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Your search keyword '"Kukita, R."' showing total 4 results
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4 results on '"Kukita, R."'

1. Constraints on Triton atmospheric evolution from occultations: 1989-2022

Author

Sicardy, B., Tej, A., Gomes-Junior, A. R., Romanov, F. D., Bertrand, T., Ashok, N. M., Lellouch, E., Morgado, B. E., Assafin, M., Desmars, J., Camargo, J. I. B., Kilic, Y., Ortiz, J. L., Vieira-Martins, R., Braga-Ribas, F., Ninan, J. P., Bhatt, B. C., Kumar, S. Pramod, Swain, V., Sharma, S., Saha, A., Ojha, D. K., Pawar, G., Deshmukh, S., Deshpande, A., Ganesh, S., Jain, J. K., Mathew, S. K., Kumar, H., Bhalerao, V., Anupama, G. C., Barway, S., Brandeker, A., Floren, H. G., Olofsson, G., Bruno, G., Mao, Y. M., Ye, R. H., Zou, Q. Y., Sun, Y. K., Shen, Y. Y., Zhao, J. Y., Grishin, D. N., Romanova, L. V., Marchis, F., Fukui, K., Kukita, R., Benedetti-Rossi, G., Santos-Sanz, P., Dhyani, N., Gokhale, A., Kate, A., Sicardy, B., Tej, A., Gomes-Junior, A. R., Romanov, F. D., Bertrand, T., Ashok, N. M., Lellouch, E., Morgado, B. E., Assafin, M., Desmars, J., Camargo, J. I. B., Kilic, Y., Ortiz, J. L., Vieira-Martins, R., Braga-Ribas, F., Ninan, J. P., Bhatt, B. C., Kumar, S. Pramod, Swain, V., Sharma, S., Saha, A., Ojha, D. K., Pawar, G., Deshmukh, S., Deshpande, A., Ganesh, S., Jain, J. K., Mathew, S. K., Kumar, H., Bhalerao, V., Anupama, G. C., Barway, S., Brandeker, A., Floren, H. G., Olofsson, G., Bruno, G., Mao, Y. M., Ye, R. H., Zou, Q. Y., Sun, Y. K., Shen, Y. Y., Zhao, J. Y., Grishin, D. N., Romanova, L. V., Marchis, F., Fukui, K., Kukita, R., Benedetti-Rossi, G., Santos-Sanz, P., Dhyani, N., Gokhale, A., and Kate, A.

Abstract

Context - Around the year 2000, Triton's south pole experienced an extreme summer solstice that occurs every about 650 years, when the subsolar latitude reached about 50{\deg}. Bracketing this epoch, a few occultations probed Triton's atmosphere in 1989, 1995, 1997, 2008 and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of Triton's atmospheric pressure which is presented here. Aims- The goal is to constrain the Volatile Transport Models (VTMs) of Triton's atmosphere that is basically in vapor pressure equilibrium with the nitrogen ice at its surface. Methods - Fits to the occultation light curves yield Triton's atmospheric pressure at the reference radius 1400 km, from which the surface pressure is induced. Results - The fits provide a pressure p_1400= 1.211 +/- 0.039 microbar at radius 1400 km (47 km altitude), from which a surface pressure of p_surf= 14.54 +/- 0.47 microbar is induced (1-sigma error bars). To within error bars, this is identical to the pressure derived from the previous occultation of 5 October 2017, p_1400 = 1.18 +/- 0.03 microbar and p_surf= 14.1 +/- 0.4 microbar, respectively. Based on recent models of Triton's volatile cycles, the overall evolution over the last 30 years of the surface pressure is consistent with N2 condensation taking place in the northern hemisphere. However, models typically predict a steady decrease in surface pressure for the period 2005-2060, which is not confirmed by this observation. Complex surface-atmosphere interactions, such as ice albedo runaway and formation of local N2 frosts in the equatorial regions of Triton could explain the relatively constant pressure between 2017 and 2022., Comment: 8 pages, 4 figures, accepted for publication in Astronomy and Astrophysics

Published
2024

2. Scaling slowly rotating asteroids by stellar occultations

Author

Marciniak, A., Ďurech, J., Choukroun, A., Hanuš, J., Ogłoza, W., Szakáts, R., Molnár, L., Pál, A., Monteiro, F., Frappa, E., Beisker, W., Pavlov, H., Moore, J., Adomavičienė, R., Aikawa, R., Andersson, S., Antonini, P., Argentin, Y., Asai, A., Assoignon, P., Barton, J., Baruffetti, P., Bath, K. L., Behrend, R., Benedyktowicz, L., Bernasconi, L., Biguet, G., Billiani, M., Błażewicz, D., Boninsegna, R., Borkowski, M., Bosch, J., Brazill, S., Bronikowska, M., Bruno, A., Bąk, M. Butkiewicz, Caron, J., Casalnuovo, G., Castellani, J. J., Ceravolo, P., Conjat, M., Delincak, P., Delpau, J., Demeautis, C., Demirkol, A., Dróżdż, M., Duffard, R., Durandet, C., Eisfeldt, D., Evangelista, M., Fauvaud, S., Fauvaud, M., Ferrais, M., Filipek, M., Fini, P., Fukui, K., Gährken, B., Geier, S., George, T., Goffin, B., Golonka, J., Goto, T., Grice, J., Guhl, K., Halíř, K., Hanna, W., Harman, M., Hashimoto, A., Hasubick, W., Higgins, D., Higuchi, M., Hirose, T., Hirsch, R., Hofschulz, O., Horaguchi, T., Horbowicz, J., Ida, M., Ignácz, B., Ishida, M., Isobe, K., Jehin, E., Joachimczyk, B., Jones, A., Juan, J., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kasebe, H., Kattentidt, B., Kim, D. -H., Kim, M. -J., Kitazaki, K., Klotz, A., Komraus, M., Konstanciak, I., Tóth, R. Könyves, Kouno, K., Kowald, E., Krajewski, J., Krannich, G., Kreutzer, A., Kryszczyńska, A., Kubánek, J., Kudak, V., Kugel, F., Kukita, R., Kulczak, P., Lazzaro, D., Licandro, J., Livet, F., Maley, P., Manago, N., Mánek, J., Manna, A., Matsushita, H., Meister, S., Mesquita, W., Messner, S., Michelet, J., Michimani, J., Mieczkowska, I., Morales, N., Motyliński, M., Murawiecka, M., Newman, J., Nikitin, V., Nishimura, M., Oey, J., Oszkiewicz, D., Owada, M., Pakštienė, E., Pawłowski, M., Pereira, W., Perig, V., Perła, J., Pilcher, F., Podlewska-Gaca, E., Polák, J., Polakis, T., Polińska, M., Popowicz, A., Richard, F., Rives, J. J., Rodrigues, T., Rogiński, Ł., Rondón, E., Rottenborn, M., Schäfer, R., Schnabel, C., Schreurs, O., Selva, A., Simon, M., Skiff, B., Skrutskie, M., Skrzypek, J., Sobkowiak, K., Sonbas, E., Sposetti, S., Stuart, P., Szyszka, K., Terakubo, K., Thomas, W., Trela, P., Uchiyama, S., Urbanik, M., Vaudescal, G., Venable, R., Watanabe, Ha., Watanabe, Hi., Winiarski, M., Wróblewski, R., Yamamura, H., Yamashita, M., Yoshihara, H., Zawilski, M., Zelený, P., Żejmo, M., Żukowski, K., Żywica, S., Marciniak, A., Ďurech, J., Choukroun, A., Hanuš, J., Ogłoza, W., Szakáts, R., Molnár, L., Pál, A., Monteiro, F., Frappa, E., Beisker, W., Pavlov, H., Moore, J., Adomavičienė, R., Aikawa, R., Andersson, S., Antonini, P., Argentin, Y., Asai, A., Assoignon, P., Barton, J., Baruffetti, P., Bath, K. L., Behrend, R., Benedyktowicz, L., Bernasconi, L., Biguet, G., Billiani, M., Błażewicz, D., Boninsegna, R., Borkowski, M., Bosch, J., Brazill, S., Bronikowska, M., Bruno, A., Bąk, M. Butkiewicz, Caron, J., Casalnuovo, G., Castellani, J. J., Ceravolo, P., Conjat, M., Delincak, P., Delpau, J., Demeautis, C., Demirkol, A., Dróżdż, M., Duffard, R., Durandet, C., Eisfeldt, D., Evangelista, M., Fauvaud, S., Fauvaud, M., Ferrais, M., Filipek, M., Fini, P., Fukui, K., Gährken, B., Geier, S., George, T., Goffin, B., Golonka, J., Goto, T., Grice, J., Guhl, K., Halíř, K., Hanna, W., Harman, M., Hashimoto, A., Hasubick, W., Higgins, D., Higuchi, M., Hirose, T., Hirsch, R., Hofschulz, O., Horaguchi, T., Horbowicz, J., Ida, M., Ignácz, B., Ishida, M., Isobe, K., Jehin, E., Joachimczyk, B., Jones, A., Juan, J., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kasebe, H., Kattentidt, B., Kim, D. -H., Kim, M. -J., Kitazaki, K., Klotz, A., Komraus, M., Konstanciak, I., Tóth, R. Könyves, Kouno, K., Kowald, E., Krajewski, J., Krannich, G., Kreutzer, A., Kryszczyńska, A., Kubánek, J., Kudak, V., Kugel, F., Kukita, R., Kulczak, P., Lazzaro, D., Licandro, J., Livet, F., Maley, P., Manago, N., Mánek, J., Manna, A., Matsushita, H., Meister, S., Mesquita, W., Messner, S., Michelet, J., Michimani, J., Mieczkowska, I., Morales, N., Motyliński, M., Murawiecka, M., Newman, J., Nikitin, V., Nishimura, M., Oey, J., Oszkiewicz, D., Owada, M., Pakštienė, E., Pawłowski, M., Pereira, W., Perig, V., Perła, J., Pilcher, F., Podlewska-Gaca, E., Polák, J., Polakis, T., Polińska, M., Popowicz, A., Richard, F., Rives, J. J., Rodrigues, T., Rogiński, Ł., Rondón, E., Rottenborn, M., Schäfer, R., Schnabel, C., Schreurs, O., Selva, A., Simon, M., Skiff, B., Skrutskie, M., Skrzypek, J., Sobkowiak, K., Sonbas, E., Sposetti, S., Stuart, P., Szyszka, K., Terakubo, K., Thomas, W., Trela, P., Uchiyama, S., Urbanik, M., Vaudescal, G., Venable, R., Watanabe, Ha., Watanabe, Hi., Winiarski, M., Wróblewski, R., Yamamura, H., Yamashita, M., Yoshihara, H., Zawilski, M., Zelený, P., Żejmo, M., Żukowski, K., and Żywica, S.

Abstract

As evidenced by recent survey results, majority of asteroids are slow rotators (P>12 h), but lack spin and shape models due to selection bias. This bias is skewing our overall understanding of the spins, shapes, and sizes of asteroids, as well as of their other properties. Also, diameter determinations for large (>60km) and medium-sized asteroids (between 30 and 60 km) often vary by over 30% for multiple reasons. Our long-term project is focused on a few tens of slow rotators with periods of up to 60 hours. We aim to obtain their full light curves and reconstruct their spins and shapes. We also precisely scale the models, typically with an accuracy of a few percent. We used wide sets of dense light curves for spin and shape reconstructions via light-curve inversion. Precisely scaling them with thermal data was not possible here because of poor infrared data: large bodies are too bright for WISE mission. Therefore, we recently launched a campaign among stellar occultation observers, to scale these models and to verify the shape solutions, often allowing us to break the mirror pole ambiguity. The presented scheme resulted in shape models for 16 slow rotators, most of them for the first time. Fitting them to stellar occultations resolved previous inconsistencies in size determinations. For around half of the targets, this fitting also allowed us to identify a clearly preferred pole solution, thus removing the ambiguity inherent to light-curve inversion. We also address the influence of the uncertainty of the shape models on the derived diameters. Overall, our project has already provided reliable models for around 50 slow rotators. Such well-determined and scaled asteroid shapes will, e.g. constitute a solid basis for density determinations when coupled with mass information. Spin and shape models continue to fill the gaps caused by various biases., Comment: Accepted to Astronomy & Astrophysics. 12 pages + appendices

Published
2023
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3. Citizen Science Astronomy with a Network of Small Telescope: The Launch and Deployment of JWST

Author

Lambert, R. A., Marchis, F., F., Asencio, J., Blaclard, G., Sgro, L. A., Giorgini, J. D., Plavchan, P., White, T., Verveen, A., Goto, T., Kuossari, P., Sethu, N., Loose, M. A., Will, S., Sibbernsen, K., Pickering, J. W., Randolph, J., Fukui, K., Huet, P., Guillet, B., Clerget, O., Stahl, S., Yoblonsky, N., Lauvernier, M., Matsumura, T., Yamato, M., Laugier, J. M., Brodt-Vilain, O., Espudo, A., Kukita, R., Iida, S., Kardel, S., Green, D., Tikkanen, P., Douvas, A., Billiani, M., Knight, G., Ryno, M., Simard, G., Knight, R., Primm, M., Wildhagen, B., Poncet, J., Frachon, T., Shimizu, M., Jackson, A., Parker, B., Redfern, G., Nikiforov, P., Friday, E., Lincoln, K., Sweitzer, J., Mitsuoka, R., Cabral, K., Katterfeld, A., Fairfax, M., Lambert, R. A., Marchis, F., F., Asencio, J., Blaclard, G., Sgro, L. A., Giorgini, J. D., Plavchan, P., White, T., Verveen, A., Goto, T., Kuossari, P., Sethu, N., Loose, M. A., Will, S., Sibbernsen, K., Pickering, J. W., Randolph, J., Fukui, K., Huet, P., Guillet, B., Clerget, O., Stahl, S., Yoblonsky, N., Lauvernier, M., Matsumura, T., Yamato, M., Laugier, J. M., Brodt-Vilain, O., Espudo, A., Kukita, R., Iida, S., Kardel, S., Green, D., Tikkanen, P., Douvas, A., Billiani, M., Knight, G., Ryno, M., Simard, G., Knight, R., Primm, M., Wildhagen, B., Poncet, J., Frachon, T., Shimizu, M., Jackson, A., Parker, B., Redfern, G., Nikiforov, P., Friday, E., Lincoln, K., Sweitzer, J., Mitsuoka, R., Cabral, K., Katterfeld, A., and Fairfax, M.

Abstract

We present a coordinated campaign of observations to monitor the brightness of the James Webb Space Telescope (JWST) as it travels toward the second Earth-Sun Lagrange point and unfolds using the network ofUnistellar digital telescopes. Those observations collected by citizen astronomers across the world allowed us to detect specific phases such as the separation from the booster, glare due to a change of orientation after a maneuver, the unfurling of the sunshield, and deployment of the primary mirror. After deployment of the sunshield on January 6 2022, the 6-h lightcurve has a significant amplitude and shows small variations due to the artificial rotation of the space telescope during commissionning. These variations could be due to the deployment of the primary mirror or some changes in orientation of the space telescope. This work illustrates the power of a worldwide array of small telescopes, operated by citizen astronomers, to conduct large scientific campaigns over a long timeframe. In the future, our network and others will continue to monitor JWST to detect potential degradations to the space environment by comparing the evolution of the lightcurve., Comment: 15 pages, 13 figures and 2 tables, SPIE Ground-based and Airborne Telescopes IX, AS22 SPIE Astronomical Telescopes + Instrumentation, 12182-144

Published
2022

4. Scaling slowly rotating asteroids with stellar occultations

Author

Marciniak, A., Ďurech, J., Choukroun, A., Hanuš, J., Ogłoza, W., Szakáts, R., Molnár, L., Pál, A., Monteiro, F., Frappa, E., Beisker, W., Pavlov, H., Moore, J., Adomavičienė, R., Aikawa, R., Andersson, S., Antonini, P., Argentin, Y., Asai, A., Assoignon, P., Barton, J., Baruffetti, P., Bath, K. L., Behrend, R., Benedyktowicz, L., Bernasconi, L., Biguet, G., Billiani, M., Błażewicz, D., Boninsegna, R., Borkowski, M., Bosch, J., Brazill, S., Bronikowska, M., Bruno, A., Butkiewicz-Bąk, M., Caron, J., Casalnuovo, G., Castellani, J. J., Ceravolo, P., Conjat, M., Delincak, P., Delpau, J., Demeautis, C., Demirkol, A., Dróżdż, M., Duffard, R., Durandet, C., Eisfeldt, D., Evangelista, M., Fauvaud, S., Fauvaud, M., Ferrais, M., Filipek, M., Fini, P., Fukui, K., Gährken, B., Geier, S., George, T., Goffin, B., Golonka, J., Goto, T., Grice, J., Guhl, K., Halíř, K., Hanna, W., Harman, M., Hashimoto, A., Hasubick, W., Higgins, D., Higuchi, M., Hirose, T., Hirsch, R., Hofschulz, O., Horaguchi, T., Horbowicz, J., Ida, M., Ignácz, B., Ishida, M., Isobe, K., Jehin, E., Joachimczyk, B., Jones, A., Juan, J., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kasebe, H., Kattentidt, B., Kim, D.-H., Kim, M.-J., Kitazaki, K., Klotz, A., Komraus, M., Konstanciak, I., Könyves-Tóth, R., Kouno, K., Kowald, E., Krajewski, J., Krannich, G., Kreutzer, A., Kryszczyńska, A., Kubánek, J., Kudak, V., Kugel, F., Kukita, R., Kulczak, P., Lazzaro, D., Licandro, J., Livet, F., Maley, P., Manago, N., Mánek, J., Manna, A., Matsushita, H., Meister, S., Mesquita, W., Messner, S., Michelet, J., Michimani, J., Mieczkowska, I., Morales, N., Motyliński, M., Murawiecka, M., Newman, J., Nikitin, V., Nishimura, M., Oey, J., Oszkiewicz, D., Owada, M., Pakštienė, E., Pawłowski, M., Pereira, W., Perig, V., Perła, J., Pilcher, F., Podlewska-Gaca, E., Polák, J., Polakis, T., Polińska, M., Popowicz, A., Richard, F., Rives, J. J, Rodrigues, T., Rogiński, Ł., Rondón, E., Rottenborn, M., Schäfer, R., Schnabel, C., Schreurs, O., Selva, A., Simon, M., Skiff, B., Skrutskie, M., Skrzypek, J., Sobkowiak, K., Sonbas, E., Sposetti, S., Stuart, P., Szyszka, K., Terakubo, K., Thomas, W., Trela, P., Uchiyama, S., Urbanik, M., Vaudescal, G., Venable, R., Watanabe, Ha., Watanabe, Hi., Winiarski, M., Wróblewski, R., Yamamura, H., Yamashita, M., Yoshihara, H., Zawilski, M., Zelený, P., Żejmo, M., Żukowski, K., Żywica, S., Marciniak, A., Ďurech, J., Choukroun, A., Hanuš, J., Ogłoza, W., Szakáts, R., Molnár, L., Pál, A., Monteiro, F., Frappa, E., Beisker, W., Pavlov, H., Moore, J., Adomavičienė, R., Aikawa, R., Andersson, S., Antonini, P., Argentin, Y., Asai, A., Assoignon, P., Barton, J., Baruffetti, P., Bath, K. L., Behrend, R., Benedyktowicz, L., Bernasconi, L., Biguet, G., Billiani, M., Błażewicz, D., Boninsegna, R., Borkowski, M., Bosch, J., Brazill, S., Bronikowska, M., Bruno, A., Butkiewicz-Bąk, M., Caron, J., Casalnuovo, G., Castellani, J. J., Ceravolo, P., Conjat, M., Delincak, P., Delpau, J., Demeautis, C., Demirkol, A., Dróżdż, M., Duffard, R., Durandet, C., Eisfeldt, D., Evangelista, M., Fauvaud, S., Fauvaud, M., Ferrais, M., Filipek, M., Fini, P., Fukui, K., Gährken, B., Geier, S., George, T., Goffin, B., Golonka, J., Goto, T., Grice, J., Guhl, K., Halíř, K., Hanna, W., Harman, M., Hashimoto, A., Hasubick, W., Higgins, D., Higuchi, M., Hirose, T., Hirsch, R., Hofschulz, O., Horaguchi, T., Horbowicz, J., Ida, M., Ignácz, B., Ishida, M., Isobe, K., Jehin, E., Joachimczyk, B., Jones, A., Juan, J., Kamiński, K., Kamińska, M. K., Kankiewicz, P., Kasebe, H., Kattentidt, B., Kim, D.-H., Kim, M.-J., Kitazaki, K., Klotz, A., Komraus, M., Konstanciak, I., Könyves-Tóth, R., Kouno, K., Kowald, E., Krajewski, J., Krannich, G., Kreutzer, A., Kryszczyńska, A., Kubánek, J., Kudak, V., Kugel, F., Kukita, R., Kulczak, P., Lazzaro, D., Licandro, J., Livet, F., Maley, P., Manago, N., Mánek, J., Manna, A., Matsushita, H., Meister, S., Mesquita, W., Messner, S., Michelet, J., Michimani, J., Mieczkowska, I., Morales, N., Motyliński, M., Murawiecka, M., Newman, J., Nikitin, V., Nishimura, M., Oey, J., Oszkiewicz, D., Owada, M., Pakštienė, E., Pawłowski, M., Pereira, W., Perig, V., Perła, J., Pilcher, F., Podlewska-Gaca, E., Polák, J., Polakis, T., Polińska, M., Popowicz, A., Richard, F., Rives, J. J, Rodrigues, T., Rogiński, Ł., Rondón, E., Rottenborn, M., Schäfer, R., Schnabel, C., Schreurs, O., Selva, A., Simon, M., Skiff, B., Skrutskie, M., Skrzypek, J., Sobkowiak, K., Sonbas, E., Sposetti, S., Stuart, P., Szyszka, K., Terakubo, K., Thomas, W., Trela, P., Uchiyama, S., Urbanik, M., Vaudescal, G., Venable, R., Watanabe, Ha., Watanabe, Hi., Winiarski, M., Wróblewski, R., Yamamura, H., Yamashita, M., Yoshihara, H., Zawilski, M., Zelený, P., Żejmo, M., Żukowski, K., and Żywica, S.

Abstract

Context. As evidenced by recent survey results, the majority of asteroids are slow rotators (spin periods longer than 12 h), but lack spin and shape models because of selection bias. This bias is skewing our overall understanding of the spins, shapes, and sizes of asteroids, as well as of their other properties. Also, diameter determinations for large (>60 km) and medium-sized asteroids (between 30 and 60 km) often vary by over 30% for multiple reasons. Aims. Our long-term project is focused on a few tens of slow rotators with periods of up to 60 h. We aim to obtain their full light curves and reconstruct their spins and shapes. We also precisely scale the models, typically with an accuracy of a few percent. Methods. We used wide sets of dense light curves for spin and shape reconstructions via light-curve inversion. Precisely scaling them with thermal data was not possible here because of poor infrared datasets: large bodies tend to saturate in WISE mission detectors. Therefore, we recently also launched a special campaign among stellar occultation observers, both in order to scale these models and to verify the shape solutions, often allowing us to break the mirror pole ambiguity. Results. The presented scheme resulted in shape models for 16 slow rotators, most of them for the first time. Fitting them to chords from stellar occultation timings resolved previous inconsistencies in size determinations. For around half of the targets, this fitting also allowed us to identify a clearly preferred pole solution from the pair of two mirror pole solutions, thus removing the ambiguity inherent to light-curve inversion. We also address the influence of the uncertainty of the shape models on the derived diameters. Conclusions. Overall, our project has already provided reliable models for around 50 slow rotators. Such well-determined and scaled asteroid shapes will, for example, constitute a solid basis fo

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