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pro vyhledávání: '"Ercolino, Andrea"'
Autor:
Ercolino, Andrea
The light curves and spectra of many Type I and Type II supernovae (SNe) are heavily influenced by the interaction of the SN ejecta with circumstellar material (CSM) surrounding the progenitor star. The observed diversity shows that many progenitors
Externí odkaz:
http://arxiv.org/abs/2410.16742
Publikováno v:
A&A 685, A169 (2024)
Over the last decade, evidence has accumulated that massive stars do not typically evolve in isolation but instead follow a tumultuous journey with a companion star on their way to core collapse. While Roche-lobe overflow appears instrumental for the
Externí odkaz:
http://arxiv.org/abs/2402.12977
Autor:
Menon, Athira, Ercolino, Andrea, Urbaneja, Miguel A., Lennon, Daniel J., Herrero, Artemio, Hirai, Ryosuke, Langer, Norbert, Schootemeijer, Abel, Chatzopoulos, Emmanouil, Frank, Juhan, Shiber, Sagiv
Blue supergiants are the brightest stars in their host galaxies and yet their evolutionary status has been a long-standing problem in stellar astrophysics. In this pioneering work, we present a large sample of 59 early B-type supergiants in the Large
Externí odkaz:
http://arxiv.org/abs/2311.05581
Many supernovae (SNe) imply an interaction of the SN ejecta with matter (CSM) surrounding the progenitor star. This suggests that many massive stars may undergo various degrees of envelope stripping shortly before exploding, and produce a considerabl
Externí odkaz:
http://arxiv.org/abs/2308.01819
Autor:
Jenkins, James S., Díaz, Matías R., Kurtovic, Nicolás T., Espinoza, Néstor, Vines, Jose I., Rojas, Pablo A. Peña, Brahm, Rafael, Torres, Pascal, Cortés-Zuleta, Pía, Soto, Maritza G., Lopez, Eric D., King, George W., Wheatley, Peter J., Winn, Joshua N., Ciardi, David R., Ricker, George, Vanderspek, Roland, Latham, David W., Seager, Sara, Jenkins, Jon M., Beichman, Charles A., Bieryla, Allyson, Burke, Christopher J., Christiansen, Jessie L., Henze, Christopher E., Klaus, Todd C., McCauliff, Sean, Mori, Mayuko, Narita, Norio, Nishiumi, Taku, Tamura, Motohide, de Leon, Jerome Pitogo, Quinn, Samuel N., Villaseñor, Jesus Noel, Vezie, Michael, Lissauer, Jack J., Collins, Karen A., Collins, Kevin I., Isopi, Giovanni, Mallia, Franco, Ercolino, Andrea, Petrovich, Cristobal, Jordán, Andrés, Acton, Jack S., Armstrong, David J., Bayliss, Daniel, Bouchy, François, Belardi, Claudia, Bryant, Edward M., Burleigh, Matthew R., Cabrera, Juan, Casewell, Sarah L., Chaushev, Alexander, Cooke, Benjamin F., Eigmüller, Philipp, Erikson, Anders, Foxell, Emma, Gänsicke, Boris T., Gill, Samuel, Gillen, Edward, Günther, Maximilian N., Goad, Michael R., Hooton, Matthew J., Jackman, James A. G., Louden, Tom, McCormac, James, Moyano, Maximiliano, Nielsen, Louise D., Pollacco, Don, Queloz, Didier, Rauer, Heike, Raynard, Liam, Smith, Alexis M. S., Tilbrook, Rosanna H., Titz-Weider, Ruth, Turner, Oliver, Udry, Stéphane, Walker, Simon. R., Watson, Christopher A., West, Richard G., Palle, Enric, Ziegler, Carl, Law, Nicholas, Mann, Andrew W.
About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters,
Externí odkaz:
http://arxiv.org/abs/2009.12832
Autor:
Cloutier, Ryan, Rodriguez, Joseph E., Irwin, Jonathan, Charbonneau, David, Stassun, Keivan G., Mortier, Annelies, Latham, David W., Isaacson, Howard, Howard, Andrew W., Udry, Stéphane, Wilson, Thomas G., Watson, Christopher A., Pinamonti, Matteo, Lienhard, Florian, Giacobbe, Paolo, Guerra, Pere, Collins, Karen A., Beiryla, Allyson, Esquerdo, Gilbert A., Matthews, Elisabeth, Matson, Rachel A., Howell, Steve B., Furlan, Elise, Crossfield, Ian J. M., Winters, Jennifer G., Nava, Chantanelle, Ment, Kristo, Lopez, Eric D., Ricker, George, Vanderspek, Roland, Seager, Sara, Jenkins, Jon M., Ting, Eric B., Tenenbaum, Peter, Sozzetti, Alessandro, Sha, Lizhou, Ségransan, Damien, Schlieder, Joshua E., Sasselov, Dimitar, Roy, Arpita, Robertson, Paul, Rice, Ken, Poretti, Ennio, Piotto, Giampaolo, Phillips, David, Pepper, Joshua, Pepe, Francesco, Molinari, Emilio, Mocnik, Teo, Micela, Giuseppina, Mayor, Michel, Fiorenzano, Aldo F. Martinez, Mallia, Franco, Lubin, Jack, Lovis, Christophe, López-Morales, Mercedes, Kosiarek, Molly R., Kielkopf, John F., Kane, Stephen R., Jensen, Eric L. N., Isopi, Giovanni, Huber, Daniel, Hill, Michelle L., Harutyunyan, Avet, Gonzales, Erica, Giacalone, Steven, Ghedina, Adriano, Ercolino, Andrea, Dumusque, Xavier, Dressing, Courtney D., Damasso, Mario, Dalba, Paul A., Cosentino, Rosario, Conti, Dennis M., Colón, Knicole D., Collins, Kevin I., Cameron, Andrew Collier, Ciardi, David, Christiansen, Jessie, Chontos, Ashley, Cecconi, Massimo, Caldwell, Douglas A., Burke, Christopher, Buchhave, Lars, Beichman, Charles, Behmard, Aida, Beard, Corey, Murphy, Joseph M. Akana
Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally-driven atmospheric mass loss and of terrestrial planet formatio
Externí odkaz:
http://arxiv.org/abs/2004.06682
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Publikováno v:
Astronomy & Astrophysics / Astronomie et Astrophysique; 5/3/2024, Vol. 685, p1-22, 22p
Akademický článek
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