the excitation of extra modes, potentially offering a way to uncover the origins of these signals. However, mode identification is hindered by uncertainties when identifying the true pulsation frequencies of the extra modes. We compare mode amplitude ratios in classical double-mode stars to stars with extra modes at low amplitudes and find that they separate into two distinct groups. Finally, we find a high percentage of modulated stars among the fundamental-mode pulsators, but also find that at least 28% of them do not exhibit modulation, confirming that a significant fraction of stars lack the Blazhko effect., Comment: 35 pages, 26 figures, and a 19-page appendix. Accepted for publication in ApJS. Light curve data temporarily available: https://konkoly.hu/staff/lmolnar/tess_rrl_firstlight_all_lcs.txt

Published
2021
Full Text
View/download PDF

7. SN 2018agk: A Prototypical Type Ia Supernova with a Smooth Power-law Rise in Kepler (K2)

Author

Wang, Qinan, Rest, Armin, Zenati, Yossef, Ridden-Harper, Ryan, Dimitriadis, Georgios, Narayan, Gautham, Villar, V. Ashley, Magee, Mark R., Foley, Ryan J., Shaya, Edward J., Garnavich, Peter, Wang, Lifan, Hu, Lei, Bodi, Attila, Armstrong, Patrick, Auchettl, Katie, Barclay, Thomas, Barentsen, Geert, Bognár, Zsófia, Brimacombe, Joseph, Bulger, Joanna, Burke, Jamison, Challis, Peter, Chambers, Kenneth, Coulter, David A., Csörnyei, Géza, Cseh, Borbála, Deckers, Maxime, Dotson, Jessie L., Galbany, Lluís, González-Gaitán, Santiago, Gromadzki, Mariusz, Gully-Santiago, Michael, Hanyecz, Ottó, Hedges, Christina, Hiramatsu, Daichi, Hosseinzadeh, Griffin, Howell, D. Andrew, Howell, Steve B., Huber, Mark E., Jha, Saurabh W., Jones, David O., Könyves-Tóth, Réka, Kalup, Csilla, Kilpatrick, Charlie, Kriskovics, Levente, Li, Wenxiong, Lowe, Thomas B, Margheim, Steven, McCully, Curtis, Mitra, Ayan, Muñoz, Jose A., Nicholl, Matt, Nordin, Jakob, Pál, András, Pan, Yen-Chen, Piro, Anthony L, Rest, Sofia, Rino-Silvestre, João, Rojas-Bravo, César, Sárneczky, Krisztián, Siebert, Matthew R., Smartt, Stephen J., Smith, Ken, Sódor, Ádám, Stritzinger, Maximilian D., Szabó, Róbert, Szakáts, Róbert, Tucker, Brad E., Vinkó, József, Wang, Xiaofeng, Wheeler, J. Craig, Young, David R., Zenteno, Alfredo, Zhang, Kaicheng, and Zsidi, Gabriella

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the 30-min cadence Kepler/K2 light curve of the Type Ia supernova (SN Ia) SN 2018agk, covering approximately one week before explosion, the full rise phase and the decline until 40 days after peak. We additionally present ground-based observations in multiple bands within the same time range, including the 1-day cadence DECam observations within the first $\sim$5 days after the first light. The Kepler early light curve is fully consistent with a single power-law rise, without evidence of any bump feature. We compare SN 2018agk with a sample of other SNe~Ia without early excess flux from the literature. We find that SNe Ia without excess flux have slowly-evolving early colors in a narrow range ($g-i\approx -0.20\pm0.20$ mag) within the first $\sim 10$ days. On the other hand, among SNe Ia detected with excess, SN 2017cbv and SN 2018oh tend to be bluer, while iPTF16abc's evolution is similar to normal SNe Ia without excess in $g-i$. We further compare the Kepler light curve of SN 2018agk with companion-interaction models, and rule out the existence of a typical non-degenerate companion undergoing Roche-lobe overflow at viewing angles smaller than $45^{\circ}$., Comment: 20 pages, 14 figures, 5 tables. Published in ApJ

Published
2021
Full Text
View/download PDF

8. Dipper-like variability of the Gaia alerted young star V555 Ori

Author

Nagy, Zsófia, Szegedi-Elek, Elza, Ábrahám, Péter, Kóspál, Ágnes, Bódi, Attila, Bouvier, Jérôme, Kun, Mária, Moór, Attila, Cseh, Borbála, Farkas-Takács, Anikó, Hanyecz, Ottó, Hodgkin, Simon, Ignácz, Bernadett, Kiss, Csaba, Könyves-Tóth, Réka, Kriskovics, Levente, Marton, Gábor, Mészáros, László, Ordasi, András, Pál, András, Sarkis, Paula, Sárneczky, Krisztián, Sódor, Ádám, Szabados, László, Szabó, Zsófia Marianna, Szakáts, Róbert, Tarczay-Nehéz, Dóra, Vida, Krisztián, and Zsidi, Gabriella

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

V555 Ori is a T Tauri star, whose 1.5 mag brightening was published as a Gaia science alert in 2017. We carried out optical and near-infrared photometric, and optical spectroscopic observations to understand the light variations. The light curves show that V555 Ori was faint before 2017, entered a high state for about a year, and returned to the faint state by mid-2018. In addition to the long-term flux evolution, quasi-periodic brightness oscillations were also evident, with a period of about 5 days. At optical wavelengths both the long-term and short-term variations exhibited colourless changes, while in the near-infrared they were consistent with changing extinction. We explain the brightness variations as the consequence of changing extinction. The object has a low accretion rate whose variation in itself would not be enough to reproduce the optical flux changes. This behaviour makes V555 Ori similar to the pre-main sequence star AA Tau, where the light changes are interpreted as periodic eclipses of the star by a rotating inner disc warp. The brightness maximum of V555 Ori was a moderately obscured ($A_V$=2.3 mag) state, while the extinction in the low state was $A_V$=6.4 mag. We found that while the Gaia alert hinted at an accretion burst, V555 Ori is a standard dipper, similar to the prototype AA Tau. However, unlike in AA Tau, the periodic behaviour was also detectable in the faint phase, implying that the inner disc warp remained stable in both the high and low states of the system., Comment: Accepted to MNRAS

Published
2021
Full Text
View/download PDF

9. Photometric and spectroscopic investigations of the Galactic field RRc candidates V764 Mon and HY Com

Author

Benko, Jozsef M., Sodor, Adam, and Pal, Andras

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

By analyzing photometric and spectroscopic time series in this paper, we show that the pulsator V764 Mon, assumed to be the brightest RR Lyrae star in the sky, is in fact a rapidly rotating delta Scuti star with an unusually long dominant period (P1=0.29 d). Our spectroscopy confirmed the discovery of the Gaia satellite about the binarity of V764 Mon. In the case of HY Com, a `bona fide' RRc star, we present its first complete radial velocity curve. Additionally, we found that the star continues its strong phase variation reported before., Comment: 18 pages, 7 figures, 6 tables. To appear in Acta Astron

Published
2021
Full Text
View/download PDF

10. Extended Aperture Photometry of K2 RR Lyrae stars

Author

Plachy, Emese, Molnár, László, Bódi, Attila, Skarka, Marek, Szabó, Pál, Szabó, Róbert, Klagyivik, Péter, Sódor, Ádám, and Pope, Benjamin J. S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The \textit{Kepler} space telescope observed thousands of RR Lyrae stars in the K2 mission. In this paper we present our photometric solutions using extended apertures in order to conserve the flux of the stars to the highest possible extent. With this method we are able to avoid most of the problems that RR Lyrae light curves produced by other pipelines suffer from. For post-processing we apply the K2SC pipeline to our light curves. We provide the EAP (Extended Aperture Photometry) of 432 RR Lyrae stars observed in campaigns 3, 4, 5, and 6. We also provide subclass classifications based on Fourier parameters. We investigated in particular the presence of the Blazhko effect in the stars, and found it to be 44.7\% among the RRab stars, in agreement with results from independent samples. We found that the amplitude and phase modulation in the Blazhko stars may behave rather differently, at least over the length of a K2 Campaign. We also identified four anomalous Cepheid candidates in the sample one of which is potentially the first Blazhko-modulated member of its class., Comment: 20 pages, 13 figures, accepted in ApJS, light curves available at https://konkoly.hu/KIK/data_en.html

Published
2019
Full Text
View/download PDF

11. The Type II-P Supernova 2017eaw: from explosion to the nebular phase

Author

Szalai, Tamás, Vinkó, József, Könyves-Tóth, Réka, Nagy, Andrea P., Bostroem, K. Azalee, Sárneczky, Krisztián, Brown, Peter J., Pejcha, Ondrej, Bódi, Attila, Cseh, Borbála, Csörnyei, Géza, Dencs, Zoltán, Hanyecz, Ottó, Ignácz, Bernadett, Kalup, Csilla, Kriskovics, Levente, Ordasi, András, Pál, András, Seli, Bálint, Sódor, Ádám, Szakáts, Róbert, Vida, Krisztián, Zsidi, Gabriella, Arcavi, Iair, Ashall, Chris, Burke, Jamison, Galbany, Lluís, Hiramatsu, Daichi, Hosseinzadeh, Griffin, Hsiao, Eric Y., Howell, D. Andrew, McCully, Curtis, Moran, Shane, Rho, Jeonghee, Sand, David J., Shahbandeh, Melissa, Valenti, Stefano, Wang, Xiaofeng, and Wheeler, J. Craig

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The nearby SN 2017eaw is a Type II-P (``plateau') supernova showing early-time, moderate CSM interaction. We present a comprehensive study of this SN including the analysis of high-quality optical photometry and spectroscopy covering the very early epochs up to the nebular phase, as well as near-UV and near-infrared spectra, and early-time X-ray and radio data. The combined data of SNe 2017eaw and 2004et allow us to get an improved distance to the host galaxy, NGC 6946, as $D \sim 6.85$ $\pm 0.63$ Mpc; this fits in recent independent results on the distance of the host and disfavors the previously derived (30% shorter) distances based on SN 2004et. From modeling the nebular spectra and the quasi-bolometric light curve, we estimate the progenitor mass and some basic physical parameters for the explosion and the ejecta. Our results agree well with previous reports on a RSG progenitor star with a mass of $\sim15-16$ M$_\odot$. Our estimation on the pre-explosion mass-loss rate ($\dot{M} \sim3 \times 10^{-7} -$ $1\times 10^{-6} M_{\odot}$ yr$^{-1}$) agrees well with previous results based on the opacity of the dust shell enshrouding the progenitor, but it is orders of magnitude lower than previous estimates based on general light-curve modeling of Type II-P SNe. Combining late-time optical and mid-infrared data, a clear excess at 4.5 $\mu$m can be seen, supporting the previous statements on the (moderate) dust formation in the vicinity of SN 2017eaw., Comment: 34 pages, 19 figures, 7 tables; accepted for publication in ApJ

Published
2019
Full Text
View/download PDF

13. Large amplitude change in spot-induced rotational modulation of the Kepler Ap star KIC 2569073

Author

Drury, Jason A., Murphy, Simon J., Derekas, Aliz, Sódor, Ádám, Stello, Dennis, Kuehn, Charles A., Bedding, Timothy R., Bognár, Zsófia, Szigeti, László, Szakáts, Róbert, Sárneczky, Krisztián, and Molnár, László

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

An investigation of the 200 $\times$ 200 pixel 'superstamp' images of the centres of the open clusters NGC 6791 and NGC 6819 allows for the identification and study of many variable stars that were not included in the Kepler target list. KIC 2569073 (V=14.22), is a particularly interesting variable Ap star that we discovered in the NGC 6791 superstamp. With a rotational period of 14.67 days and 0.034-mag variability, it has one of the largest peak-to-peak variations of any known Ap star. Colour photometry reveals an anti-phase correlation between the $B$ band, and the $V$, $R$ and $I$ bands. This Ap star is a rotational variable, also known as an $\alpha^2$ CVn, star, and is one of only a handful of Ap stars observed by Kepler. While no change in spot period or amplitude is observed within the 4-year Kepler timeseries, the amplitude shows a large increase compared to ground-based photometry obtained two decades ago., Comment: 8 pages, 7 figures, 3 tables, Accepted for publication to MNRAS

Published
2017
Full Text
View/download PDF

14. The SERMON project: 48 new field Blazhko stars and an investigation of modulation-period distribution

Author

Skarka, Marek, Liška, Jiří, Auer, Reinhold F., Prudil, Zdeněk, Juráňová, Anna, and Sódor, Ádam

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We investigated 1234 fundamental mode RR Lyrae stars observed by the All Sky Automated Survey (ASAS) to identify the Blazhko (BL) effect. A sample of 1547 BL stars from the literature was collected to compare the modulation-period distribution with stars newly identified in our sample. A classical frequency spectra analysis was performed using Period04 software. Data points from each star from the ASAS database were analysed individually to avoid confusion with artificial peaks and aliases. Statistical methods were used in the investigation of the modulation-period distribution. Altogether we identified 87 BL stars (48 new detections), 7 candidate stars, and 22 stars showing long-term period variations. The distribution of modulation periods of newly identified BL stars corresponds well to the distribution of modulation periods of stars located in the Galactic field, Galactic bulge, Large Magellanic Cloud, and globular cluster M5 collected from the literature. As a very important by-product of this comparison, we found that pulsation periods of BL stars follow Gaussian distribution with the mean period of $0.54\pm0.07$ d, while the modulation periods show log-normal distribution with centre at $\log(P_{\rm m}~{\rm [d]})=1.78\pm0.30$ dex. This means that 99.7 % of all known modulated stars have BL periods between 7.6 and 478 days. We discuss the identification of long modulation periods and show, that a significant percentage of stars showing long-term period variations could be classified as BL stars., Comment: 13 pages, 9 figures, Accepted for publication in Astronomy & Astrophysics

Published
2016
Full Text
View/download PDF

15. The diversity of light curve variations of Blazhko stars

Author

Sódor, Ádám

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The ground-based Konkoly Blazhko Survey I and II aim to collect accurate, extended, multicolour light curves of galactic field RRab stars in order to determine the incidence rate of the modulation in the sample, to study the modulation in details, to study long-term changes in the modulation properties and to find changes in the mean global physical parameters of the stars with Blazhko phase. Here the diversity of light curve variations of Blazhko stars is demonstrated through a sub-sample of the modulated RRab stars found by the first part of this survey., Comment: 4 pages, 2 figures. Published in AN (2010, AN, 331, P47). Proceeding a poster contribution at the 4th HELAS International Conference, Lanzarote, Spain, 1-5 February, 2010

Published
2011

16. On the distribution of the modulation frequencies of RR Lyrae stars

Author

Jurcsik, Johanna, Szeidl, Béla, Nagy, Andrea, and Sódor, Ádám

Subjects
Astrophysics
Abstract

For the first time connection between the pulsation and modulation properties of RR Lyrae stars has been detected. Based on the available data it is found that the possible range of the modulation frequencies, i.e, the possible maximum value of the modulation frequency depends on the pulsation frequency. Short period variables (P < 0.4 d) can have modulation period as short as some days, while longer period variables (P > 0.6 d) always exhibit modulation with P_mod > 20 d. We interpret this tendency with the equality of the modulation period with the surface rotation period, because similar distribution of the rotational periods is expected if an upper limit of the total angular momentum of stars leaving the RGB exists. The distribution of the projected rotational velocities of red and blue horizontal branch stars at different temperatures shows a similar behaviour as v_rot derived for RR Lyrae stars from their modulation periods. This common behaviour gives reason to identify the modulation period with the rotational period of the modulated RR Lyrae stars., Comment: 12 pages, 7 figures, 1 table. Accepted for publication in Acta Astronomica

Published
2005

18. Mid-infrared time-domain study of recent dust production events in the extreme debris disc of TYC 4209-1322-1

Author

Moór, Attila, primary, Ábrahám, Péter, additional, Kóspál, Ágnes, additional, Su, Kate Y L, additional, Rieke, George H, additional, Vida, Krisztián, additional, Cataldi, Gianni, additional, Bódi, Attila, additional, Bognár, Zsófia, additional, Cseh, Borbála, additional, Csörnyei, Géza, additional, Egei, Nóra, additional, Farkas, Anikó, additional, Hanyecz, Ottó, additional, Ignácz, Bernadett, additional, Kalup, Csilla, additional, Könyves-Tóth, Réka, additional, Kriskovics, Levente, additional, Mészáros, László, additional, Pál, András, additional, Ordasi, András, additional, Sárneczky, Krisztián, additional, Seli, Bálint, additional, Sódor, Ádám, additional, Szakáts, Róbert, additional, Vinkó, József, additional, and Zsidi, Gabriella, additional

Published
2022
Full Text
View/download PDF

19. SN 2018agk: A Prototypical Type Ia Supernova with a Smooth Power-law Rise in Kepler (K2)

Author

Wang, Qinan, primary, Rest, Armin, additional, Zenati, Yossef, additional, Ridden-Harper, Ryan, additional, Dimitriadis, Georgios, additional, Narayan, Gautham, additional, Villar, V. Ashley, additional, Magee, Mark R., additional, Foley, Ryan J., additional, Shaya, Edward J., additional, Garnavich, Peter, additional, Wang, Lifan, additional, Hu, Lei, additional, Bódi, Attila, additional, Armstrong, Patrick, additional, Auchettl, Katie, additional, Barclay, Thomas, additional, Barentsen, Geert, additional, Bognár, Zsófia, additional, Brimacombe, Joseph, additional, Bulger, Joanna, additional, Burke, Jamison, additional, Challis, Peter, additional, Chambers, Kenneth, additional, Coulter, David A., additional, Csörnyei, Géza, additional, Cseh, Borbála, additional, Deckers, Maxime, additional, Dotson, Jessie L., additional, Galbany, Lluís, additional, González-Gaitán, Santiago, additional, Gromadzki, Mariusz, additional, Gully-Santiago, Michael, additional, Hanyecz, Ottó, additional, Hedges, Christina, additional, Hiramatsu, Daichi, additional, Hosseinzadeh, Griffin, additional, Howell, D. Andrew, additional, Howell, Steve B., additional, Huber, Mark E., additional, Jha, Saurabh W., additional, Jones, David O., additional, Könyves-Tóth, Réka, additional, Kalup, Csilla, additional, Kilpatrick, Charles D., additional, Kriskovics, Levente, additional, Li, Wenxiong, additional, Lowe, Thomas B, additional, Margheim, Steven, additional, McCully, Curtis, additional, Mitra, Ayan, additional, Muñoz, Jose A., additional, Nicholl, Matt, additional, Nordin, Jakob, additional, Pál, András, additional, Pan, Yen-Chen, additional, Piro, Anthony L., additional, Rest, Sofia, additional, Rino-Silvestre, João, additional, Rojas-Bravo, César, additional, Sárneczky, Krisztián, additional, Siebert, Matthew R., additional, Smartt, Stephen J., additional, Smith, Ken, additional, Sódor, Ádám, additional, Stritzinger, Maximilian D., additional, Szabó, Róbert, additional, Szakáts, Róbert, additional, Tucker, Brad E., additional, Vinkó, József, additional, Wang, Xiaofeng, additional, Wheeler, J. Craig, additional, Young, David R., additional, Zenteno, Alfredo, additional, Zhang, KaiCheng, additional, and Zsidi, Gabriella, additional

Published
2021
Full Text
View/download PDF

20. A comprehensive look at RR Lyrae stars through high-precision photometry and astrometry

Author

Molnár, László, Bódi, Attila, Pál, András, Bhardwaj, Anupam, Hambsch, Franz-Josef, Benkő, József, Derekas, Aliz, Ebadi, Mohammad, Joyce, Meridith, Hasanzadeh, Amir, Kolenberg, Katrien, Lund, Michael B., Nemec, James N., Netzel, Henryka, Ngeow, Chow-Choong, Pepper, Joshua, Plachy, Emese, Prudil, Zdenek, Siverd, Robert J., Skarka, Marek, Smolec, Radek, Sódor, Ádám, Sylla, Salma, Szabó, Pál, Szabó, Róbert, Kjeldsen, Hans, Christensen-Dalsgaard, Jørgen, and Ricker, George R.

Subjects
stellar astrophysics, RR Lyrae variables, pulsating stars, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The TESS and Gaia missions are both collecting data of exquisite quality for RR Lyrae-type pulsating stars. We combine light curve shape information from TESS with distances and brightnesses from Gaia to build a detailed classification scheme that is able to filter out intrinsically fainter binaries and rotational variables as well as short-period Cepheids that otherwise have light curves very similar to that of RR Lyrae stars, while preserving targets with unusual light curve shapes. We build a clean sample from the RR Lyrae stars in the vicinity of the Sun, out to 5-10 kpc distances. Based on the TESS light curves we find that a large fraction of RR Lyrae stars exhibit various additional low-amplitude modes. The distribution of extra modes in period is markedly different from that of stars within the bulge and globular clusters, signaling a metallicity dependence in the mode periods and excitation mechanisms. We also detect a possible dependence of extra modes from color and hence effective temperatures in overtone RRc stars. While these new results have brought us closer to true asteroseismic analysis of RR Lyrae stars, we show through new échelle-type diagrams that mode identification is still hindered by the strong influence of the radial mode(s) dominating the pulsation., {"references":["Bovy, J., et al., 2016, ApJ, 818, 130","Gaia Collaboration, 2021, A&A, 649, 1","Jurcsik, J., et al., 2015, ApJS, 219, 25","Molnár, L., et al., 2017, EpJ WoC, 160, 04008","Netzel, H., et al., 2019, MNRAS, 487, 5584","Pál, A., 2012, MNRAS, 421, 1825","Smolec, R., et al., 2017, MNRAS, 467, 2349"]}

Published
2021
Full Text
View/download PDF

21. Extended Aperture Photometry of K2 RR Lyrae stars

Author

Plachy Emese, Klagyivik Péter, Molnár László, Sódor Ádám, and Szabó Róbert

Subjects
Physics, QC1-999
Abstract

We present the method of the Extended Aperture Photometry (EAP) that we applied on K2 RR Lyrae stars. Our aim is to minimize the instrumental variations of attitude control maneuvers by using apertures that cover the positional changes in the field of view thus contain the stars during the whole observation. We present example light curves that we compared to the light curves from the K2 Systematics Correction (K2SC) pipeline applied on the automated Single Aperture Photometry (SAP) and on the Pre-search Data Conditioning Simple Aperture Photometry (PDCSAP) data.

Published
2017
Full Text
View/download PDF

22. KIC 2831097 A short orbital-period candidate RR Lyrae binary

Author

Sódor Ádám, Skarka Marek, Liška Jir̆í, and Bognár Zsófia

Subjects
Physics, QC1-999
Abstract

KIC 2831097 was discovered to be a first-overtone RR Lyrae pulsator based on 4-year Kepler photometry (Sódor et al. 2017, MNRAS, 465, L1). The data show strong, 0.1 d amplitude systematic phase variations that can be explained by light travel-time effect caused by an about 2-year period orbital motion in a binary system, superimposed on a linear pulsation-period decrease. To verify the binary hypothesis, several well-timed radial-velocity observations will be sufficient.

Published
2017
Full Text
View/download PDF

23. Dipper-like variability of the Gaia alerted young star V555 Ori

Author

Nagy, Zsófia, primary, Szegedi-Elek, Elza, additional, Ábrahám, Péter, additional, Kóspál, Ágnes, additional, Bódi, Attila, additional, Bouvier, Jérôme, additional, Kun, Mária, additional, Moór, Attila, additional, Cseh, Borbála, additional, Farkas-Takács, Anikó, additional, Hanyecz, Ottó, additional, Hodgkin, Simon, additional, Ignácz, Bernadett, additional, Kiss, Csaba, additional, Könyves-Tóth, Réka, additional, Kriskovics, Levente, additional, Marton, Gábor, additional, Mészáros, László, additional, Ordasi, András, additional, Pál, András, additional, Sarkis, Paula, additional, Sárneczky, Krisztián, additional, Sódor, Ádám, additional, Szabados, László, additional, Szabó, Zsófia Marianna, additional, Szakáts, Róbert, additional, Tarczay-Nehéz, Dóra, additional, Vida, Krisztián, additional, and Zsidi, Gabriella, additional

Published
2021
Full Text
View/download PDF

24. Ejecta Masses in Type Ia Supernovae—Implications for the Progenitor and the Explosion Scenario**Based in part on observations obtained with the Hobby-Eberly Telescope (HET), which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximillians-Universitaet Muenchen, and Georg-August Universitaet Goettingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly.

Author

Bora, Zsófia, Könyves-Tóth, Réka, Vinkó, József, Bánhidi, Dominik, Bíró, Imre Barna, Bostroem, K. Azalee, Bódi, Attila, Burke, Jamison, Csányi, István, Cseh, Borbála, Farah, Joseph, Filippenko, Alexei V., Hegedüs, Tibor, Hiramatsu, Daichi, Horti-Dávid, Ágoston, Howell, D. Andrew, Jha, Saurabh W., Kalup, Csilla, Krezinger, Máté, Kriskovics, Levente, McCully, Curtis, Newsome, Megan, Ordasi, András, Gonzalez, Estefania Padilla, Pál, András, Pellegrino, Craig, Seli, Bálint, Sódor, Ádám, Szabó, Zsófia Marianna, Szabó, Olivér Norton, Szakáts, Róbert, Szalai, Tamás, Székely, Péter, Terreran, Giacomo, Varga, Vázsony, Vida, Krisztián, Wang, Xiaofeng, and Wheeler, J. Craig

Abstract

The progenitor system(s) as well as the explosion mechanism(s) of thermonuclear (Type Ia) supernovae are long-standing issues in astrophysics. Here we present ejecta masses and other physical parameters for 28 recent Type Ia supernovae inferred from multiband photometric and optical spectroscopic data. Our results confirm that the majority of SNe Ia show observableejecta masses below the Chandrasekhar-limit (having a mean Mej≈ 1.1 ± 0.3 M⊙), consistent with the predictions of recent sub-MChexplosion models. They are compatible with models assuming either single- or double-degenerate progenitor configurations. We also recover a sub-sample of supernovae within 1.2 M⊙< Mej< 1.5 M⊙that are consistent with near-Chandrasekhar explosions. Taking into account the uncertainties of the inferred ejecta masses, about half of our SNe are compatible with both explosion models. We compare our results with those in previous studies, and discuss the caveats and concerns regarding the applied methodology.

Published
2024
Full Text
View/download PDF

26. Extended Aperture Photometry of K2 RR Lyrae stars

Author

Plachy, Emese, primary, Molnár, László, additional, Bódi, Attila, additional, Skarka, Marek, additional, Szabó, Pál, additional, Szabó, Róbert, additional, Klagyivik, Péter, additional, Sódor, Ádám, additional, and Pope, Benjamin J. S., additional

Published
2019
Full Text
View/download PDF

27. Spectroscopic monitoring of bright A-F type candidate hybrid stars discovered by the Kepler mission

Author

De Cat, Peter, Lampens, Patricia, Frémat, Yves, Vermeylen, Lore, Dumortier, Louis, Sódor, Ádám, Skarka, Marek, and Bognár, Zsófia

Subjects
stars, Physics, spectroscopy, Multidisciplinary, astrophysics, variability, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Kepler, spectroscopie, astronomy, étoiles, Stars, variabilité, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, astronomie, Spectroscopy, Astrophysics::Galaxy Astrophysics, astrophysique
Abstract

We report on a study of 250 optical spectra for 50 bright A/F-type candidate hybrid pulsating stars from the Kepler field. Most of the spectra have been collected with the high-resolution spectrograph HERMES attached to the Mercator telescope, La Palma. We determined the radial velocities (RVs), projected rotational velocities, fundamental atmospheric parameters and provide a classification based on the appearance of the cross-correlation profiles and the behaviour of the RVs with time in order to find true hybrid pulsators. Additionally, we also detected new spectroscopic binary and multiple systems in our sample and determined the fraction of spectroscopic systems. In order to be able to extend this investigation to the fainter A-F type candidate hybrid stars, various high-quality spectra collected with 3–4 m sized telescopes suitably equipped with a high-resolution spectrograph and furthermore located in the Northern hemisphere would be ideal. This programme could be done using the new instruments installed at the Devasthal Observatory.

Published
2018
Full Text
View/download PDF

28. Spectroscopic and photometric time series of the bright RRc star T Sex.

Author

Benkő, József M, Sódor, Ádám, and Pál, András

Subjects
*RR Lyrae stars, *TIME series analysis, *PULSATING stars, *STELLAR oscillations, *STELLAR atmospheres, *SPACE telescopes
Abstract

We present spectroscopic time series observations on one of the brightest northern RRc stars, namely T Sex. Additionally, we also analysed extended photometric data sets, particularly the recent observations of the TESS space telescope. The main findings of our studies are as follows: T Sex, unlike all RRc stars whose space photometry has been analysed, shows only the 0.5 fx frequency as an additional pulsation frequency. With this, T Sex may be the first represent of such rare RRc stars found from space photometry. The spectroscopic data show a periodic distortion of the H α line with the pulsation phase. This phenomenon has not been reported for any RR Lyrae stars. The characteristic line distortion is probably caused by the turbulent convection, which resulted in higher macroturbulent velocity for T Sex than that for typical RRab stars. Line doubling of the Na D line was observed between the 0.37 and 0.80 pulsation phases. The explanation of this phenomenon is that the two absorption components originate from different sources. The redder component comes from the pulsating atmosphere of the star, while the bluer one comes from the interstellar space. At phase 0.438, we detected emission on the Na D line, which may indicate a weak shock wave. [ABSTRACT FROM AUTHOR]

Published
2021
Full Text
View/download PDF

30. Large amplitude change in spot-induced rotational modulation of the Kepler Ap star KIC 2569073

Author

Drury, Jason A., primary, Murphy, Simon J., additional, Derekas, Aliz, additional, Sódor, Ádám, additional, Stello, Dennis, additional, Kuehn, Charles A., additional, Bedding, Timothy R., additional, Bognár, Zsófia, additional, Szigeti, László, additional, Szakáts, Róbert, additional, Sárneczky, Krisztián, additional, and Molnár, László, additional

Published
2017
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results