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218 results on '"Vazan, A."'

3. The Distribution of Planet Radius in Kepler Multiplanet Systems Depends on Gap Complexity

Author

David R. Rice, Jason H. Steffen, and Allona Vazan

Subjects
Exoplanets, Exoplanet systems, Planetary system formation, Astrophysics, QB460-466
Abstract

The distribution of small planet radius ( 0.35) exhibit a lower frequency of sub-Earths (2.5 times less) and sub-Neptunes (1.3 times less) and a higher frequency of super-Earths (1.4 times more) than planets in low-complexity systems. This may suggest that planetary systems with more irregular spacings are more likely to undergo dynamic interactions that influence planet scattering, composition, and atmospheric retention. The gap complexity metric proves to be a valuable tool in linking the orbital configurations of planets to their physical characteristics.

Published
2024
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7. Magnesium oxide-water compounds at megabar pressure and implications on planetary interiors

Author

Shuning Pan, Tianheng Huang, Allona Vazan, Zhixin Liang, Cong Liu, Junjie Wang, Chris J. Pickard, Hui-Tian Wang, Dingyu Xing, and Jian Sun

Subjects
Science
Abstract

Magnesium Oxide and water are abundant in the interior of planets. Here, the authors predict three new MgO-H2O compounds: Mg2O3H2, MgO3H4 and MgO4H6, and they exhibit superionic behavior in planetary interior conditions.

Published
2023
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10. Ariel planetary interiors White Paper

Author

Helled, Ravit, Werner, Stephanie, Dorn, Caroline, Guillot, Tristan, Ikoma, Masahiro, Ito, Yuichi, Kama, Mihkel, Lichtenberg, Tim, Miguel, Yamila, Shorttle, Oliver, Tackley, Paul J., Valencia, Diana, and Vazan, Allona

Published
2022
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11. Exploring the link between star and planet formation with Ariel

Author

Turrini, Diego, Codella, Claudio, Danielski, Camilla, Fedele, Davide, Fonte, Sergio, Garufi, Antonio, Guarcello, Mario Giuseppe, Helled, Ravit, Ikoma, Masahiro, Kama, Mihkel, Kimura, Tadahiro, Kruijssen, J. M. Diederik, Maldonado, Jesus, Miguel, Yamila, Molinari, Sergio, Nikolaou, Athanasia, Oliva, Fabrizio, Panić, Olja, Pignatari, Marco, Podio, Linda, Rickman, Hans, Schisano, Eugenio, Shibata, Sho, Vazan, Allona, and Wolkenberg, Paulina

Published
2022
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12. How planets grow by pebble accretion: V. Silicate rainout delays the contraction of sub-Neptunes.

Author

Vazan, Allona, Ormel, Chris W., and Brouwers, Marc G.

Subjects
*NATURAL satellite atmospheres, *NATURAL satellites, *PLANETARY atmospheres, *PLANETARY interiors, *PLANETS, *PROTOPLANETARY disks
Abstract

The characterization of super-Earth- to Neptune-sized exoplanets relies heavily on our understanding of their formation and evolution. In this study, we link a model of planet formation by pebble accretion to the planets' long-term observational properties by calculating the interior evolution, starting from the dissipation of the protoplanetary disk. We investigate the evolution of the interior structure in 5–20 M⊕ planets, accounting for silicate redistribution caused by convective mixing, rainout (condensation and settling), and mass loss. Specifically, we have followed the fate of the hot silicate vapor that remained in the planet's envelope after planet formation as the planet cools. We find that disk dissipation is followed by a rapid contraction of the envelope from the Hill or Bondi radius to about one-tenth of that size within 10 Myr. Subsequent cooling leads to substantial growth of the planetary core through silicate rainout accompanied by inflated radii, in comparison to the standard models of planets that formed with core-envelope structure. We examined the dependence of rainout on the planet's envelope mass, on the distance from its host star, on its silicate mass, and on the atmospheric opacity. We find that the population of planets that formed with polluted envelopes can be roughly divided into three groups based on the mass of their gas envelopes: bare rocky cores that have shed their envelopes, super-Earth planets with a core-envelope structure, and Neptune-like planets with diluted cores that undergo gradual rainout. For polluted planets that formed with envelope masses below 0.4 M⊕, we anticipate that the inflation of the planet's radius caused by rainout will enhance the mass loss by a factor of 2–8 compared to planets with unpolluted envelopes. Our model bridges the gap between the predicted composition gradients in massive planets and the core-envelope structure in smaller planets. [ABSTRACT FROM AUTHOR]

Published
2024
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13. A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images

Author

Tianjun Gan, Charles Cadieux, Farbod Jahandar, Allona Vazan, Sharon X. Wang, Shude Mao, Jaime A. Alvarado-Montes, D. N. C. Lin, Étienne Artigau, Neil J. Cook, René Doyon, Andrew W. Mann, Keivan G. Stassun, Adam J. Burgasser, Benjamin V. Rackham, Steve B. Howell, Karen A. Collins, Khalid Barkaoui, Avi Shporer, Jerome de Leon, Luc Arnold, George R. Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Artem Burdanov, David Charbonneau, Georgina Dransfield, Akihiko Fukui, Elise Furlan, Michaël Gillon, Matthew J. Hooton, Hannah M. Lewis, Colin Littlefield, Ismael Mireles, Norio Narita, Chris W. Ormel, Samuel N. Quinn, Ramotholo Sefako, Mathilde Timmermans, Michael Vezie, and Julien de Wit

Subjects
M dwarf stars, Radial velocity, Photometry, M stars, Extrasolar gaseous planets, Astronomy, QB1-991
Abstract

Observations and statistical studies have shown that giant planets are rare around M dwarfs compared with Sun-like stars. The formation mechanism of these extreme systems has remained under debate for decades. With the help of the TESS mission and ground-based follow-up observations, we report the discovery of TOI-4201b, the most massive and densest hot Jupiter around an M dwarf known so far with a radius of 1.22 ± 0.04 R _J and a mass of 2.48 ± 0.09 M _J , about 5 times heavier than most other giant planets around M dwarfs. It also has the highest planet-to-star mass ratio ( q ∼ 4 × 10 ^−3 ) among such systems. The host star is an early M dwarf with a mass of 0.61 ± 0.02 M _⊙ and a radius of 0.63 ± 0.02 R _⊙ . It has significant supersolar iron abundance ([Fe/H] = 0.52 ± 0.08 dex). However, interior structure modeling suggests that its planet TOI-4201b is metal-poor, which challenges the classical core-accretion correlation of stellar−planet metallicity, unless the planet is inflated by additional energy sources. Building on the detection of this planet, we compare the stellar metallicity distribution of four planetary groups: hot/warm Jupiters around G/M dwarfs. We find that hot/warm Jupiters show a similar metallicity dependence around G-type stars. For M-dwarf host stars, the occurrence of hot Jupiters shows a much stronger correlation with iron abundance, while warm Jupiters display a weaker preference, indicating possible different formation histories.

Published
2023
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14. Interior and Evolution of the Giant Planets

Author

Yamila Miguel and Allona Vazan

Subjects
giant planets interiors, giant planets evolution, planet formation, Science
Abstract

The giant planets were the first to form and hold the key to unveiling the solar system’s formation history in their interiors and atmospheres. Furthermore, the unique conditions present in the interiors of the giant planets make them natural laboratories for exploring different elements under extreme conditions. We are at a unique time to study these planets. The missions Juno to Jupiter and Cassini to Saturn have provided invaluable information to reveal their interiors like never before, including extremely accurate gravity data, atmospheric abundances and magnetic field measurements that revolutionised our knowledge of their interior structures. At the same time, new laboratory experiments and modelling efforts also improved, and statistical analysis of these planets is now possible to explore all the different conditions that shape their interiors. We review the interior structure of Jupiter, Saturn, Uranus and Neptune, including the need for inhomogeneous structures to explain the data, the problems unsolved and the effect that advances in our understanding of their internal structure have on their formation and evolution.

Published
2023
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17. Performance of Prognostic Risk Scores in Chronic Heart Failure Patients Enrolled in the European Society of Cardiology Heart Failure Long-Term Registry

Author

Crespo-Leiro, M., Anker, S., Mebazaa, A., Coats, A., Filippatos, G., Ferrari, R., Maggioni, A.P., Piepoli, M.F., Amir, O., Chioncel, O., Dahlström, U., Delgado Jimenez, J.F., Drozdz, J., Erglis, A., Fazlibegovic, E., Fonseca, C., Fruhwald, F., Gatzov, P., Goncalvesova, E., Hassanein, M., Hradec, J., Kavoliuniene, A., Lainscak, M., Logeart, D., Merkely, B., Metra, M., Otljanska, M., Seferovic, P.M., Srbinovska Kostovska, E., Temizhan, A., Tousoulis, D., Ferreira, T., Andarala, M., Fiorucci, E., Folkesson Lefrancq, E., Glémot, M., Gracia, G., Konte, M., Laroche, C., McNeill, P.A., Missiamenou, V., Taylor, C., Auer, J., Ablasser, K., Dolze, T., Brandner, K., Gstrein, S., Poelzl, G., Moertl, D., Reiter, S., Podczeck-Schweighofer, A., Muslibegovic, A., Vasilj, M., Cesko, M., Zelenika, D., Palic, B., Pravdic, D., Cuk, D., Vitlianova, K., Katova, T., Velikov, T., Kurteva, T., Kamenova, D., Antova, M., Sirakova, V., Krejci, J., Mikolaskova, M., Spinar, J., Krupicka, J., Malek, F., Hegarova, M., Lazarova, M., Monhart, Z., Sobhy, M., El Messiry, F., El Shazly, A.H., Elrakshy, Y., Youssef, A., Moneim, A.A., Noamany, M., Reda, A., Abdel Dayem, T.K., Farag, N., Ibrahim Halawa, S., Abdel Hamid, M., Said, K., Saleh, A., Ebeid, H., Hanna, R., Aziz, R., Louis, O., Enen, M.A., Ibrahim, B.S., Nasr, G., Elbahry, A., Sobhy, H., Ashmawy, M., Gouda, M., Aboleineen, W., Bernard, Y., Luporsi, P., Meneveau, N., Pillot, M., Morel, M., Seronde, M.-F., Schiele, F., Briand, F., Delahaye, F., Damy, T., Eicher, J.-C., de Groote, P., Fertin, M., Lamblin, N., Isnard, R., Lefol, C., Thevenin, S., Hagege, A., Jondeau, G., Le Marcis, V., Ly, J.-F., Coisne, D., Lequeux, B., Le Moal, V., Mascle, S., Lotton, P., Behar, N., Donal, E., Thebault, C., Ridard, C., Reynaud, A., Basquin, A., Bauer, F., Codjia, R., Galinier, M., Tourikis, P., Stavroula, M., Stefanadis, C., Chrysohoou, C., Kotrogiannis, I., Matzaraki, V., Dimitroula, T., Karavidas, A., Tsitsinakis, G., Kapelios, C., Nanas, J., Kampouri, H., Nana, E., Kaldara, E., Eugenidou, A., Vardas, P., Saloustros, I., Patrianakos, A., Tsaknakis, T., Evangelou, S., Nikoloulis, N., Tziourganou, H., Tsaroucha, A., Papadopoulou, A., Douras, A., Polgar, L., Kosztin, A., Nyolczas, N., Csaba Nagy, A., Halmosi, R., Elber, J., Alony, I., Shotan, A., Vazan Fuhrmann, A., Romano, S., Marcon, S., Penco, M., Di Mauro, M., Lemme, E., Carubelli, V., Rovetta, R., Bulgari, M., Quinzani, F., Lombardi, C., Bosi, S., Schiavina, G., Squeri, A., Barbieri, A., Di Tano, G., Pirelli, S., Fucili, A., Passero, T., Musio, S., Di Biase, M., Correale, M., Salvemini, G., Brognoli, S., Zanelli, E., Giordano, A., Agostoni, P., Italiano, G., Salvioni, E., Copelli, S., Modena, M.G., Reggianini, L., Valenti, C., Olaru, A., Bandino, S., Deidda, M., Mercuro, G., Cadeddu Dessalvi, C., Marino, P.N., Di Ruocco, M.V., Sartori, C., Piccinino, C., Parrinello, G., Licata, G., Torres, D., Giambanco, S., Busalacchi, S., Arrotti, S., Novo, S., Inciardi, R.M., Pieri, P., Chirco, P.R., Ausilia Galifi, M., Teresi, G., Buccheri, D., Minacapelli, A., Veniani, M., Frisinghelli, A., Priori, S.G., Cattaneo, S., Opasich, C., Gualco, A., Pagliaro, M., Mancone, M., Fedele, F., Cinque, A., Vellini, M., Scarfo, I., Romeo, F., Ferraiuolo, F., Sergi, D., Anselmi, M., Melandri, F., Leci, E., Iori, E., Bovolo, V., Pidello, S., Frea, S., Bergerone, S., Botta, M., Canavosio, F.G., Gaita, F., Merlo, M., Cinquetti, M., Sinagra, G., Ramani, F., Fabris, E., Stolfo, D., Artico, J., Miani, D., Fresco, C., Daneluzzi, C., Proclemer, A., Cicoira, M., Zanolla, L., Marchese, G., Torelli, F., Vassanelli, C., Voronina, N., Tamakauskas, V., Smalinskas, V., Karaliute, R., Petraskiene, I., Kazakauskaite, E., Rumbinaite, E., Vysniauskas, V., Brazyte-Ramanauskiene, R., Petraskiene, D., Stankala, S., Switala, P., Juszczyk, Z., Sinkiewicz, W., Gilewski, W., Pietrzak, J., Orzel, T., Kasztelowicz, P., Kardaszewicz, P., Lazorko-Piega, M., Gabryel, J., Mosakowska, K., Bellwon, J., Rynkiewicz, A., Raczak, G., Lewicka, E., Dabrowska-Kugacka, A., Bartkowiak, R., Sosnowska-Pasiarska, B., Wozakowska-Kaplon, B., Krzeminski, A., Zabojszcz, M., Mirek-Bryniarska, E., Grzegorzko, A., Bury, K., Nessler, J., Zalewski, J., Furman, A., Broncel, M., Poliwczak, A., Bala, A., Zycinski, P., Rudzinska, M., Jankowski, L., Kasprzak, J.D., Michalak, L., Wojtczak Soska, K., Huziuk, I., Retwinski, A., Flis, P., Weglarz, J., Bodys, A., Grajek, S., Kaluzna-Oleksy, M., Straburzynska-Migaj, E., Dankowski, R., Szymanowska, K., Grabia, J., Szyszka, A., Nowicka, A., Samcik, M., Wolniewicz, L., Baczynska, K., Komorowska, K., Poprawa, I., Komorowska, E., Sajnaga, D., Zolbach, A., Dudzik-Plocica, A., Abdulkarim, A.-F., Lauko-Rachocka, A., Kaminski, L., Kostka, A., Cichy, A., Ruszkowski, P., Splawski, M., Fitas, G., Szymczyk, A., Serwicka, A., Fiega, A., Zysko, D., Krysiak, W., Szabowski, S., Skorek, E., Pruszczyk, P., Bienias, P., Ciurzynski, M., Welnicki, M., Mamcarz, A., Folga, A., Zielinski, T., Rywik, T., Leszek, P., Sobieszczanska-Malek, M., Piotrowska, M., Kozar-Kaminska, K., Komuda, K., Wisniewska, J., Tarnowska, A., Balsam, P., Marchel, M., Opolski, G., Kaplon-Cieslicka, A., Gil, R.J., Mozenska, O., Byczkowska, K., Gil, K., Pawlak, A., Michalek, A., Krzesinski, P., Piotrowicz, K., Uzieblo-Zyczkowska, B., Stanczyk, A., Skrobowski, A., Ponikowski, P., Jankowska, E., Rozentryt, P., Polonski, L., Gadula-Gacek, E., Nowalany-Kozielska, E., Kuczaj, A., Kalarus, Z., Szulik, M., Przybylska, K., Klys, J., Prokop-Lewicka, G., Kleinrok, A., Tavares Aguiar, C., Ventosa, A., Pereira, S., Faria, R., Chin, J., De Jesus, I., Santos, R., Silva, P., Moreno, N., Queirós, C., Lourenço, C., Pereira, A., Castro, A., Andrade, A., Oliveira Guimaraes, T., Martins, S., Placido, R., Lima, G., Brito, D., Francisco, A.R., Cardiga, R., Proenca, M., Araujo, I., Marques, F., Moura, B., Leite, S., Campelo, M., Silva-Cardoso, J., Rodrigues, J., Rangel, I., Martins, E., Sofia Correia, A., Peres, M., Marta, L., Ferreira da Silva, G., Severino, D., Durao, D., Leao, S., Magalhaes, P., Moreira, I., Filipa Cordeiro, A., Ferreira, C., Araujo, C., Ferreira, A., Baptista, A., Radoi, M., Bicescu, G., Vinereanu, D., Sinescu, C.-J., Macarie, C., Popescu, R., Daha, I., Dan, G.-A., Stanescu, C., Dan, A., Craiu, E., Nechita, E., Aursulesei, V., Christodorescu, R., Otasevic, P., Simeunovic, D., Ristic, A.D., Celic, V., Pavlovic-Kleut, M., Suzic Lazic, J., Stojcevski, B., Pencic, B., Stevanovic, A., Andric, A., Iric-Cupic, V., Jovic, M., Davidovic, G., Milanov, S., Mitic, V., Atanaskovic, V., Antic, S., Pavlovic, M., Stanojevic, D., Stoickov, V., Ilic, S., Deljanin Ilic, M., Petrovic, D., Stojsic, S., Kecojevic, S., Dodic, S., Cemerlic Adic, N., Cankovic, M., Stojiljkovic, J., Mihajlovic, B., Radin, A., Radovanovic, S., Krotin, M., Klabnik, A., Pernicky, M., Murin, J., Kovar, F., Kmec, J., Semjanova, H., Strasek, M., Savnik Iskra, M., Ravnikar, T., Cernic Suligoj, N., Komel, J., Fras, Z., Jug, B., Glavic, T., Losic, R., Bombek, M., Krajnc, I., Krunic, B., Horvat, S., Kovac, D., Rajtman, D., Cencic, V., Letonja, M., Winkler, R., Valentincic, M., Melihen-Bartolic, C., Bartolic, A., Pusnik Vrckovnik, M., Kladnik, M., Slemenik Pusnik, C., Marolt, A., Klen, J., Drnovsek, B., Leskovar, B., Fernandez Anguita, M.J., Gallego Page, J.C., Salmeron Martinez, F.M., Andres, J., Genis, A.B., Mirabet, S., Mendez, A., Garcia-Cosio, L., Roig, E., Leon, V., Gonzalez-Costello, J., Muntane, G., Garay, A., Alcade-Martinez, V., Lopez Fernandez, S., Rivera-Lopez, R., Puga-Martinez, M., Fernandez-Alvarez, M., Serrano-Martinez, J.L., Grille-Cancela, Z., Marzoa-Rivas, R., Blanco-Canosa, P., Paniagua-Martin, M.J., Barge-Caballero, E., Laynez Cerdena, I., Famara Hernandez Baldomero, I., Lara Padron, A., Ofelia Rosillo, S., Dalmau Gonzalez-Gallarza, R., Salvador Montanes, O., Iniesta Manjavacas, A.M., Castro Conde, A., Araujo, A., Soria, T., Garcia-Pavia, P., Gomez-Bueno, M., Cobo-Marcos, M., Alonso-Pulpon, L., Segovia Cubero, J., Sayago, I., Gonzalez-Segovia, A., Briceno, A., Escribano Subias, P., Vicente Hernandez, M., Ruiz Cano, M.J., Gomez Sanchez, M.A., Barrios Garrido-Lestache, E., Garcia Pinilla, J.M., Garcia de la Villa, B., Sahuquillo, A., Bravo Marques, R., Torres Calvo, F., Perez-Martinez, M.T., Gracia-Rodenas, M.R., Garrido-Bravo, I.P., Pastor-Perez, F., Pascual-Figal, D.A., Diaz Molina, B., Orus, J., Epelde Gonzalo, F., Bertomeu, V., Valero, R., Martinez-Abellan, R., Quiles, J., Rodrigez-Ortega, J.A., Mateo, I., ElAmrani, A., Fernandez-Vivancos, C., Bierge Valero, D., Almenar-Bonet, L., Sanchez-Lazaro, I.J., Marques-Sule, E., Facila-Rubio, L., Perez-Silvestre, J., Garcia-Gonzalez, P., Ridocci-Soriano, F., Garcia-Escriva, D., Pellicer-Cabo, A., de la Fuente Galan, L., Lopez Diaz, J., Recio Platero, A., Arias, J.C., Blasco-Peiro, T., Sanz Julve, M., Sanchez-Insa, E., Aured-Guallar, C., Portoles-Ocampo, A., Melin, M., Hägglund, E., Stenberg, A., Lindahl, I.-M., Asserlund, B., Olsson, L., Afzelius, M., Karlström, P., Tengvall, L., Wiklund, P.-A., Olsson, B., Kalayci, S., Cavusoglu, Y., Gencer, E., Yilmaz, M.B., Gunes, H., Canepa, Marco, Fonseca, Candida, Chioncel, Ovidiu, Laroche, Cécile, Crespo-Leiro, Maria G., Coats, Andrew J.S., Mebazaa, Alexandre, Piepoli, Massimo F., Tavazzi, Luigi, and Maggioni, Aldo P.

Published
2018
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18. A massive hot Jupiter orbiting a metal-rich early-M star discovered in the TESS full frame images

Author

Gan, Tianjun, Cadieux, Charles, Jahandar, Farbod, Vazan, Allona, Wang, Sharon X., Mao, Shude, Lin, D. N. C., Artigau, Étienne, Cook, Neil J., Doyon, René, Mann, Andrew W., Stassun, Keivan G., Howell, Steve B., Collins, Karen A., Barkaoui, Khalid, Shporer, Avi, de Leon, Jerome, Arnold, Luc, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Burdanov, Artem, Charbonneau, David, Dransfield, Georgina, Fukui, Akihiko, Furlan, Elise, Gillon, Michaël, Hooton, Matthew J., Lewis, Hannah M., Littlefield, Colin, Mireles, Ismael, Narita, Norio, Ormel, Chris W., Quinn, Samuel N., Sefako, Ramotholo, Timmermans, Mathilde, Vezie, Michael, and de Wit, Julien

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

Observations and statistical studies have shown that giant planets are rare around M dwarfs compared with Sun-like stars. The formation mechanism of these extreme systems remains under debate for decades. With the help of the TESS mission and ground based follow-up observations, we report the discovery of TOI-4201b, the most massive and densest hot Jupiter around an M dwarf known so far with a radius of $1.22\pm 0.04\ R_J$ and a mass of $2.48\pm0.09\ M_J$, about 5 times heavier than most other giant planets around M dwarfs. It also has the highest planet-to-star mass ratio ($q\sim 4\times 10^{-3}$) among such systems. The host star is an early-M dwarf with a mass of $0.61\pm0.02\ M_{\odot}$ and a radius of $0.63\pm0.02\ R_{\odot}$. It has significant super-solar iron abundance ([Fe/H]=$0.52\pm 0.08$ dex). However, interior structure modeling suggests that its planet TOI-4201b is metal-poor, which challenges the classical core-accretion correlation of stellar-planet metallicity, unless the planet is inflated by additional energy sources. Building on the detection of this planet, we compare the stellar metallicity distribution of four planetary groups: hot/warm Jupiters around G/M dwarfs. We find that hot/warm Jupiters show a similar metallicity dependence around G-type stars. For M dwarf host stars, the occurrence of hot Jupiters shows a much stronger correlation with iron abundance, while warm Jupiters display a weaker preference, indicating possible different formation histories., 21 pages, 11 figures, 4 tables, submitted to AJ

Published
2023

20. A chemical survey of exoplanets with ARIEL

Author

Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Heske, Astrid, Leconte, Jérémy, Micela, Giusi, Ollivier, Marc, Pilbratt, Göran, Puig, Ludovic, Turrini, Diego, Vandenbussche, Bart, Wolkenberg, Paulina, Beaulieu, Jean-Philippe, Buchave, Lars A., Ferus, Martin, Griffin, Matt, Guedel, Manuel, Justtanont, Kay, Lagage, Pierre-Olivier, Machado, Pedro, Malaguti, Giuseppe, Min, Michiel, Nørgaard-Nielsen, Hans Ulrik, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Swain, Mark, Szabo, Robert, Werner, Stephanie, Barstow, Joanna, Burleigh, Matt, Cho, James, du Foresto, Vincent Coudé, Coustenis, Athena, Decin, Leen, Encrenaz, Therese, Galand, Marina, Gillon, Michael, Helled, Ravit, Morales, Juan Carlos, Muñoz, Antonio García, Moneti, Andrea, Pagano, Isabella, Pascale, Enzo, Piccioni, Giuseppe, Pinfield, David, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Triaud, Amaury, Venot, Olivia, Waldmann, Ingo, Waltham, David, Wright, Gillian, Amiaux, Jerome, Auguères, Jean-Louis, Berthé, Michel, Bezawada, Naidu, Bishop, Georgia, Bowles, Neil, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Crouzet, Pierre-Elie, Da Peppo, Vania, Sanz, Isabel Escudero, Focardi, Mauro, Frericks, Martin, Hunt, Tom, Kohley, Ralf, Middleton, Kevin, Morgante, Gianluca, Ottensamer, Roland, Pace, Emanuele, Pearson, Chris, Stamper, Richard, Symonds, Kate, Rengel, Miriam, Renotte, Etienne, Ade, Peter, Affer, Laura, Alard, Christophe, Allard, Nicole, Altieri, Francesca, André, Yves, Arena, Claudio, Argyriou, Ioannis, Aylward, Alan, Baccani, Cristian, Bakos, Gaspar, Banaszkiewicz, Marek, Barlow, Mike, Batista, Virginie, Bellucci, Giancarlo, Benatti, Serena, Bernardi, Pernelle, Bézard, Bruno, Blecka, Maria, Bolmont, Emeline, Bonfond, Bertrand, Bonito, Rosaria, Bonomo, Aldo S., Brucato, John Robert, Brun, Allan Sacha, Bryson, Ian, Bujwan, Waldemar, Casewell, Sarah, Charnay, Bejamin, Pestellini, Cesare Cecchi, Chen, Guo, Ciaravella, Angela, Claudi, Riccardo, Clédassou, Rodolphe, Damasso, Mario, Damiano, Mario, Danielski, Camilla, Deroo, Pieter, Di Giorgio, Anna Maria, Dominik, Carsten, Doublier, Vanessa, Doyle, Simon, Doyon, René, Drummond, Benjamin, Duong, Bastien, Eales, Stephen, Edwards, Billy, Farina, Maria, Flaccomio, Ettore, Fletcher, Leigh, Forget, François, Fossey, Steve, Fränz, Markus, Fujii, Yuka, García-Piquer, Álvaro, Gear, Walter, Geoffray, Hervé, Gérard, Jean Claude, Gesa, Lluis, Gomez, H., Graczyk, Rafał, Griffith, Caitlin, Grodent, Denis, Guarcello, Mario Giuseppe, Gustin, Jacques, Hamano, Keiko, Hargrave, Peter, Hello, Yann, Heng, Kevin, Herrero, Enrique, Hornstrup, Allan, Hubert, Benoit, Ida, Shigeru, Ikoma, Masahiro, Iro, Nicolas, Irwin, Patrick, Jarchow, Christopher, Jaubert, Jean, Jones, Hugh, Julien, Queyrel, Kameda, Shingo, Kerschbaum, Franz, Kervella, Pierre, Koskinen, Tommi, Krijger, Matthijs, Krupp, Norbert, Lafarga, Marina, Landini, Federico, Lellouch, Emanuel, Leto, Giuseppe, Luntzer, A., Rank-Lüftinger, Theresa, Maggio, Antonio, Maldonado, Jesus, Maillard, Jean-Pierre, Mall, Urs, Marquette, Jean-Baptiste, Mathis, Stephane, Maxted, Pierre, Matsuo, Taro, Medvedev, Alexander, Miguel, Yamila, Minier, Vincent, Morello, Giuseppe, Mura, Alessandro, Narita, Norio, Nascimbeni, Valerio, Nguyen Tong, N., Noce, Vladimiro, Oliva, Fabrizio, Palle, Enric, Palmer, Paul, Pancrazzi, Maurizio, Papageorgiou, Andreas, Parmentier, Vivien, Perger, Manuel, Petralia, Antonino, Pezzuto, Stefano, Pierrehumbert, Ray, Pillitteri, Ignazio, Piotto, Giampaolo, Pisano, Giampaolo, Prisinzano, Loredana, Radioti, Aikaterini, Réess, Jean-Michel, Rezac, Ladislav, Rocchetto, Marco, Rosich, Albert, Sanna, Nicoletta, Santerne, Alexandre, Savini, Giorgio, Scandariato, Gaetano, Sicardy, Bruno, Sierra, Carles, Sindoni, Giuseppe, Skup, Konrad, Snellen, Ignas, Sobiecki, Mateusz, Soret, Lauriane, Sozzetti, Alessandro, Stiepen, A., Strugarek, Antoine, Taylor, Jake, Taylor, William, Terenzi, Luca, Tessenyi, Marcell, Tsiaras, Angelos, Tucker, C., Valencia, Diana, Vasisht, Gautam, Vazan, Allona, Vilardell, Francesc, Vinatier, Sabrine, Viti, Serena, Waters, Rens, Wawer, Piotr, Wawrzaszek, Anna, Whitworth, Anthony, Yung, Yuk L., Yurchenko, Sergey N., Osorio, María Rosa Zapatero, Zellem, Robert, Zingales, Tiziano, and Zwart, Frans

Published
2018
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21. Changes in erythrocyte deformability during day and possible role of melatonin

Author

Vazan Rastislav, Plauterova Katarina, Porubska Gabriela, and Radosinska Jana

Subjects
erythrocyte deformability, filtrability, diurnal changes, melatonin, Diseases of the endocrine glands. Clinical endocrinology, RC648-665
Abstract

Objectives. The deformability of erythrocytes is their ability to change shape in order to pass through the capillaries. Th is is necessary for quality of microcirculation and sufficient delivery of oxygen to the tissues. Th e aim of our study was to investigate the possible spontaneous changes in the erythrocyte deformability during day and evaluation of the possible direct effects of melatonin (hormone involved in regulation of biorhythms) on the erythrocyte deformability. Methods. Samples of capillary blood were taken from 12 healthy volunteers in the morning (8:00) and early in the evening (16:30). Determination of erythrocyte deformability was done based on the measurement of their filtrability. It was measured immediately aft er the sample collection and 2-hour lasting incubation without or with melatonin (2000 μmol/L). Results. Erythrocyte deformability was significantly lower in the morning (filtrability index: 0.68±0.01 morning vs. 0.71±0.01 early evening, p

Published
2018
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24. Priming Effect of on the Enhancement of Germination Traits in Aged Seeds of Chamomile (Matricaria chamomilla L.) Seeds Preserved in Medium and Long-term Storage

Author

Leila Falahhosseini, Mohammad Ali Alizadeh, and Saeed Vazan

Subjects
Chamomile, Matricaria, deterioration, Priming, Germination, seedling growth, Agriculture (General), S1-972, Medicine
Abstract

Chamomile (Matricaria chamomilla L.) is a widely used medicinal plant possessing several pharmacological effects due to presence of active compounds. In order to study of seed priming effects on seedling growth of chamomile, an experimental design, based on randomized complete design with three replications was conducted under greenhouse conditions in Research Institute of Forests and Rangelands in 2014-2015. Experimental factors were A) three chamomile accessions as code of gene bank 8959 (Brojen), 15123 (Arak) and 23879 (Isfahan), B) five conservation methods including: medium-term storage (active cold room 4 °C for 15 years), long- term storage (basic cold room-18 °C for 15 years), regenerated seeds in open storage 22 °C for 2 years (Control) and aged seed under accelerated ageing )40 °C,98% of relative humidity for 48 and 72h) and C) priming treatments including: without priming /(control), osmopriming (PEG-0.3Mpa), hormonal priming (Gibberllic acid 250 and 500ppm), hydropriming (imbibition with distilled water). Data collected for seed emergence percent, root and shoot length, seedling length, vigor index, seedling weight and three Proxidase, Catalase and Super Oxid Desmotaz (SOD) enzymatic activities. Variance analysis showed significant effects of all factors and their interactions except accession by conservation interaction effects for seedling length (P

Published
2017

27. Ariel planetary interiors White Paper

Author

Ravit Helled, Yuichi Ito, Oliver Shorttle, Caroline Dorn, Yamila Miguel, Tim Lichtenberg, Allona Vazan, Mihkel Kama, Masahiro Ikoma, Stephanie C. Werner, Tristan Guillot, Paul J. Tackley, Diana Valencia, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Helled, R [0000-0001-5555-2652], Dorn, C [0000-0001-6110-4610], Guillot, T [0000-0002-7188-8428], Ikoma, M [0000-0002-5658-5971], Ito, Y [0000-0002-0598-3021], Lichtenberg, T [0000-0002-3286-7683], Miguel, Y [0000-0002-0747-8862], Valencia, D [0000-0003-3993-4030], Vazan, A [0000-0001-9504-3174], Apollo - University of Cambridge Repository, Astronomy, University of Zurich, and Helled, Ravit

Subjects
Ariel, 010504 meteorology & atmospheric sciences, 530 Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, 01 natural sciences, Astrobiology, Atmospheric composition, Planet composition, Atmosphere-interior interaction, White paper, 1912 Space and Planetary Science, Planet, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Planetary interiors, Radius, Galaxy, Exoplanet, 13. Climate action, Space and Planetary Science, 10231 Institute for Computational Science, Physics::Space Physics, 3103 Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

The recently adopted Ariel ESA mission will measure the atmospheric composition of a large number of exoplanets. This information will then be used to better constrain planetary bulk compositions. While the connection between the composition of a planetary atmosphere and the bulk interior is still being investigated, the combination of the atmospheric composition with the measured mass and radius of exoplanets will push the field of exoplanet characterisation to the next level, and provide new insights of the nature of planets in our galaxy. In this white paper, we outline the ongoing activities of the interior working group of the Ariel mission, and list the desirable theoretical developments as well as the challenges in linking planetary atmospheres, bulk composition and interior structure., Experimental Astronomy, 53, ISSN:0922-6435, ISSN:1572-9508

Published
2022

28. Implementation of Microfluidic Chip Electrophoresis for the Detection of B-cell Clonality

Author

Vazan M, Kasubova I, Vanochova A, Lukac P, Plank L, and Lasabova Z

Subjects
b-cell clonality, protocol biomed-2, hda-page, microfluidic chip electrophoresis, Medicine
Abstract

Introduction: A clonal population of B-cells is defined as those cells arising from the mitotic division of a single somatic cell with the same rearrangement of immunoglobulin genes. This gives rise to DNA markers for each individual lymphoid cell and its progenies and enables us to study clonality in different B-cell malignancies using multiplex polymerase chain reaction - PCR. The BIOMED-2 protocol has been implemented for clonality detection in lymphoproliferative diseases and exploits multiplex PCR reaction, subsequently analyzed by heteroduplex analysis (HDA) using polyacrylamide gel electrophoresis (PAGE). With the advent of miniaturization and automation of molecular biology methods, lab-on-chip technologies were developed and replace partially the conventional approaches. We tested device for microfluidic chip, which is used for B-cells clonality analysis, using a PCR reaction for three subregions called frameworks (FR) of the immunoglobulin heavy locus (IGH) gene.

Published
2016
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29. One-Pot solvent-free synthesis of Highly Substituted Imidazoles catalyzed by zeolite

Author

Zinat Gordi and Mohammad Vazan

Subjects
Zeolite, One-pot synthesis, Solvent-free, Trisubstituted imidazoles, Tetrasubstituted imidazoles, Elementary particle physics, QC793-793.5
Abstract

A series of tri- and tetra- substituted imidazoles were synthesized from benzyl, aldehyde and ammonium acetate in the presence of zeolite as an ecofriendly reusable catalyst under microwave irradiation in the absence of solvent. The yields are high to excellent and the use of microwave irradiation reduces reaction times to few minute.

Published
2015
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32. Planetary Exploration Horizon 2061 Report, Chapter 3: From science questions to Solar System exploration

Author

Dehant, Véronique, Blanc, Michel, Mackwell, Steve, Soderlund, Krista M., Beck, Pierre, Bunce, Emma, Charnoz, Sébastien, Foing, Bernard, Filice, Valerio, Fletcher, Leigh N., Forget, François, Griton, Léa, Hammel, Heidi, Höning, Dennis, Imamura, Takeshi, Jackman, Caitriona, Kaspi, Yohai, Korablev, Oleg, Leconte, Jérémy, Lellouch, Emmanuel, Marty, Bernard, Mangold, Nicolas, Michel, Patrick, Morbidelli, Alessandro, Mousis, Olivier, Prieto-Ballesteros, Olga, Spohn, Tilman, Schmidt, Jürgen, Sterken, Veerle J., Tosi, Nicola, Vandaele, Ann C., Vernazza, Pierre, Vazan, Allona, and Westall, Frances

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), A.1, H.1.0, Physics - Geophysics, 86-02, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Geophysics (physics.geo-ph), Astrophysics - Earth and Planetary Astrophysics
Abstract

This chapter of the Planetary Exploration Horizon 2061 Report reviews the way the six key questions about planetary systems, from their origins to the way they work and their habitability, identified in chapter 1, can be addressed by means of solar system exploration, and how one can find partial answers to these six questions by flying to the different provinces to the solar system: terrestrial planets, giant planets, small bodies, and up to its interface with the local interstellar medium. It derives from this analysis a synthetic description of the most important space observations to be performed at the different solar system objects by future planetary exploration missions. These observation requirements illustrate the diversity of measurement techniques to be used as well as the diversity of destinations where these observations must be made. They constitute the base for the identification of the future planetary missions we need to fly by 2061, which are described in chapter 4. Q1- How well do we understand the diversity of planetary systems objects? Q2- How well do we understand the diversity of planetary system architectures? Q3- What are the origins and formation scenarios for planetary systems? Q4- How do planetary systems work? Q5- Do planetary systems host potential habitats? Q6- Where and how to search for life?, 107 pages, 37 figures, Horizon 2061 is a science-driven, foresight exercise, for future scientific investigations

Published
2022

34. Chapter 3 - From science questions to Solar System exploration

Author

Dehant, Véronique, Blanc, Michel, Mackwell, Steve, Soderlund, Krista M., Beck, Pierre, Bunce, Emma, Charnoz, Sébastien, Foing, Bernard, Filice, Valerio, Fletcher, Leigh N., Forget, François, Griton, Léa, Hammel, Heidi, Höning, Dennis, Imamura, Takeshi, Jackman, Caitriona, Kaspi, Yohai, Korablev, Oleg, Leconte, Jérémy, Lellouch, Emmanuel, Marty, Bernard, Mangold, Nicolas, Michel, Patrick, Morbidelli, Alessandro, Mousis, Olivier, Prieto-Ballesteros, Olga, Spohn, Tilman, Schmidt, Juergen, Sterken, Veerle J., Tosi, Nicola, Vandaele, Ann C., Vernazza, Pierre, Vazan, Allona, and Westall, Frances

Published
2023
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36. Exploring the link between star and planet formation with Ariel

Author

Fabrizio Oliva, Linda Podio, Athanasia Nikolaou, Marco Pignatari, Sergio Fonte, Davide Fedele, Camilla Danielski, Diego Turrini, Allona Vazan, Ravit Helled, Mihkel Kama, Sho Shibata, Yamila Miguel, Masahiro Ikoma, Antonio Garufi, Olja Panić, Tadahiro Kimura, Paulina Wolkenberg, Hans Rickman, Eugenio Schisano, Sergio Molinari, Jesus Maldonado, J. M. Diederik Kruijssen, Claudio Codella, M. G. Guarcello, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, National Science Foundation (US), and Istituto Nazionale di Astrofisica

Subjects
Ariel, 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, Protoplanetary discs, Star (graph theory), Stellar classification, 01 natural sciences, Astrobiology, Atmospheric composition, Planet, 0103 physical sciences, Planet Formation, Stellar characterization, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Planet formation, education.field_of_study, Star formation, Astronomy and Astrophysics, Protoplanetary Discs, Galaxy, Galactic environment, Stellar Characterization, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Star Formation, Astrophysics::Earth and Planetary Astrophysics, Galactic Environment, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made., The goal of the Ariel space mission is to observe a large and diversified population of transiting planets around a range of host star types to collect information on their atmospheric composition. The planetary bulk and atmospheric compositions bear the marks of the way the planets formed: Ariel’s observations will therefore provide an unprecedented wealth of data to advance our understanding of planet formation in our Galaxy. A number of environmental and evolutionary factors, however, can affect the final atmospheric composition. Here we provide a concise overview of which factors and effects of the star and planet formation processes can shape the atmospheric compositions that will be observed by Ariel, and highlight how Ariel’s characteristics make this mission optimally suited to address this very complex problem. © The Author(s) 2021., D.T., S.F., S.M., E.S., and A.N. acknowledge the support of the Italian Space Agency (ASI) through the ASI-INAF contract 2018-22-HH.0. D.T., C.C., D.F., and L.P. acknowledge the support of the PRIN-INAF 2016 “The Cradle of Life - GENESIS-SKA (General Conditions in Early Planetary Systems for the rise of life with SKA”. D.T., S.F., S.M. D.F, J.M., F.O., P.W. acknowledge the support of the Italian National Institute of Astrophysics (INAF) through the INAF Main Stream project “Ariel and the astrochemical link between circumstellar discs and planets” (CUP: C54I19000700005). S.M. acknowledges support from the European Research Council via the Horizon 2020 Framework Programme ERC Synergy “ECOGAL” Project GA-855130. M.K. acknowledges funding by the University of Tartu ASTRA project 2014-2020.4.01.16-0029 KOMEET “Benefits for Estonian Society from Space Research and Application”, financed by the EU European Regional Development Fund. J.M.D.K. gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) through an Emmy Noether Research Group (grant number KR4801/1-1) and the DFG Sachbeihilfe (grant number KR4801/2-1), as well as from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907). The research of O.P. is funded by the Royal Society, through Royal Society Dorothy Hodgkin Fellowship DH140243. M.P. thanks the support to NuGrid from STFC (through the University of Hull’s Consolidated Grant ST/R000840/1), and access to VIPER, the University of Hull High Performance Computing Facility. M.P. acknowledges the support from the ”Lendulet-2014” Program of the Hungarian Academy of Sciences (Hungary), from the ERC Consolidator Grant (Hungary) funding scheme (Project RADIOSTAR, G.A. n. 724560), by the National Science Foundation (NSF, USA) under grant No. PHY-1430152 (JINA Center for the Evolution of the Elements). M.P. also thanks the UK network BRIDGCE and the ChETEC COST Action (CA16117), supported by COST (European Cooperation in Science and Technology). M.I. thanks the support by JSPS KAKENHI 18H05439. C.D. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709), and the Group project Ref. PID2019-110689RB-I00/AEI/10.13039/501100011033.

Published
2022

38. Interior and Evolution of the Giant Planets.

Author

Miguel, Yamila and Vazan, Allona

Subjects
*MAGNETIC field measurements, *PLANETARY interiors, *SOLAR system, *URANUS (Planet), *JUPITER (Planet)
Abstract

The giant planets were the first to form and hold the key to unveiling the solar system's formation history in their interiors and atmospheres. Furthermore, the unique conditions present in the interiors of the giant planets make them natural laboratories for exploring different elements under extreme conditions. We are at a unique time to study these planets. The missions Juno to Jupiter and Cassini to Saturn have provided invaluable information to reveal their interiors like never before, including extremely accurate gravity data, atmospheric abundances and magnetic field measurements that revolutionised our knowledge of their interior structures. At the same time, new laboratory experiments and modelling efforts also improved, and statistical analysis of these planets is now possible to explore all the different conditions that shape their interiors. We review the interior structure of Jupiter, Saturn, Uranus and Neptune, including the need for inhomogeneous structures to explain the data, the problems unsolved and the effect that advances in our understanding of their internal structure have on their formation and evolution. [ABSTRACT FROM AUTHOR]

Published
2023
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42. Hypertensive disorders in women with peripartum cardiomyopathy: insights from the ESC EORP PPCM Registry

Author

Jackson, Alice M., Petrie, Mark C., Frogoudaki, Alexandra, Laroche, Cécile, Gustafsson, Finn, Ibrahim, Bassem, Mebazaa, Alexandre, Johnson, Mark R., Seferovic, Petar M., Regitz‐Zagrosek, Vera, Mbakwem, Amam, Böhm, Michael, Prameswari, Hawani Sasmaya, Abdel Gawad, Doaa Ahmed Fouad, Goland, Sorel, Damasceno, Albertino, Karaye, Kamilu, Farhan, Hasan Ali, Hamdan, Righab, Maggioni, Aldo P., Sliwa, Karen, Bauersachs, Johann, Meer, Peter, Favaloro, R., Favaloro, L., Carballo, M., Peradejordi, M., Renedo, M.F., Absi, D., Bertolotti, A., Ratto, R., Talavera, M.L., Gomez, R., Lockwood, S., Barton, T., Austin, M‐A., Arstall, M., Aldridge, E., Chow, Y.Y., Dekker, G., Mahadavan, G., Rose, J., Wittwer, M., Hoppe, U., Sandhofer, A., Bahshaliyev, A., Gasimov, Z., Babayev, A., Niftiyev, P., Hasanova, I., AlBannay, R., AlHaiki, W., Husain, A., Mahdi, N., Kurlianskaya, A., Lukyanchyk, M., Shatova, O., Troyanova‐Shchutskaia, T., Anghel, L., De Pauw, M., Gevaert, S., De Backer, J., De Hosson, M., Vervaet, P., Timmermans, P.J., Janssen, A., Yameogo, N.V., Kagambega, L.J., Cumyn, A., Caron, N., Cote, A‐M., Sauve, N., Nkulu, D. Ngoy, Lez, D. Malamba, Yolola, E. Ngoy, Krejci, J., Poloczkova, H., Ersboll, A., Gustafsson, F., Elrakshy, Y., Hassanein, M., Hammad, B., Eldin, O. Nour, Fouad, D., Salman, S., Zareh, Z., Abdeall, D., Elenin, H. Abo, Ebaid, H., El Nagar, A., Farag, S., Saed, M., El Rahman, Y H Abd, Ibrahim, B.S., Abdelhamid, M., Hanna, R.N. W., Youssef, G., Awad, R., Botrous, O.L. I., Halawa, S. Ibrahim, Nasr, G., Saad, A., El Tahlawi, M., Abdelbaset, M., El‐saadawy, M., El‐shorbagy, A., Shalaby, G., Anttonen, O., Tolppanen, H., Hamekoski, S., Menez, T., Noel, A., Lamblin, N., Mouquet, F., Coulon, C., Groote, P., Langlois, S., Schurtz, G., Cohen‐Solal, A., Mebazaa, A., Fournier, M‐C., Louadah, B., Akrout, N., Logeart, D., Leurent, G., Jovanova, S., Arnaudova‐Dezulovicj, F., Livrinova, V., Bauersachs, J., Hilfiker‐Kleiner, D., Berliner, D., Jungesblut, M., Koenig, T., Moulig, V.A., Pfeffer, T.J., Böhm, M., Kindermann, I., Schwarz, V., Schmitt, C., Swojanowsky, P., Pettit, S., Petrie, M., McAdam, M., Patton, D., Bakhai, A., Krishnamurthy, V., Lim, L., Clifford, P., Bowers, N., Clark, A. L., Witte, K., Cullington, D., Oliver, J., Simms, A., Mcginlay, M., McDonagh, T., Shah, A. M., Amin‐Youssef, G., De Courcey, J., Martin, K., Shaw, S., Vause, S., Wallace, S., Malin, G., Wick, C., Nikolaou, M., Rentoukas, I., Chinchilla, H., Andino, L., Iyengar, S., Chandra, S., Yadav, D.K., Babu, R. Ravi, Singh, A.K., Kumar, S., Karunamay, B.B., Chaubey, S.K., Dhiman, S.R., Jha, V.C., Singh, S.K., Kodati, D., Dasari, R., Sultana, S., Dewi, T.I., Prameswari, H. Sasmaya, Al‐Farhan, H.A., Al‐Hussein, A., Yaseen, I.F., Al‐Azzawi, Falah, Al‐Saedi, Ghazi, Mahmood, G.M., Mohammed, M.K., Ridha, A.F., Shotan, A., Vazan, A., Goland, S., Biener, M., Senni, M., Grosu, A., Martin, E., Esposti, D. Degli, Bacchelli, S., Borghi, C., Metra, M., Sciatti, E., Orabona, R., Sani, F., Brunetti, N.D., Sinagra, G., Bobbo, M., D'Agata Mottolese, B., Gesuete, V., Rakar, S., Ramani, F., Kamiya, C., Barasa, A., Ngunga, M., Bajraktari, G., Hyseni, V., Lleshi, D., Pllana, E., Pllana, T., Noruzbaeva, A., Ismailov, F., Mirrakhimov, E., Abilova, S., Lunegova, O., Kerimkulova, A., Osmankulova, G., Duishenalieva, M., Kurmanbekova, B., Turgunov, M., Mamasaidova, S., Bektasheva, E., Kavoliuniene, A., Muckiene, G., Vaitiekiene, A., Celutkiene, J., Balkevicine, L., Barysiene, J., Chee, K.H., Damasceno, A., Machava, M., Veldhuisen, D.J., Meer, P., Berg, M., Roos‐Hesselink, J., Hagen, I., Baris, L., Hurtado, P., Ezeonu, P., Isiguzo, G., Obeka, N., Onoh, R., Asogwa, F., Onyema, C., Otti, K., Ojji, D., Odili, A., Nwankwo, A., Karaye, K., Ishaq, N., Sanni, B., Abubakar, H., Mohammed, B., Sani, M., Kehinde, M., Mbakwem, A., Afolabi, B., Amadi, C., Kilasho, M., Qamar, N., Furnaz, S., Gurmani, S., Kayani, M.G.A. Mahmood, Munir, R., Hussain, S., Malik, S., Mumtaz, S., Saligan, J.R., Rubis, P., Biernacka‐Fijalkowska, B., Lesniak‐Sobelga, A., Wisniowska‐Smialek, S., Kasprzak, J.D., Lelonek, M., Zycinski, P., Jankowski, L., Grajek, S., Oko‐Sarnowska, Z., Rutkowska, A. Bartczak, Kaluzna‐Oleksy, M., Plaskota, K., Demkow, M., Dzielinska, Z., Henzel, J., Kryczka, K., Moiseeva, O., Irtyuga, O., Karelkina, E., Zazerskaya, I., Seferovic, P.M., Milinkovic, I., Živkovic, I., Ristic, A.D., Milasinovic, D., Kong, W. KF, Tan, L.K., Tan, J.L., Thain, S., Poh, K.K., Yip, J., Sliwa, K., Azibani, F., Hovelmann, J., Viljoen, C., Briton, O., Zamora, E., Orcajo, N. Alonso, Carbonell, R., Pascual, C., Muncharaz, J. Farre, Alonso‐Pulpon, L., Cubero, J. Segovia, Urquia, M. Taibo, Garcia‐Pavia, P., Gomez‐Bueno, M., Cobo‐Marcos, M., Briceno, A., Galvan, E. De Teresa, Garcia‐Pinilla, J.M., Robles‐Mezcua, A., Morcillo‐Hildalgo, L., Elbushi, A., Suliman, A., Ahamed, N., Jazzar, K., Murtada, M., Schaufelberger, M., Goloskokova, V., Hullin, R., Yarol, N., Arrigo, M., Cavusoglu, Y., Eraslan, S., Fak, A.S., Enar, S. Catirli, Sarac, L., Cankurtaran, B., Gumrukcuoglu, H., Ozturk, F., Omagino, J., Mondo, C., Lwabi, P., Ingabire, P., Nabbaale, J., Nyakoojo, W., Okello, E., Sebatta, E., Ssinabulya, I., Atukunda, E., Kitooleko, S., Semu, T., Salih, B.T., Komaranchath, A.M., Almahmeed, W.A.R., Gerges, F., Farook, F.S. Mohamed, Albakshy, F., Mahmood, N., Wani, S., Freudenberger, R., Islam, N., Quinones, J., Sundlof, D., Beitler, C., Centolanza, L., Cornell, K., Huffaker, S., Matos, L., Marzo, K., Paruchuri, V., Patel, D., Abdullaev, T., Alyavi, B., Mirzarakhimova, S., Tsoy, I., Bekbulatova, R., and Uzokov, J.

Abstract

Aims: \ud Hypertensive disorders occur in women with peripartum cardiomyopathy (PPCM). How often hypertensive disorders co-exist, and to what extent they impact outcomes, is less clear. We describe differences in phenotype and outcomes in women with PPCM with and without hypertensive disorders during pregnancy.\ud \ud Methods: \ud The European Society of Cardiology PPCM Registry enrolled women with PPCM from 2012-2018. Three groups were examined: 1) women without hypertension (‘PPCM-noHTN’); 2) women with hypertension but without pre-eclampsia (‘PPCM-HTN’); 3) women with pre-eclampsia (‘PPCM-PE’). Maternal (6-month) and neonatal outcomes were compared.\ud \ud Results: \ud Of 735 women included, 452 (61.5%) had PPCM-noHTN, 99 (13.5%) had PPCM-HTN and 184 (25.0%) had PPCM-PE. Compared to women with PPCM-noHTN, women with PPCM-PE had more severe symptoms (NYHA IV in 44.4% and 29.9%, p

Published
2021

43. Rye Cover Crop Management Affects Weeds and Yield of Corn (Zea mays L.)

Author

Saeed MAFAKHERI, Mohammad Reza ARDAKANI, Fariba MEIGHANI, Mohammad Javad MIRHADI, and Saeed VAZAN

Subjects
Forestry, SD1-669.5, Agriculture (General), S1-972
Abstract

In recent years, increasing application of chemical herbicides has raised concerns over their destructive impacts on living organisms and environmental health and it requires studies on non-chemical weed management methods. As a result, this experiment was initiated in November 2008 at experimental field of Islamic Azad University, Karaj Branch, in order to evaluate weed-suppressive ability of winter rye cover crop and mulch, and its effects on following corn yield production. Treatments included three rye seeding rates (500, 750 and 1000 kernels/m2) and three rye kill dates (29/3/2009, 15/4/2009 and 3/5/2009). In the fall 2008 rye was planted, then in the above three dates have been killed and left on the soil surface to provide mulching effect. Then in middle of June 2009, corn plants planted on the same plots of winter rye. Weeds density and biomass production were monitored in the fourth, sixth and eighth weeks after planting (WAP) corn. Corn yield production was also measured in late October 2009. Results showed that rye seeding rate has not affected weeds significantly but rye kill date had significant effect. The first kill date stimulated weeds germination and growth. The third kill date reduced density of all weeds in the fourth WAP on average 28.73% and their biomass production in the sixth WAP on average 21.38%. This treatment also increased corn grain production 7.89% at the end of the season. Finally, results of the experiment indicate that using cover crops should be combined with other methods to control weeds efficiently and to prevent yield production loss.

Published
2010
Full Text
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44. The Modeling of Development Stages of Sunflower on the Basis of Temperature and Photoperiod

Author

Sasan REZADUST, Mohamad MEHDI KARIMI, Saiid VAZAN, Mohammad Reza ARDAKANI, Ali KASHANI, and Esmaeel GHOLINEZHAD

Subjects
Forestry, SD1-669.5, Agriculture (General), S1-972
Abstract

This experiment was conducted at the Station of Agricultural Research and Natural Resources, Khoy, Iran in 2007 and 2008 to evaluate the effect of temperature and photoperiod on the duration of development stages of sunflower. A randomized complete block design using a 8 x 3 factorial arrangement with four replications involving eight plantings (29th April, 4th May, 14th May, 24th May, 1st June, 10th June, 19th June and 28th June) and three sunflower cultivars (‘Sor’, ‘Eroflor’, ‘Azargol’). From the results obtained, all development stages, especially the generative phase were influenced by planting date. The duration of each development stage decreased with the delay in planting. The designed models indicated that the minimum temperature and photoperiod were directly proportional to development rate (DR) the whole life cycle of different sunflower cultivars. DR decreased from emergence (E) to physiological maturity (PM) as day length increased. The relationship between DR and photoperiod could be used as a practical model for estimating E to PM duration of these sunflower cultivars.

Published
2010
Full Text
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45. Jointly Modeling Aspect and Polarity for Aspect-based Sentiment Analysis in Persian Reviews

Author

Vazan, Milad and Razmara, Jafar

Subjects
FOS: Computer and information sciences, Artificial Intelligence (cs.AI), Computer Science - Computation and Language, Computer Science - Artificial Intelligence, Computation and Language (cs.CL)
Abstract

Identification of user's opinions from natural language text has become an exciting field of research due to its growing applications in the real world. The research field is known as sentiment analysis and classification, where aspect category detection (ACD) and aspect category polarity (ACP) are two important sub-tasks of aspect-based sentiment analysis. The goal in ACD is to specify which aspect of the entity comes up in opinion while ACP aims to specify the polarity of each aspect category from the ACD task. The previous works mostly propose separate solutions for these two sub-tasks. This paper focuses on the ACD and ACP sub-tasks to solve both problems simultaneously. The proposed method carries out multi-label classification where four different deep models were employed and comparatively evaluated to examine their performance. A dataset of Persian reviews was collected from CinemaTicket website including 2200 samples from 14 categories. The developed models were evaluated using the collected dataset in terms of example-based and label-based metrics. The results indicate the high applicability and preference of the CNN and GRU models in comparison to LSTM and Bi-LSTM., 20 pages, 9 figures

Published
2021

46. How planets grow by pebble accretion IV: Envelope opacity trends from sedimenting dust and pebbles

Author

Amy Bonsor, Allona Vazan, Chris W. Ormel, and M. G. Brouwers

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Solar System, Planetesimal, Opacity, Uranus, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Accretion (astrophysics), humanities, Space and Planetary Science, Planet, Neptune, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The amount of nebular gas that a planet can bind is limited by its cooling rate, which is set by the opacity of its envelope. Accreting dust and pebbles contribute to the envelope opacity and, thus, influence the outcome of planet formation. Our aim is to model the size evolution and opacity contribution of solids inside planetary envelopes. We then use the resultant opacity relations to study emergent trends in planet formation. We design a model for the opacity of solids in planetary envelopes that accounts for the growth, fragmentation and erosion of pebbles during their sedimentation. We formulate analytical expressions for the opacity of pebbles and dust and map out their trends as a function of depth, planet mass, distance and accretion rate. We find that the accretion of pebbles rather than planetesimals can produce fully convective envelopes, but only in lower-mass planets that reside in the outer disk or in those that are accreting pebbles at a high rate. In these conditions, pebble sizes are limited by fragmentation and erosion, allowing them to pile up in the envelope. At higher planetary masses or reduced accretion rates, a different regime applies where the sizes of sedimenting pebbles are only limited by their rate of growth. The opacity in this growth-limited regime is much lower, steeply declines with depth and planet mass but is invariant with the pebble mass flux. Our results imply that the opacity of a forming planetary envelope can not be approximated by a value that is constant with either depth or planet mass. When applied to the Solar System, we argue that Uranus and Neptune could not have maintained a sufficiently high opacity to avoid runaway gas accretion unless they both experienced sufficiently rapid accretion of solids and formed late., Accepted to A&A. Comments are welcome

Published
2021

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