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1. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS$_4$ measured from stellar occultations

Author

Rommel, F. L., Braga-Ribas, F., Ortiz, J. L., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J. I. B., Vieira-Martins, R., Assafin, M., Morgado, B. E., Boufleur, R. C., Benedetti-Rossi, G., Gomes-Júnior, A. R., Fernández-Valenzuela, E., Holler, B. J., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J. L., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, R., Aissa, D. Baba, Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fişek, S., Çakır, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C. L., Emilio, M., Burdanov, A. Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R. Zanmar, Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuž, H., Bacci, P., Maestripieri, M., Grazia, M. D., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O. M., Serra-Ricart, M., Alarcon, M. R., Licandro, J., Masi, G., Bacci, R., Bosch, J. M., Behem, R., Prost, J. -P., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A. P., Montigiani, N., Foster, C. R., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pál, A., Csák, B., Fernández-Garcia, E., Castro-Tirado, A. J., Hudin, L., Madiedo, J. M., Anghel, R. M., Calvo-Fernández, J. F., Valvasori, A., Guido, E., Gherase, R. M., Kamoun, S., Fafet, R., Sánchez-González, M., Curelaru, L., Vîntdevară, C. D., Danescu, C. A., Gout, J. -F., Schmitz, C. J., Sota, A., Belskaya, I., Rodríguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssière, M., Oliveira, J. Marques, Popescu, M., Mammana, L. A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Pribulla, T., Tomko, D., Husárik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gährken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P. Waldemar, Bykowski, W., Müller, T. G., Ogloza, W., Gonçalves, R., Ferreira, J. F., Ferreira, M., Bento, M., Meister, S., Bagiran, M. N., Tekeş, M., Marciniak, A., Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G. B., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klös, O., Weber, C., Urbaník, M., Rousselot, L., Kubánek, J., André, P., Colazo, C., Spagnotto, J., Sickafoose, A. A., Hueso, R., Sánchez-Lavega, A., Fisher, R. S., Rengstorf, A. W., Perelló, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O. C., Kalkan, S., Canales-Moreno, O., Trigo-Rodríguez, J. M., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D. N., Dumitrescu, V., Wilberger, A. J., Barnes, J. W., Fieber-Beyer, S. K., Swaney, R. L., Fuentes, C., Mendez, R. A., Dumitru, B. D., Flynn, R. L., and Wake, D. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

This work aims at constraining the size, shape, and geometric albedo of the dwarf planet candidate 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also studied the object's topography by analyzing the obtained limb and the residuals between observed chords and the best-fitted ellipse. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with three to up to sixty-one positive chords. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fitted ellipse, combined with the object's rotational information from the literature, constrains the object's size, shape, and albedo. Additionally, we developed a new method to characterize topography features on the object's limb. The global limb has a semi-major axis of 412 $\pm$ 10 km, a semi-minor axis of 385 $\pm$ 17 km, and the position angle of the minor axis is 121 $^\circ$ $\pm$ 16$^\circ$. From this instantaneous limb, we obtained 2002 MS4's geometric albedo and the projected area-equivalent diameter. Significant deviations from the fitted ellipse in the northernmost limb are detected from multiple sites highlighting three distinct topographic features: one 11 km depth depression followed by a 25$^{+4}_{-5}$ km height elevation next to a crater-like depression with an extension of 322 $\pm$ 39 km and 45.1 $\pm$ 1.5 km deep. Our results present an object that is $\approx$138 km smaller in diameter than derived from thermal data, possibly indicating the presence of a so-far unknown satellite. However, within the error bars, the geometric albedo in the V-band agrees with the results published in the literature, even with the radiometric-derived albedo.

Published
2023
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2. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author

Ortiz, J. L., Santos-Sanz, P., Sicardy, B., Benedetti-Rossi, G., Bérard, D., Morales, N., Duffard, R., Braga-Ribas, F., Hopp, U., Ries, C., Nascimbeni, V., Marzari, F., Granata, V., Pál, A., Kiss, C., Pribulla, T., Komžík, R., Hornoch, K., Pravec, P., Bacci, P., Maestripieri, M., Nerli, L., Mazzei, L., Bachini, M., Martinelli, F., Succi, G., Ciabattari, F., Mikuz, H., Carbognani, A., Gaehrken, B., Mottola, S., Hellmic, S., Rommel, F. L., Fernández-Valenzuela, E., Bagatin, A. Campo, Cikota, S., Cikota, A., Lecacheux, J., Vieira-Martins, R., Camargo, J. I. B., Assafin, M., Colas, F., Behrend, R., Desmars, J., Meza, E., Alvarez-Candal, A., Beisker, W., Gomes-Junior, A. R., Morgado, B. E., Roques, F., Vachier, F., Berthier, J., Mueller, T. G., Madiedo, J. M., Unsalan, O., Sonbas, E., Karaman, N., Erece, O., Koseoglu, D. T., Ozisik, T., Kalkan, S., Guney, Y., Niaei, M. S., Satir, O., Yesilyaprak, C., Puskullu, C., Kabas, A., Demircan, O., Alikakos, J., Charmandaris, V., Leto, G., Ohlert, J., Christille, J. M., Szakáts, R., Farkas, A. Takácsné, Varga-Verebélyi, E., Marton, G., Marciniak, A., Bartczak, P., Santana-Ros, T., Butkiewicz-Bąk, M., Dudziński, G., Alí-Lagoa, V., Gazeas, K., Tzouganatos, L., Paschalis, N., Tsamis, V., Sánchez-Lavega, A., Pérez-Hoyos, S., Hueso, R., Guirado, J. C., Peris, V., and Iglesias-Marzoa, R.

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

Among the four known transneptunian dwarf planets, Haumea is an exotic, very elongated, and fast rotating body. In contrast to the other dwarf planets, its size, shape, albedo, and density are not well constrained. Here we report results of a multi-chord stellar occultation, observed on 2017 January 21. Secondary events observed around the main body are consistent with the presence of a ring of opacity 0.5, width 70 km, and radius 2,287$_{-45}^{+75}$ km. The Centaur Chariklo was the first body other than a giant planet to show a ring system and the Centaur Chiron was later found to possess something similar to Chariklo's rings. Haumea is the first body outside the Centaur population with a ring. The ring is coplanar with both Haumea's equator and the orbit of its satellite Hi'iaka. Its radius places close to the 3:1 mean motion resonance with Haumea's spin period. The occultation by the main body provides an instantaneous elliptical limb with axes 1,704 $\pm$ 4 km x 1,138 $\pm$ 26 km. Combined with rotational light-curves, it constrains Haumea's 3D orientation and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea's largest axis is at least 2,322 $\pm$ 60 km, larger than thought before. This implies an upper limit of 1,885 $\pm$ 80 kg m$^{-3}$ for Haumea's density, smaller and less puzzling than previous estimations, and a geometric albedo of 0.51 $\pm$ 0.02, also smaller than previous estimations. No global N$_2$ or CH$_4$ atmosphere with pressures larger than 15 and 50 nbar (3-$\sigma$ limits), respectively, is detected.

Published
2020
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3. The large Trans-Neptunian Object 2002 TC$_{302}$ from combined stellar occultation, photometry and astrometry data

Author

Ortiz, J. L., Santos-Sanz, P., Sicardy, B., Benedetti-Rossi, G., Duffard, R., Morales, N., Braga-Ribas, F., Fernández-Valenzuela, E., Nascimbeni, V., Nardiello, D., Carbognani, A., Buzzi, L., Aletti, A., Bacci, P., Maestripieri, M., Mazzei, L., Mikuz, H., Skvarc, J., Ciabattari, F., Lavalade, F., Scarfi, G., Mari, J. M., Conjat, M., Sposetti, S., Bachini, M., Succi, G., Mancini, F., Alighieri, M., Canto, E. Dal, Masucci, M., Vara-Lubiano, M., Gutiérrez, P. J., Desmars, J., Lecacheux, J., Vieira-Martins, R., Camargo, J. I. B., Assafin, M., Colas, F., Beisker, W., Behrend, R., Mueller, T. G., Meza, E., Gomes-Junior, A. R., Roques, F., Vachier, F., Mottola, S., Hellmich, S., Bagatin, A. Campo, Alvarez-Candal, A., Cikota, S., Cikota, A., Christille, J. M., Pál, A., Kiss, C., Pribulla, T., Komžík, R., Madiedo, J. M., Charmandaris, V., Alikakos, J., Szakáts, R., Farkas-Takács, A., Varga-Verebélyi, E., Marton, G., Marciniak, A., Bartczak, P., Butkiewicz-Bak, M., Dudziński, G., Alí-Lagoa, V., Gazeas, K., Paschalis, N., Tsamis, V., Guirado, J. C., Peris, V., Iglesias-Marzoa, R., Schnabel, C., Manzano, F., Navarro, A., Perelló, C., Vecchione, A., Noschese, A., and Morrone, L.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

On 28th January 2018, the large Trans-Neptunian Object (TNO) 2002TC302 occulted a m$_v= $15.3 star with ID 130957813463146112 in the Gaia DR2 stellar catalog. 12 positive occultation chords were obtained from Italy, France, Slovenia and Switzerland. Also, 4 negative detections were obtained near the north and south limbs. This represents the best observed stellar occultation by a TNO other than Pluto, in terms of the number of chords published thus far. From the 12 chords, an accurate elliptical fit to the instantaneous projection of the body, compatible with the near misses, can be obtained. The resulting ellipse has major and minor axes of 543 $\pm$ 18 km and 460 $\pm$ 11 km, respectively, with a position angle of 3 $\pm$ 1 degrees for the minor axis. This information, combined with rotational light curves obtained with the 1.5m telescope at Sierra Nevada Observatory and the 1.23m telescope at Calar Alto observatory, allows us to derive possible 3D shapes and density estimations for the body, based on hydrostatic equilibrium assumptions. The effective area equivalent diameter is $\sim$ 84 km smaller than the radiometrically derived diameter using thermal data from Herschel and Spitzer Space Telescopes. This might indicate the existence of an unresolved satellite of up to $\sim$ 300 km in diameter, to account for all the thermal flux, although the occultation and thermal diameters are compatible within their error bars given the considerable uncertainty of the thermal results. The existence of a potential satellite also appears to be consistent with other ground-based data presented here. From the effective occultation diameter combined with H$_V$ measurements we derive a geometric albedo of 0.147 $\pm$ 0.005, which would be somewhat smaller if 2002TC302 has a satellite. The best occultation light curves do not show any signs of ring features or any signatures of a global atmosphere., Comment: Accepted for publication in Astronomy & Astrophysics. 14 pages, 9 figures

Published
2020
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4. 2023 DZ2 Planetary Defense Campaign

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reddy, Vishnu, Kelley, Michael S., Benner, Lance, Dotson, Jessie, Erasmus, Nicolas, Farnocchia, Davide, Linder, Tyler, Masiero, Joseph R., Thomas, Cristina, Bauer, James M., Alarcon, Miguel R., Bacci, P., Bamberger, Daniel, Battle, Adam, Benkhaldoun, Zouhair, Betti, Guido, Birlan, Mirel, Brozovic, Marina, Burt, Brian, Cantillo, David C., Chandra, Sunil, Chomette, Gregoire, Coates, Ashley, DeMeo, Francesca, Devogèle, Maxime, Fatka, Petr, Ferrais, Marin, Fini, Paolo, van Gend, Carel, Giorgini, Jon D., Glamazda, Dmitry, Holmes, Robert, Hora, Joseph L., Horiuchi, Shinji, Hornoch, Kamil, Iozzi, Marco, Jacques, Cristóvão, Jehin, Emmanuel, Jiang, Hai, Kaiser, Galina, Kušnirák, Peter, Kuznetsov, Eduard, de León, Julia, Liakos, Alexios, Licandro, Javier, Lister, Tim, Liu, Jing, Lopez-Oquendo, Andy, Maestripieri, M., Mathias, Donovan, Micheli, Marco, Naidu, Shantanu P., Nastasi, Alessandro, Nedelcu, Alin, Petrescu, Elisabeta, Popescu, Marcel, Potter, Stephen B., Pravec, Petr, Sanchez, Juan, Santana-Ros, Toni, Serra-Ricart, M., Sioulas, Nick, Sonka, Adrian B., Squilloni, Alessio, Tombelli, Maura, Trelia, Madalina M., Trilling, David, Warner, Elizabeth M., Wells, Guy, Wheeler, Lorien, Wiles, Mike, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reddy, Vishnu, Kelley, Michael S., Benner, Lance, Dotson, Jessie, Erasmus, Nicolas, Farnocchia, Davide, Linder, Tyler, Masiero, Joseph R., Thomas, Cristina, Bauer, James M., Alarcon, Miguel R., Bacci, P., Bamberger, Daniel, Battle, Adam, Benkhaldoun, Zouhair, Betti, Guido, Birlan, Mirel, Brozovic, Marina, Burt, Brian, Cantillo, David C., Chandra, Sunil, Chomette, Gregoire, Coates, Ashley, DeMeo, Francesca, Devogèle, Maxime, Fatka, Petr, Ferrais, Marin, Fini, Paolo, van Gend, Carel, Giorgini, Jon D., Glamazda, Dmitry, Holmes, Robert, Hora, Joseph L., Horiuchi, Shinji, Hornoch, Kamil, Iozzi, Marco, Jacques, Cristóvão, Jehin, Emmanuel, Jiang, Hai, Kaiser, Galina, Kušnirák, Peter, Kuznetsov, Eduard, de León, Julia, Liakos, Alexios, Licandro, Javier, Lister, Tim, Liu, Jing, Lopez-Oquendo, Andy, Maestripieri, M., Mathias, Donovan, Micheli, Marco, Naidu, Shantanu P., Nastasi, Alessandro, Nedelcu, Alin, Petrescu, Elisabeta, Popescu, Marcel, Potter, Stephen B., Pravec, Petr, Sanchez, Juan, Santana-Ros, Toni, Serra-Ricart, M., Sioulas, Nick, Sonka, Adrian B., Squilloni, Alessio, Tombelli, Maura, Trelia, Madalina M., Trilling, David, Warner, Elizabeth M., Wells, Guy, Wheeler, Lorien, and Wiles, Mike

Abstract

We present the results of a fourth planetary defense exercise, focused this time on the small near-Earth asteroid (NEA) 2023 DZ2 and conducted during its close approach to the Earth in 2023 March. The International Asteroid Warning Network (IAWN), with support from NASA's Planetary Defense Coordination Office (PDCO), has been coordinating planetary defense observational campaigns since 2017 to test the operational readiness of the global planetary defense capabilities. The last campaign focused on the NEA Apophis, and an outcome of that exercise was the need for a short burst campaign to replicate a real-life near-Earth object impact hazard scenario. The goal of the 2023 DZ2 campaign was to characterize the small NEA as a potential impactor and exercise the planetary defense system including observations, hypothetical risk assessment and risk prediction, and hazard communication with a short notice of just 24 hr. The entire campaign lasted about 10 days. The campaign team was divided into several working groups based on the characterization method: photometry, spectroscopy, thermal IR photometry and optical polarimetry, radar, and risk assessment. Science results from the campaign show that 2023 DZ2 has a rotation period of 6.2745 ± 0.0030 minutes; visible wavelength color photometry/spectroscopy/polarimetry and near-IR spectroscopy all point to an E-type taxonomic classification with surface composition analogous to aubrite meteorites; and radar observations show that the object has a diameter of 30 ± 10 m, consistent with the high albedo (0.49) derived from polarimetric and thermal IR observations.

Published
2024

5. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author

Rommel, F. L., primary, Braga-Ribas, F., additional, Ortiz, J. L., additional, Sicardy, B., additional, Santos-Sanz, P., additional, Desmars, J., additional, Camargo, J. I. B., additional, Vieira-Martins, R., additional, Assafin, M., additional, Morgado, B. E., additional, Boufleur, R. C., additional, Benedetti-Rossi, G., additional, Gomes-Júnior, A. R., additional, Fernández-Valenzuela, E., additional, Holler, B. J., additional, Souami, D., additional, Duffard, R., additional, Margoti, G., additional, Vara-Lubiano, M., additional, Lecacheux, J., additional, Plouvier, J. L., additional, Morales, N., additional, Maury, A., additional, Fabrega, J., additional, Ceravolo, P., additional, Jehin, E., additional, Albanese, D., additional, Mariey, H., additional, Cikota, S., additional, Ruždjak, D., additional, Cikota, A., additional, Szakáts, R., additional, Baba Aissa, D., additional, Gringahcene, Z., additional, Kashuba, V., additional, Koshkin, N., additional, Zhukov, V., additional, Fişek, S., additional, Çakir, O., additional, Özer, S., additional, Schnabel, C., additional, Schnabel, M., additional, Signoret, F., additional, Morrone, L., additional, Santana-Ros, T., additional, Pereira, C. L., additional, Emilio, M., additional, Burdanov, A. Y., additional, de Wit, J., additional, Barkaoui, K., additional, Gillon, M., additional, Leto, G., additional, Frasca, A., additional, Catanzaro, G., additional, Sanchez, R. Zanmar, additional, Tagliaferri, U., additional, Di Sora, M., additional, Isopi, G., additional, Krugly, Y., additional, Slyusarev, I., additional, Chiorny, V., additional, Mikuž, H., additional, Bacci, P., additional, Maestripieri, M., additional, Grazia, M. D., additional, de la Cueva, I., additional, Yuste-Moreno, M., additional, Ciabattari, F., additional, Kozhukhov, O. M., additional, Serra-Ricart, M., additional, Alarcon, M. R., additional, Licandro, J., additional, Masi, G., additional, Bacci, R., additional, Bosch, J. M., additional, Behem, R., additional, Prost, J.-P., additional, Renner, S., additional, Conjat, M., additional, Bachini, M., additional, Succi, G., additional, Stoian, L., additional, Juravle, A., additional, Carosati, D., additional, Gowe, B., additional, Carrillo, J., additional, Zheleznyak, A. P., additional, Montigiani, N., additional, Foster, C. R., additional, Mannucci, M., additional, Ruocco, N., additional, Cuevas, F., additional, Di Marcantonio, P., additional, Coretti, I., additional, Iafrate, G., additional, Baldini, V., additional, Collins, M., additional, Pál, A., additional, Csák, B., additional, Fernández-Garcia, E., additional, Castro-Tirado, A. J., additional, Hudin, L., additional, Madiedo, J. M., additional, Anghel, R. M., additional, Calvo-Fernández, J. F., additional, Valvasori, A., additional, Guido, E., additional, Gherase, R. M., additional, Kamoun, S., additional, Fafet, R., additional, Sánchez-González, M., additional, Curelaru, L., additional, Vîntdevară, C. D., additional, Danescu, C. A., additional, Gout, J.-F., additional, Schmitz, C. J., additional, Sota, A., additional, Belskaya, I., additional, Rodríguez-Marco, M., additional, Kilic, Y., additional, Frappa, E., additional, Klotz, A., additional, Lavayssière, M., additional, Oliveira, J. Marques, additional, Popescu, M., additional, Mammana, L. A., additional, Fernández-Lajús, E., additional, Schmidt, M., additional, Hopp, U., additional, Komžík, R., additional, Pribulla, T., additional, Tomko, D., additional, Husárik, M., additional, Erece, O., additional, Eryilmaz, S., additional, Buzzi, L., additional, Gährken, B., additional, Nardiello, D., additional, Hornoch, K., additional, Sonbas, E., additional, Er, H., additional, Burwitz, V., additional, Sybilski, P. Waldemar, additional, Bykowski, W., additional, Müller, T. G., additional, Ogloza, W., additional, Gonçalves, R., additional, Ferreira, J. F., additional, Ferreira, M., additional, Bento, M., additional, Meister, S., additional, Bagiran, M. N., additional, Tekeş, M., additional, Marciniak, A., additional, Moravec, Z., additional, Delinčák, P., additional, Gianni, G., additional, Casalnuovo, G. B., additional, Boutet, M., additional, Sanchez, J., additional, Klemt, B., additional, Wuensche, N., additional, Burzynski, W., additional, Borkowski, M., additional, Serrau, M., additional, Dangl, G., additional, Klös, O., additional, Weber, C., additional, Urbaník, M., additional, Rousselot, L., additional, Kubánek, J., additional, André, P., additional, Colazo, C., additional, Spagnotto, J., additional, Sickafoose, A. A., additional, Hueso, R., additional, Sánchez-Lavega, A., additional, Fisher, R. S., additional, Rengstorf, A. W., additional, Perelló, C., additional, Dascalu, M., additional, Altan, M., additional, Gazeas, K., additional, de Santana, T., additional, Sfair, R., additional, Winter, O. C., additional, Kalkan, S., additional, Canales-Moreno, O., additional, Trigo-Rodríguez, J. M., additional, Tsamis, V., additional, Tigani, K., additional, Sioulas, N., additional, Lekkas, G., additional, Bertesteanu, D. N., additional, Dumitrescu, V., additional, Wilberger, A. J., additional, Barnes, J. W., additional, Fieber-Beyer, S. K., additional, Swaney, R. L., additional, Fuentes, C., additional, Mendez, R. A., additional, Dumitru, B. D., additional, Flynn, R. L., additional, and Wake, D. A., additional

Published
2023
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6. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, B., Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Burwitz, V., Waldemar Sybilski, P., Bykowski, W., Müller, Thomas G., Ogloza, W., Gonçalves, R., Ferreira, J.F., Ferreira, M., Bento, M., Urbaník, M., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., Juravle, A., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Holler, B.J., Er, H., Weber, C., Kalkan, S., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Rommel, F.L., Braga-Ribas, F., Ortiz Moreno, José Luis, Sicardy, B., Santos Sanz, Pablo, Desmars, Josselin, Camargo, J.I.B., Vieira-Martins, R., Assafin, M., Morgado, B.E., Boufleur, R.C., Burwitz, V., Waldemar Sybilski, P., Bykowski, W., Müller, Thomas G., Ogloza, W., Gonçalves, R., Ferreira, J.F., Ferreira, M., Bento, M., Urbaník, M., Di Sora, M., Souami, Damya, Canales-Moreno, O., Meister, S., Bagiran, M.N., Tekeş, M., Marciniak, Anna, Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G.B., Isopi, G., Tsamis, V., Boutet, M., Sanchez, J., Trigo-Rodríguez, Josep M., Duffard, René, Renner, S., Rousselot, L., Margoti, G., Kubánek, J., André, P., Krugly, Yurij, Colazo, C., Spagnotto, J., Sickafoose, A.A., Hueso, R., Sánchez-Lavega, A., Fisher, R.S., Conjat, M., Lecacheux, J., Rengstorf, A.W., Perelló, C., Slyusarev, I., Vara-Lubiano, M., Dascalu, M., Castro-Tirado, Alberto J., Tigani, K., Sioulas, Nick, Lekkas, G., Bertesteanu, D.N., Bachini, M., Dumitrescu, V., Wilberger, A.J., Chiorny, V., Barnes, J.W., Fieber-Beyer, S.K., Swaney, R.L., Fuentes, C., Hudin, L., Plouvier, J.L., Mendez, R.A., Dumitru, B.D., Succi, G., Flynn, R.L., Mikuz, H., Wake, D.A., Morales, Nicolás, Maury, Alain, Fabrega, J., Ceravolo, P., Jehin, Emmanuel, Madiedo, J.M., Albanese, D., Mariey, H., Stoian, L., Bacci, P., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, Róbert, Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Anghel, R.M., Zhukov, V., Maestripieri, M., Juravle, A., Fişek, S., Çakir, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, Toni, Pereira, C.L., Grazia, M.D., Calvo-Fernández, J.F., Carosati, D., Emilio, M., Burdanov, A.Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Carrillo, J., Zanmar Sanchez, R., Tagliaferri, U., Gowe, B., Valvasori, A., Klemt, B., de la Cueva, I., Guido, E., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O.M., Serra-Ricart, M., Alarcon, Miguel R., Licandro, Javier, Masi, G., Bacci, Roberto, Wuensche, N., Kamoun, S., Bosch, Josep M., Behem, R., Gherase, R.M., Prost, J.-P., Altan, M., Zheleznyak, A.P., Montigiani, N., Foster, C.R., Mannucci, M., Burzynski, W., Ruocco, Nello, Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Gazeas, K., Fafet, R., Collins, M., Pál, András, Borkowski, M., Csák, B., Fernández-García, Emilio, Benedetti-Rossi, G., Sánchez-González, M., Curelaru, L., Vîntdevară, C.D., Danescu, C.A., de Santana, T., Gout, J.-F., Schmitz, C.J., Serrau, M., Sota, Alfredo, Belskaya, Irina, Rodríguez-Marco, M., Kilic, Y., Gomes-Júnior, A.R., Frappa, E., Klotz, A., Lavayssière, M., Sfair, R., Marques Oliveira, J., Dangl, G., Popescu, Marcel, Mammana, L.A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Fernández-Valenzuela, Estela, Pribulla, T., Tomko, D., Winter, O.C., Klös, O., Husárik, Marek, Erece, O., Eryilmaz, S., Buzzi, Luca, Gährken, B., Nardiello, D., Hornoch, Kamil, Sonbas, E., Holler, B.J., Er, H., Weber, C., and Kalkan, S.

Abstract

Context. The physical characterization of trans-Neptunian objects is essential for improving our understanding of the formation and evolution of our Solar System. Stellar occultation is a ground-based technique that can be successfully used to determine some of the TNOs’ fundamental physical properties with high precision, such as size and shape. Aims. This work is aimed at constraining the size, shape, and geometric albedo of the dwarf planet candidate (307261) 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also study the object’s topography by analyzing the obtained limb and residuals between the observed chords and the best-fit ellipse. Metods. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with between 3 and 61 positive chords. We derived the occultation light curves using differential aperture photometry, from which the star ingress and egress instants were calculated. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fit ellipse, combined with the object’s rotational information from the literature, sets constraints on the object’s size, shape, and albedo. Additionally, we developed a new method to characterize the topography features on the object’s limb. Results. The global limb has a semi-major axis of a′ = 412 ± 10 km, a semi-minor axis of b′= 385 ± 17 km, and the position angle of the minor axis is 121° ± 16°. From this instantaneous limb, we obtained 2002 MS4’s geometric albedo of pV = 0.1 ± 0.025, using HV = 3.63 ± 0.05 mag and a projected area-equivalent diameter of 796 ± 24 km. Significant deviations from the fitted ellipse in the northernmost limb were detected from multiple sites, highlighting three distinct topographic features: one 11 km depth depression, followed by a 25−5+4 k

Published
2023

7. The Second International Asteroid Warning Network Timing Campaign: 2005 LW3

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Farnocchia, Davide, Reddy, Vishnu, Bauer, James M., Warner, Elizabeth M., Micheli, Marco, Payne, Matthew J., Farnham, Tony, Kelley, Michael S., Alarcon, Miguel R., Bacci, P., Bacci, Roberto, Bachini, M., Baillié, Kevin, Baj, Giorgio, Bamberger, Daniel, Barkov, Anatoly P., Beck, Stefan, Betti, Guido, Biancalani, Enrico, Bolin, Bryce T., Briggs, David, Buzzi, Luca, Cheng, Haowen, Christensen, Eric, Coffano, Alessandro, Conversi, Luca, Demeautis, Christophe, Denneau, Larry, Desmars, Josselin, Djupvik, Anlaug A., Elenin, Leonid, Fini, Paolo, Felber, Tobias, Flynn, Randy, Galli, Gianni, Granvik, Mikael, Gray, Bill, Gray, Zuri, Grazzini, Luca, Hasubick, Werner, Hoffmann, Tobias, Holmes, Robert, Iozzi, Marco, Ivanov, Alexander L., Ivanov, Viktor A., Ivanova, Natalya V., Jacques, Cristóvão, Jiang, Hai, Jinghui, Zheng, Kasikov, Anni, Kim, Myung-Jin, Kumar, Balaji, Lee, Hee-Jae, Li, Bin, Liu, Jing, Licandro, Javier, Linder, Tyler, Lysenkov, Vadim E., Maestripieri, M., Mantero, Andrea, Marinello, Vladimiro, McCormick, Jennie, Moon, Darrel, Nastasi, Alessandro, Neill, James D., Neue, Guenther, Novichonok, Artem O., Ocaña, Francisco, Pizzetti, Gianpaolo, Pomazan, Anton, Purdum, Josiah N., Ratinaud, Christophe, Roh, Dong-Goo, Romanov, Filipp D., Ruocco, Nello, Santana-Ros, Toni, Scarmato, Toni, Schmalz, Anastasia, Schmalz, Sergei, Serra-Ricart, M., Sherrod, Clay, Sioulas, Nick, Soffiantini, Andrea, Succi, G., Tholen, David J., Thomsen, Jeppe S., Thuillot, William, Wainscoat, Richard, Wells, Guy, Weryk, Robert, Yakovenko, Nikolai A., Yim, Hong-Suh, Zhai, Chengxing, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Farnocchia, Davide, Reddy, Vishnu, Bauer, James M., Warner, Elizabeth M., Micheli, Marco, Payne, Matthew J., Farnham, Tony, Kelley, Michael S., Alarcon, Miguel R., Bacci, P., Bacci, Roberto, Bachini, M., Baillié, Kevin, Baj, Giorgio, Bamberger, Daniel, Barkov, Anatoly P., Beck, Stefan, Betti, Guido, Biancalani, Enrico, Bolin, Bryce T., Briggs, David, Buzzi, Luca, Cheng, Haowen, Christensen, Eric, Coffano, Alessandro, Conversi, Luca, Demeautis, Christophe, Denneau, Larry, Desmars, Josselin, Djupvik, Anlaug A., Elenin, Leonid, Fini, Paolo, Felber, Tobias, Flynn, Randy, Galli, Gianni, Granvik, Mikael, Gray, Bill, Gray, Zuri, Grazzini, Luca, Hasubick, Werner, Hoffmann, Tobias, Holmes, Robert, Iozzi, Marco, Ivanov, Alexander L., Ivanov, Viktor A., Ivanova, Natalya V., Jacques, Cristóvão, Jiang, Hai, Jinghui, Zheng, Kasikov, Anni, Kim, Myung-Jin, Kumar, Balaji, Lee, Hee-Jae, Li, Bin, Liu, Jing, Licandro, Javier, Linder, Tyler, Lysenkov, Vadim E., Maestripieri, M., Mantero, Andrea, Marinello, Vladimiro, McCormick, Jennie, Moon, Darrel, Nastasi, Alessandro, Neill, James D., Neue, Guenther, Novichonok, Artem O., Ocaña, Francisco, Pizzetti, Gianpaolo, Pomazan, Anton, Purdum, Josiah N., Ratinaud, Christophe, Roh, Dong-Goo, Romanov, Filipp D., Ruocco, Nello, Santana-Ros, Toni, Scarmato, Toni, Schmalz, Anastasia, Schmalz, Sergei, Serra-Ricart, M., Sherrod, Clay, Sioulas, Nick, Soffiantini, Andrea, Succi, G., Tholen, David J., Thomsen, Jeppe S., Thuillot, William, Wainscoat, Richard, Wells, Guy, Weryk, Robert, Yakovenko, Nikolai A., Yim, Hong-Suh, and Zhai, Chengxing

Abstract

The Earth close approach of near-Earth asteroid 2005 LW3 on 2022 November 23 represented a good opportunity for a second observing campaign to test the timing accuracy of astrometric observation. With 82 participating stations, the International Asteroid Warning Network collected 1046 observations of 2005 LW3 around the time of the close approach. Compared to the previous timing campaign targeting 2019 XS, some individual observers were able to significantly improve the accuracy of their reported observation times. In particular, U.S. surveys achieved good timing performance. However, no broad, systematic improvement was achieved compared to the previous campaign, with an overall negative bias persisting among the different observers. The calibration of observing times and the mitigation of timing errors should be important future considerations for observers and orbit computers, respectively.

Published
2023

8. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author

Ortiz, J. L., Santos-Sanz, P., Sicardy, B., Benedetti-Rossi, G., Brard, D., Morales, N., Duffard, R., Braga-Ribas, F., Hopp, U., Ries, C., Nascimbeni, V., Marzari, F., Granata, V., Pl, A., Kiss, C., Pribulla, T., Komk, R., Hornoch, K., Pravec, P., Bacci, P., Maestripieri, M., Nerli, L., Mazzei, L., Bachini, M., Martinelli, F., Succi, G., Ciabattari, F., Mikuz, H., Carbognani, A., Gaehrken, B., Mottola, S., Hellmich, S., Rommel, F. L., Fernndez-Valenzuela, E., Bagatin, A. Campo, Cikota, S., Cikota, A., Lecacheux, J., Vieira-Martins, R., Camargo, J. I. B., Assafin, M., Colas, F., Behrend, R., Desmars, J., Meza, E., Alvarez-Candal, A., Beisker, W., Gomes-Junior, A. R., Morgado, B. E., Roques, F., Vachier, F., Berthier, J., Mueller, T. G., Madiedo, J. M., Unsalan, O., Sonbas, E., Karaman, N., Erece, O., Koseoglu, D. T., Ozisik, T., Kalkan, S., Guney, Y., Niaei, M. S., Satir, O., Yesilyaprak, C., Puskullu, C., Kabas, A., Demircan, O., Alikakos, J., Charmandaris, V., Leto, G., Ohlert, J., Christille, J. M., Szakts, R., Farkas, A. Takcsn, Varga-Vereblyi, E., Marton, G., Marciniak, A., Bartczak, P., Santana-Ros, T., Butkiewicz-Bk, M., Dudziski, G., Al-Lagoa, V., Gazeas, K., Tzouganatos, L., Paschalis, N., Tsamis, V., Snchez-Lavega, A., Prez-Hoyos, S., Hueso, R., Guirado, J. C., Peris, V., and Iglesias-Marzoa, R.

Subjects
Minor planets -- Observations, Planetary rings -- Observations, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): J. L. Ortiz (corresponding author) [1]; P. Santos-Sanz [1]; B. Sicardy [2]; G. Benedetti-Rossi [3]; D. Brard [2]; N. Morales [1]; R. Duffard [1]; F. Braga-Ribas [3, 4]; U. [...]

Published
2017
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9. Comets beyond 4 au: How pristine are Oort nuclei?

Author

Fulle, Marco, primary, Lazzarin, M, additional, Forgia, F La, additional, Zakharov, V V, additional, Bertini, I, additional, Epifani, E Mazzotta, additional, Ammannito, E, additional, Buzzoni, A, additional, Capria, M T, additional, Carbognani, A, additional, Da Deppo, V, additional, Corte, V Della, additional, Fiscale, S, additional, Frattin, E, additional, Inno, L, additional, Migliorini, A, additional, Pernechele, C, additional, Rotundi, A, additional, Sindoni, G, additional, Tubiana, C, additional, Milani, G, additional, Aletti, A, additional, Bacci, P, additional, Baj, G, additional, Bellini, F, additional, Bryssinck, E, additional, Di Grazia, M, additional, Facchini, M, additional, Feraco, M, additional, Kugel, F, additional, Maestripieri, M, additional, Tirelli, D, additional, Valvasori, A, additional, Snodgrass, C, additional, and Jones, G H, additional

Published
2022
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10. Comets beyond 4 au: How pristine are Oort nuclei?

Author

FULLE, Marco, Lazzarin, M., La Forgia, F., Zakharov, V. V., Bertini, I., Epifani, E. Mazzotta, Ammannito, E., BUZZONI, Alberto, CAPRIA, MARIA TERESA, CARBOGNANI, Albino, Da Deppo, V., Corte, V. Della, Fiscale, S., Frattin, E., INNO, LAURA, MIGLIORINI, Alessandra, PERNECHELE, Claudio, Rotundi, Alessandra, Sindoni, G., Tubiana, C., Milani, G., Aletti, A., Bacci, P., Baj, G., Bellini, F., Bryssinck, E., Di Grazia, M., Facchini, M., Feraco, M., Guido, E., Ligustri, R., Kugel, F., Maestripieri, M., Tirelli, D., Valvasori, A., Snodgrass, C., and Jones, G. H.

Subjects
Space and Planetary Science, space vehicles, Oort Cloud, Astronomy and Astrophysics, protoplanetary discs, general [comets]
Abstract

The ESA mission Comet Interceptor will target an Oort or interstellar comet during its first approach to the Sun. Meanwhile, the Vera Rubin LSST Survey will observe hundreds of active comets per month beyond 4 au from the Sun, where water vapor pressure is expected to be too low to eject dust. We discuss observations of dust tails at heliocentric distances larger than 4 au in order to retrieve the physical parameters driving cometary activity beyond Jupiter by means of a probabilistic tail model, which is consistent with the activity model defining the gas coma parameters due to the sublimation of carbon monoxide, molecular oxygen, methane, ethane and carbon dioxide since the activity onset at 85 au from the Sun. We find that: (i) All the observed dust tails are consistent with the adopted activity model; (ii) The tail fits depend on three free parameters only, all correlated to the nucleus size; (iii) Tail fits are always improved by anisotropic dust ejection, suggesting activity of Oort nuclei dominated by seasons; (iv) Inbound seasons suggest cometary activity before the ejection of protocomets into the Oort cloud, as predicted by the activity model; (v) Oort nuclei larger than 1 km may be characterized by a fallout up to ≈100 m thick deposited during ≈60 yr inbound; (vi) On the other side, Oort nuclei smaller than 1 km may appear more pristine than Jupiter Family Comets when observed at 1 au from the Sun.

Published
2022

12. The large trans-Neptunian object 2002 TC302 from combined stellar occultation, photometry, and astrometry data

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Investigación Informática, Ortiz Moreno, José Luis, Santos Sanz, Pablo, Sicardy, B., Benedetti-Rossi, G., Duffard, René, Morales Palomino, Nicolás, Braga-Ribas, F., Fernández-Valenzuela, Estela, Nascimbeni, V., Nardiello, D., Carbognani, A., Buzzi, Luca, Aletti, A., Bacci, P., Maestripieri, M., Mazzei, L., Mikuz, H., Skvarc, J., Ciabattari, F., Lavalade, F., Scarfi, G., Mari, J.M., Conjat, M., Sposetti, S., Bachini, M., Succi, G., Mancini, F., Alighieri, M., Dal Canto, E., Masucci, M., Vara-Lubiano, M., Gutiérrez, P.J., Desmars, Josselin, Lecacheux, J., Vieira-Martins, R., Camargo, J.I.B., Assafin, M., Colas, François, Beisker, W., Behrend, Raoul, Mueller, T.G., Meza, E., Gomes-Junior, A.R., Roques, F., Vachier, Frédéric, Mottola, S., Hellmich, S., Campo Bagatin, Adriano, Alvarez-Candal, Alvaro, Cikota, S., Cikota, A., Christille, J.M., Pál, András, Kiss, C., Pribulla, T., Komžík, R., Madiedo, J.M., Charmandaris, V., Alikakos, J., Szakáts, Róbert, Farkas, Anikó, Varga-Verebélyi, E., Marton, G., Marciniak, Anna, Bartczak, Przemyslaw, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Alí-Lagoa, Víctor, Gazeas, K., Paschalis, N., Tsamis, V., Guirado, J.C., Peris, V., Iglesias-Marzoa, R., Schnabel, C., Manzano, F., Navarro, A., Perelló, C., Vecchione, A., Noschese, A., Morrone, L., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Investigación Informática, Ortiz Moreno, José Luis, Santos Sanz, Pablo, Sicardy, B., Benedetti-Rossi, G., Duffard, René, Morales Palomino, Nicolás, Braga-Ribas, F., Fernández-Valenzuela, Estela, Nascimbeni, V., Nardiello, D., Carbognani, A., Buzzi, Luca, Aletti, A., Bacci, P., Maestripieri, M., Mazzei, L., Mikuz, H., Skvarc, J., Ciabattari, F., Lavalade, F., Scarfi, G., Mari, J.M., Conjat, M., Sposetti, S., Bachini, M., Succi, G., Mancini, F., Alighieri, M., Dal Canto, E., Masucci, M., Vara-Lubiano, M., Gutiérrez, P.J., Desmars, Josselin, Lecacheux, J., Vieira-Martins, R., Camargo, J.I.B., Assafin, M., Colas, François, Beisker, W., Behrend, Raoul, Mueller, T.G., Meza, E., Gomes-Junior, A.R., Roques, F., Vachier, Frédéric, Mottola, S., Hellmich, S., Campo Bagatin, Adriano, Alvarez-Candal, Alvaro, Cikota, S., Cikota, A., Christille, J.M., Pál, András, Kiss, C., Pribulla, T., Komžík, R., Madiedo, J.M., Charmandaris, V., Alikakos, J., Szakáts, Róbert, Farkas, Anikó, Varga-Verebélyi, E., Marton, G., Marciniak, Anna, Bartczak, Przemyslaw, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Alí-Lagoa, Víctor, Gazeas, K., Paschalis, N., Tsamis, V., Guirado, J.C., Peris, V., Iglesias-Marzoa, R., Schnabel, C., Manzano, F., Navarro, A., Perelló, C., Vecchione, A., Noschese, A., and Morrone, L.

Abstract

Context. Deriving physical properties of trans-Neptunian objects is important for the understanding of our Solar System. This requires observational efforts and the development of techniques suitable for these studies. Aims. Our aim is to characterize the large trans-Neptunian object (TNO) 2002 TC302. Methods. Stellar occultations offer unique opportunities to determine key physical properties of TNOs. On 28 January 2018, 2002 TC302 occulted a mv ~ 15.3 star with designation 593-005847 in the UCAC4 stellar catalog, corresponding to Gaia source 130957813463146112. Twelve positive occultation chords were obtained from Italy, France, Slovenia, and Switzerland. Also, four negative detections were obtained near the north and south limbs. This represents the best observed stellar occultation by a TNO other than Pluto in terms of the number of chords published thus far. From the 12 chords, an accurate elliptical fit to the instantaneous projection of the body can be obtained that is compatible with the near misses. Results. The resulting ellipse has major and minor axes of 543 ± 18 km and 460 ± 11 km, respectively, with a position angle of 3 ± 1 degrees for the minor axis. This information, combined with rotational light curves obtained with the 1.5 m telescope at Sierra Nevada Observatory and the 1.23 m telescope at Calar Alto observatory, allows us to derive possible three-dimensional shapes and density estimations for the body based on hydrostatic equilibrium assumptions. The effective diameter in equivalent area is around 84 km smaller than the radiometrically derived diameter using thermal data from Herschel and Spitzer Space Telescopes. This might indicate the existence of an unresolved satellite of up to ~300 km in diameter, which is required to account for all the thermal flux, although the occultation and thermal diameters are compatible within their error bars given the considerable uncertainty of the thermal results. The existence of a potential satellite also a

Published
2020

13. The large trans-Neptunian object 2002 TC302from combined stellar occultation, photometry, and astrometry data

Author

Ortiz, J. L., primary, Santos-Sanz, P., additional, Sicardy, B., additional, Benedetti-Rossi, G., additional, Duffard, R., additional, Morales, N., additional, Braga-Ribas, F., additional, Fernández-Valenzuela, E., additional, Nascimbeni, V., additional, Nardiello, D., additional, Carbognani, A., additional, Buzzi, L., additional, Aletti, A., additional, Bacci, P., additional, Maestripieri, M., additional, Mazzei, L., additional, Mikuz, H., additional, Skvarc, J., additional, Ciabattari, F., additional, Lavalade, F., additional, Scarfi, G., additional, Mari, J. M., additional, Conjat, M., additional, Sposetti, S., additional, Bachini, M., additional, Succi, G., additional, Mancini, F., additional, Alighieri, M., additional, Dal Canto, E., additional, Masucci, M., additional, Vara-Lubiano, M., additional, Gutiérrez, P. J., additional, Desmars, J., additional, Lecacheux, J., additional, Vieira-Martins, R., additional, Camargo, J. I. B., additional, Assafin, M., additional, Colas, F., additional, Beisker, W., additional, Behrend, R., additional, Mueller, T. G., additional, Meza, E., additional, Gomes-Junior, A. R., additional, Roques, F., additional, Vachier, F., additional, Mottola, S., additional, Hellmich, S., additional, Campo Bagatin, A., additional, Alvarez-Candal, A., additional, Cikota, S., additional, Cikota, A., additional, Christille, J. M., additional, Pál, A., additional, Kiss, C., additional, Pribulla, T., additional, Komžík, R., additional, Madiedo, J. M., additional, Charmandaris, V., additional, Alikakos, J., additional, Szakáts, R., additional, Farkas-Takács, A., additional, Varga-Verebélyi, E., additional, Marton, G., additional, Marciniak, A., additional, Bartczak, P., additional, Butkiewicz-Ba̧k, M., additional, Dudziński, G., additional, Alí-Lagoa, V., additional, Gazeas, K., additional, Paschalis, N., additional, Tsamis, V., additional, Guirado, J. C., additional, Peris, V., additional, Iglesias-Marzoa, R., additional, Schnabel, C., additional, Manzano, F., additional, Navarro, A., additional, Perelló, C., additional, Vecchione, A., additional, Noschese, A., additional, and Morrone, L., additional

Published
2020
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14. Dust Environment Model of the Interstellar Comet 2I/Borisov

Author

Cremonese, G., primary, Fulle, M., additional, Cambianica, P., additional, Munaretto, G., additional, Capria, M. T., additional, Forgia, F. La, additional, Lazzarin, M., additional, Migliorini, A., additional, Boschin, W., additional, Milani, G., additional, Aletti, A., additional, Arlic, G., additional, Bacci, P., additional, Bacci, R., additional, Bryssinck, E., additional, Carosati, D., additional, Castellano, D., additional, Buzzi, L., additional, Rubbo, S. Di, additional, Facchini, M., additional, Guido, E., additional, Kugel, F., additional, Ligustri, R., additional, Maestripieri, M., additional, Mantero, A., additional, Nicolas, J., additional, Ochner, P., additional, Perrella, C., additional, Trabatti, R., additional, and Valvasori, A., additional

Published
2020
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15. 2017 OH7

Author

Laux, U., Stecklum, B., Bacci, P., Maestripieri, M., Carotta, M., Tesi, L., Fagioli, G., Bonomi, R., Jaeger, M., Prosperi, E., Vollmann, W., Spoto, F., Dennefeld, M., Thuillot, W., Bouquillon, S., Taris, F., Carlucci, T., Barache, C., Fumagalli, A., Sicoli, P., Testa, A., Balam, D. D., Wiggins, P., Ikari, Y., Gilio, R., Ponzio, F., Gallotti, R., Belmonte, A., Carbognani, A., Camarasa, J., Hidas, A., Hug, G., Fornas, G., Carreno, A., Birtwhistle, P., Tinella, V., Nicolini Astronomical Robotic Observatory, N. A. R. O., Sárneczky, K., Ordasi, A., Hudin, L., Denneau, L., Heinze, A., Weiland, H., Stalder, B., Tonry, J., Jacques, C., Pimentel, E., Barros, J., Wells, G., Leuty, J., Bamberger, D., Thüringer Landessternwarte Tautenburg (TLS), Laboratoire de Mécanique, Modélisation et Procédés Propres (M2P2), Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Department of Computer Science [Verona] (UNIVR | DI), University of Verona (UNIVR), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Auckland [Auckland], Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVDA), Laboratoire d'Ingénierie des Matériaux (LIM), Centre National de la Recherche Scientifique (CNRS), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Laboratoire de l'Accélérateur Linéaire (LAL), and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Available from the Minor Planet Center.

Published
2017

16. Observations and Orbits of Comets

Author

Kulichenko, N., Pomazan, A. V., Maigurova, N. V., Bodryagin, D. V., Bacci, P., Maestripieri, M., Tesi, L., Fagioli, G., Bonomi, R., Facchini, M., Coffano, A., Marinello, W., Micheli, M., Pizzetti, G., Soffiantini, A., Cernis, K., Haver, R., Gorelli, R., Piazzolla, L. M., Jaeger, M., Prosperi, E., Prosperi, S., Vollmann, W., Wiebe, Y., Kaiser, G., Puccini, S., Buriev, A. M., Ibrohimov, A. A., Safarov, A. G., Ayubov, D. K., Asoev, H. G., Foglia, S., Galli, G., Naves, R., Campas, M., Hasubick, W., Scotti, J. V., Altieri, B., Bouy, H., Verdoes-Kleijn, G., Carry, B., Kadota, K., Abe, H., Seki, T., Sato, H., Rodríguez, D., Ionescu, D., Christie, G. W., Natusch, T., Gilmore, A. C., Kilmartin, P. M., Meech, K. J., Kleyna, J., Woodworth, D., Kashuba, V., Troianskyi, V., Kashuba, S., Baransky, A., Tochonyy, V., Gunko, N., Pogrebtsov, N., Radomskiy, V., Ruban, E., Pavluk, Y., Kurginian, E., Ershov, D., Zadorozhny, O., Kasyanchuk, A., Bakaieva, O., Shevchuk, D., Bondar, D., Pais, T., Smolynec, V., Balam, D. D., Tubbiolo, A. F., Leonard, G. J., Matheny, R. G., Kowalski, R. A., Fuls, D. C., Johnson, J. A., Christensen, E. J., Gibbs, A. R., Grauer, A. D., Larson, S. M., Seaman, R. L., Shelly, F. C., Moritz, N., Childs, W., Ikari, Y., Masi, G., Schwartz, M., Holvorcem, P., Dupouy, P., de Vanssay, J. B., James, N., Soulier, J.-F., Aymami, J. M., Camarasa, J., Linder, J., Montoro, L., Bosch, J. M., Bryssinck, E., Diepvens, A., Shurpakov, S., Gao, X. Liao X., Liao, X., Lindner, P., Dangl, G., Mainzer, A. K., Bauer, J. M., Grav, T., Masiero, J. R., Dailey, J. W., Cutri, R. M., Wright, E. L., Nugent, C., Sonnett, S., Kramer, E., Gaitan, J., Tremosa, L., Zhao, H. B., Li, B., Zhaori, G., Hong, R. Q., Hu, L. F., Lu, H., Tan, H. J., Ohshima, Y., Barona Felgosa, L., Belli, L., Bilhaj, M., Bosse, M., Schmidt, M., Breitenstein, P., Mccormick, J., Carstens, R., Drummond, J., Bulger, J., Goggia, T., Lowe, T., Schultz, A., Willman, M., Chambers, K., Chastel, S., Denneau, L., Flewelling, H., Huber, M., Lilly, E., Magnier, E., Wainscoat, R., Waters, C., Weryk, R., Pei, W., Hambsch, F.-J., Hambsch, J., Lutkenhoner, B., Paul, N., Gasparovic, G., Chen, Y., Cox, P., Betzler, A. S., Sherrod, P. C., Sherrod, L. P., Bell, C., Peterson, H., Chapman, A., Sparrenberger, M., Gonzalez, J., Hills, K., Benavides, R., Carson, P., Morales, M., Gerhard, C., Fichtl, R., Haeusler, B., Ditz, P., Hudin, L., Sugawara, K., Nohara, H., Buzzi, L., Concari, P., Cremaschini, C., Tombelli, M., Tilley, S. M., van Buitenen, G., Dymock, R., Camilleri, P., Williams, H., Heinze, A., Weiland, H., Stalder, B., Tonry, J., Sherstyuk, A., Rowe, B., Wilde, D., Flynn, R. L., Allen, L., Trilling, D., James, D., Herrera, D., Fuentes, C., Rajagopal, J., Axelrod, T., Valdes, F., Lipunov, V., Podesta, R., Gorbovskoy, E., Tiurina, N., Balanutsa, P., Kuznetsov, A., Kornilov, V., Chazov, V., Lopez, C., Podesta, F., Levato, H., Saffe, C., Maury, A., Vanssay, J. B., Noël, T., Sandness, B., Maur, A., Jacques, C., Pimentel, E., Barros, J., Acosta, A., Sofia, A., Silvia, A., Jackson, F., Limon, F., Farf, R., Wells, G., Bamberger, D., Williams, G. V., and Pomies, Marie-Paule

Subjects
[SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

Available from the Minor Planet Center.

Published
2017

17. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author

Ortiz, J.L. Santos-Sanz, P. Sicardy, B. Benedetti-Rossi, G. Bérard, D. Morales, N. Duffard, R. Braga-Ribas, F. Hopp, U. Ries, C. Nascimbeni, V. Marzari, F. Granata, V. Pál, A. Kiss, C. Pribulla, T. Komžík, R. Hornoch, K. Pravec, P. Bacci, P. Maestripieri, M. Nerli, L. Mazzei, L. Bachini, M. Martinelli, F. Succi, G. Ciabattari, F. Mikuz, H. Carbognani, A. Gaehrken, B. Mottola, S. Hellmich, S. Rommel, F.L. Fernández-Valenzuela, E. Bagatin, A.C. Cikota, S. Cikota, A. Lecacheux, J. Vieira-Martins, R. Camargo, J.I.B. Assafin, M. Colas, F. Behrend, R. Desmars, J. Meza, E. Alvarez-Candal, A. Beisker, W. Gomes, A.R. Morgado, B.E. Roques, F. Vachier, F. Berthier, J. Mueller, T.G. Madiedo, J.M. Unsalan, O. Sonbas, E. Karaman, N. Erece, O. Koseoglu, D.T. Ozisik, T. Kalkan, S. Guney, Y. Niaei, M.S. Satir, O. Yesilyaprak, C. Puskullu, C. Kabas, A. Demircan, O. Alikakos, J. Charmandaris, V. Leto, G. Ohlert, J. Christille, J.M. Szakáts, R. Farkas, A.T. Varga-Verebélyi, E. Marton, G. Marciniak, A. Bartczak, P. Santana-Ros, T. Butkiewicz-Bak, M. Dudzinski, G. Alí-Lagoa, V. Gazeas, K. Tzouganatos, L. Paschalis, N. Tsamis, V. Sánchez-Lavega, A. Pérez-Hoyos, S. Hueso, R. Guirado, J.C. Peris, V. Iglesias-Marzoa, R.

Abstract

Haumea-one of the four known trans-Neptunian dwarf planets- is a very elongated and rapidly rotating body1-3. In contrast to other dwarf planets4-6, its size, shape, albedo and density are not well constrained. The Centaur Chariklo was the first body other than a giant planet known to have a ring system7, and the Centaur Chiron was later found to possess something similar to Chariklo's rings8,9. Here we report observations from multiple Earth-based observatories of Haumea passing in front of a distant star (a multichord stellar occultation). Secondary events observed around the main body of Haumea are consistent with the presence of a ring with an opacity of 0.5, width of 70 kilometres and radius of about 2,287 kilometres. The ring is coplanar with both Haumea's equator and the orbit of its satellite Hi'iaka. The radius of the ring places it close to the 3:1 mean-motion resonance with Haumea's spin period-that is, Haumea rotates three times on its axis in the time that a ring particle completes one revolution. The occultation by the main body provides an instantaneous elliptical projected shape with axes of about 1,704 kilometres and 1,138 kilometres. Combined with rotational light curves, the occultation constrains the three-dimensional orientation of Haumea and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea's largest axis is at least 2,322 kilometres, larger than previously thought, implying an upper limit for its density of 1,885 kilograms per cubic metre and a geometric albedo of 0.51, both smaller than previous estimates1,10,11. In addition, this estimate of the density of Haumea is closer to that of Pluto than are previous estimates, in line with expectations. No global nitrogen- or methane-dominated atmosphere was detected. © 2017 Macmillan Publishers Limited, part of Springer Nature. All rights reserved.

Published
2017

18. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Ortiz Moreno, José Luis, Santos Sanz, Pablo, Sicardy, B., Benedetti-Rossi, G., Bérard, D., Morales Palomino, Nicolás, Duffard, René, Braga-Ribas, F., Hopp, U., Ries, C., Nascimbeni, V., Marzari, F., Granata, V., Pál, András, Kiss, C., Pribulla, T., Komžík, R., Hornoch, K., Pravec, Petr, Bacci, P., Maestripieri, M., Nerli, L., Mazzei, L., Bachini, M., Martinelli, F., Succi, G., Ciabattari, F., Mikuz, H., Carbognani, A., Gaehrken, B., Mottola, S., Hellmich, S., Rommel, F.L., Fernández-Valenzuela, Estela, Campo Bagatin, Adriano, Cikota, S., Cikota, A., Lecacheux, J., Vieira-Martins, R., Camargo, J.I.B., Assafin, M., Colas, François, Behrend, Raoul, Desmars, Josselin, Meza, E., Alvarez-Candal, Alvaro, Beisker, W., Gomes-Junior, A.R., Morgado, B.E., Roques, F., Vachier, Frédéric, Berthier, Jérôme, Mueller, T.G., Madiedo, J.M., Unsalan, O., Sonbas, E., Karaman, N., Erece, O., Koseoglu, D.T., Ozisik, T., Kalkan, S., Guney, Y., Niaei, M.S., Satir, O., Yesilyaprak, C., Puskullu, C., Kabas, A., Demircan, O., Alikakos, J., Charmandaris, V., Leto, G., Ohlert, J., Christille, J.M., Szakáts, Róbert, Takácsné Farkas, A., Varga-Verebélyi, E., Marton, G., Marciniak, Anna, Bartczak, Przemyslaw, Santana-Ros, Toni, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Alí-Lagoa, Víctor, Gazeas, K., Tzouganatos, L., Paschalis, N., Tsamis, V., Sánchez-Lavega, A., Pérez-Hoyos, S., Hueso, R., Guirado, J.C., Peris, V., Iglesias-Marzoa, R., Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Ortiz Moreno, José Luis, Santos Sanz, Pablo, Sicardy, B., Benedetti-Rossi, G., Bérard, D., Morales Palomino, Nicolás, Duffard, René, Braga-Ribas, F., Hopp, U., Ries, C., Nascimbeni, V., Marzari, F., Granata, V., Pál, András, Kiss, C., Pribulla, T., Komžík, R., Hornoch, K., Pravec, Petr, Bacci, P., Maestripieri, M., Nerli, L., Mazzei, L., Bachini, M., Martinelli, F., Succi, G., Ciabattari, F., Mikuz, H., Carbognani, A., Gaehrken, B., Mottola, S., Hellmich, S., Rommel, F.L., Fernández-Valenzuela, Estela, Campo Bagatin, Adriano, Cikota, S., Cikota, A., Lecacheux, J., Vieira-Martins, R., Camargo, J.I.B., Assafin, M., Colas, François, Behrend, Raoul, Desmars, Josselin, Meza, E., Alvarez-Candal, Alvaro, Beisker, W., Gomes-Junior, A.R., Morgado, B.E., Roques, F., Vachier, Frédéric, Berthier, Jérôme, Mueller, T.G., Madiedo, J.M., Unsalan, O., Sonbas, E., Karaman, N., Erece, O., Koseoglu, D.T., Ozisik, T., Kalkan, S., Guney, Y., Niaei, M.S., Satir, O., Yesilyaprak, C., Puskullu, C., Kabas, A., Demircan, O., Alikakos, J., Charmandaris, V., Leto, G., Ohlert, J., Christille, J.M., Szakáts, Róbert, Takácsné Farkas, A., Varga-Verebélyi, E., Marton, G., Marciniak, Anna, Bartczak, Przemyslaw, Santana-Ros, Toni, Butkiewicz-Bąk, Magdalena, Dudziński, Grzegorz, Alí-Lagoa, Víctor, Gazeas, K., Tzouganatos, L., Paschalis, N., Tsamis, V., Sánchez-Lavega, A., Pérez-Hoyos, S., Hueso, R., Guirado, J.C., Peris, V., and Iglesias-Marzoa, R.

Abstract

Haumea—one of the four known trans-Neptunian dwarf planets—is a very elongated and rapidly rotating body1, 2, 3. In contrast to other dwarf planets4, 5, 6, its size, shape, albedo and density are not well constrained. The Centaur Chariklo was the first body other than a giant planet known to have a ring system7, and the Centaur Chiron was later found to possess something similar to Chariklo’s rings8, 9. Here we report observations from multiple Earth-based observatories of Haumea passing in front of a distant star (a multi-chord stellar occultation). Secondary events observed around the main body of Haumea are consistent with the presence of a ring with an opacity of 0.5, width of 70 kilometres and radius of about 2,287 kilometres. The ring is coplanar with both Haumea’s equator and the orbit of its satellite Hi’iaka. The radius of the ring places it close to the 3:1 mean-motion resonance with Haumea’s spin period—that is, Haumea rotates three times on its axis in the time that a ring particle completes one revolution. The occultation by the main body provides an instantaneous elliptical projected shape with axes of about 1,704 kilometres and 1,138 kilometres. Combined with rotational light curves, the occultation constrains the three-dimensional orientation of Haumea and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea’s largest axis is at least 2,322 kilometres, larger than previously thought, implying an upper limit for its density of 1,885 kilograms per cubic metre and a geometric albedo of 0.51, both smaller than previous estimates1, 10, 11. In addition, this estimate of the density of Haumea is closer to that of Pluto than are previous estimates, in line with expectations. No global nitrogen- or methane-dominated atmosphere was detected.

Published
2017

21. Functional-orthopaedic therapy and cranial base: induced changes, utopia or reality?

Author

Maestripieri, M., Passaleva, S., Patanè, B., Cozzani, P., and Giorgetti, R.

Abstract

This study was conducted to ascertain the cranial base angle changes in skeletal Class II patients following functional-orthopaedic therapy. The cranial base flexure was measured by Ba-S-N angle. In this longitudinal study 246 patients were included; 120 male and 126 female, aged from 8 to 13 years. The study examined the following groups of patients: (A) control group of 48 Class II untreated patients, (B) control group of 26 untreated Class III patients, (C) Andreasen activator treated group of 44 Class II subjects, (D) 39 Class II patients treated with a cervical pull headgear generating orthopedic forces, (E) 31 FR2 treated patients, (F) group of 10 patients treated with rapid maxillary expansion, (G) Delaire face mask group of 31 subjects with skeletal Class III, (H) 17 Class III patients treated with rapid maxillary expansion. The pre- and post-treatment values were compared for normodivergent, hypodivergent and hyperdivergent skeletal patterns. It was found that the Ba-S-N was reduced in the maxillary expansion and FR2 treated normodivergent subjects.


Il presente lavoro ha voluto valutare le modifiche dell'angolazioe della base del cranio a seguito di un trattamento ortopedico - funzionale attraverso la misurazione dell'angolo BaSN.

Lo studio è stato condotto su di un campione di 246 soggetti, 120 maschi e 126 femmine di età compresa tra 8 e 13 anni. Il campione è stato suddiviso non solo in base al tipo di trattamento praticato, ma anche in base allla classe scheletrica attraverso l'angolo ANB. Si sono costituiti I seguenti gruppi: (A) gruppo controllo di pazienti non trattati costituito da 48 soggetti in II classe, (B) gruppo controllo di pazienti non trattati costituito da 48 soggetti in III classe, (C) gruppo trattato con attivatore di Andresen di 44 soggetti in II classe, (D) gruppo trattato con trazione cervicale con l'applicazione di forze ortopediche costituito da 39 soggetti in II classe (E) gruppo trattato con Frankel di tipo 2 costituito da 31 soggetti in II classe (F) gruppo trattato con disgiuntore rapido del palato di 10 soggetti in II classe, (G) gruppo trattato con maschera di Delaire costituito da 31 soggetti in III classe (H) gruppo trattato con disgiuntore rapido costituito da 17 soggetti in classe III.

Le variazioni rilevate a carico dell'angolo BaSN hanno evidenziato una riduzione statisticamente significativa di tale valore sia nei soggetto normodivergenti di classe II trattati con Frankel 2 che nel gruppo di soggetti normodivergenti di classe II trattati con disgiuntore rapido.

Published
2002
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24. [Diagnostic evaluation of the soft tissue profile].

Author

Nannelli P, Maestripieri M, and Verciani A

Subjects
Adult, Humans, Cephalometry methods, Face anatomy & histology, Malocclusion diagnosis
Abstract

The Authors report a cephalometric analysis of soft tissues profile to help the orthodontist to do a correct treatment plane referred to the three thirds of the face and not limited to the lower one only. This analysis is related to adult patients, and because the well known considerations about development of the soft tissues, it should be a predictable analysis of soft tissues profile at the end of growth.

Published
1990

25. [Magnets and orthognathodontics. Biological-clinical overview. 1].

Author

Maestripieri M, Giorgetti R, Nocchi L, and Nannelli P

Subjects
Orthodontic Appliances, Osteogenesis, Wound Healing, Magnetics
Abstract

A review of the physical properties of the magnetic fields is reported. Particular attention has been paid to the biological and clinical aspects of the electromagnetic fields applied to living structures of cells and bone tissue both susceptible to this exposition.

Published
1989

26. [Extrusive therapy and periodontal alignment. Considerations and indications. 2].

Author

Nannelli P, Maestripieri M, Verciani A, and Calandriello B

Subjects
Adult, Crowns, Female, Humans, Male, Malocclusion therapy, Orthodontic Appliances, Periodontal Diseases complications, Tooth Fractures complications, Tooth Fractures therapy, Periodontal Diseases therapy, Tooth Movement Techniques
Abstract

The Authors report some clinical cases treated with orthodontic forced eruption, periodontal surgery and prosthetic rehabilitation. The theoretic first part of this work was published on Dental Cadmos no. 9/87.

Published
1989

28. [Oral respiration. Diagnosis and physiopathology].

Author

Pallassini A, Maestripieri M, Mannelli A, Sandroni F, and Chicco G

Subjects
Child, Humans, Maxillofacial Development, Palatal Expansion Technique, Malocclusion etiology, Mouth Breathing complications
Abstract

The oral breathing can change the functional connections during the development of the facial bones of the children. All this causes an abnormal growth of the facial bones and of the dental structures. This work developed a new discipline to remove this problem.

Published
1989

29. [Magnets and orthodontics. Biological-clinical study. 2].

Author

Maestripieri M, Giorgetti R, Nannelli P, and Nocchi L

Subjects
Adolescent, Biomechanical Phenomena, Equipment Design, Extraoral Traction Appliances, Female, Humans, Male, Malocclusion therapy, Magnetics, Orthodontic Appliances
Abstract

The authors after preliminary remarks on new magnetic alloys, stress some biomechanic aspects related to distalization of upper molars. Radiologic examination of teeth during distalization shows a good rate of crown/tooth ratio movement. Where magnets were worn in combination with extraoral traction, they seemed to be more effective on the "test" sides rather than on the "control" sides where only extraoral forces acted.

Published
1989

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