10 results on '"Kretlow M"'
Number of results to display per page
Search Results
2. A dense ring of the trans-Neptunian object Quaoar outside its Roche limit
- Author
-
Morgado, B. E., Sicardy, B., Braga-Ribas, F., Ortiz, J. L., Salo, H., Vachier, F., Desmars, J., Pereira, C. L., Santos-Sanz, P., Sfair, R., de Santana, T., Assafin, M., Vieira-Martins, R., Gomes-Júnior, A. R., Margoti, G., Dhillon, V. S., Fernández-Valenzuela, E., Broughton, J., Bradshaw, J., Langersek, R., Benedetti-Rossi, G., Souami, D., Holler, B. J., Kretlow, M., Boufleur, R. C., Camargo, J. I. B., Duffard, R., Beisker, W., Morales, N., Lecacheux, J., Rommel, F. L., Herald, D., Benz, W., Jehin, E., Jankowsky, F., Marsh, T. R., Littlefair, S. P., Bruno, G., Pagano, I., Brandeker, A., Collier-Cameron, A., Florén, H. G., Hara, N., Olofsson, G., Wilson, T. G., Benkhaldoun, Z., Busuttil, R., Burdanov, A., Ferrais, M., Gault, D., Gillon, M., Hanna, W., Kerr, S., Kolb, U., Nosworthy, P., Sebastian, D., Snodgrass, C., Teng, J. P., and de Wit, J.
- Published
- 2023
- Full Text
- View/download PDF
3. The stellar occultation by (319) Leona on 2023 September 13 in preparation for the occultation of Betelgeuse.
- Author
-
Ortiz, J L, Kretlow, M, Schnabel, C, Morales, N, Flores-Martín, J, Sánchez González, M, Casarramona, F, Selva, A, Perelló, C, Román-Reche, A, Alonso, S, Rizos, J L, Gonçalves, R, Castillo, A, Madiedo, J M, Martínez Sánchez, P, Fernández Andújar, J M, Maestre, J L, Smith, E, and Gil, M
- Subjects
- *
OCCULTATIONS (Astronomy) , *LIGHT curves , *SMALL solar system bodies , *TIME series analysis , *ASTEROIDS , *ORBITS (Astronomy) , *PHOTOMETRY - Abstract
On 2023 December 12, the star α Orionis will be occulted by asteroid (319) Leona. This represents an extraordinary and unique opportunity to analyse the brightness distribution of Betelgeuse's photosphere with extreme angular resolution by studying light curves from different points on Earth and at different wavelengths. Here we present observations of another occultation by asteroid Leona, on 2023 September 13, whose goal was to determine Leona's projected shape and size in preparation for the December 12th event and its interpretation. The occultation campaign was highly successful with 25 positive detections from 17 different sites and a near miss. The effective diameter in projected area derived from the positive detections was 66 ± 2 km using an elliptical fit to the instantaneous limb. The body is highly elongated, with dimensions of 79.6 ± 2.2 km × 54.8 ± 1.3 km in its long and short axis, respectively, at occultation time. This result, in combination with dense time series photometry of Leona that we recently obtained, together with archival sparse photometry, allowed us to predict the angular size of the asteroid for the Betelgeuse event and to simulate the expected brightness change. Also, an accurate position coming from the occultation is provided, to improve the orbit of Leona. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
4. A dense ring of the trans-Neptunian object Quaoar outside its Roche limit
- Author
-
Morgado, B E, Sicardy, B, Braga-Ribas, F, Ortiz, J L, Salo, H, Vachier, F, Desmars, J, Pereira, C L, Santos-Sanz, P, Sfair, R, de Santana, T, Assafin, M, Vieira-Martins, R, Gomes-Júnior, A R, Margoti, G, Dhillon, V S, Fernández-Valenzuela, E, Broughton, J, Bradshaw, J, Langersek, R, Benedetti-Rossi, G, Souami, D, Holler, B J, Kretlow, M, Boufleur, R C, Camargo, J I B, Duffard, R, Beisker, W, Morales, N, Lecacheux, J, Rommel, F L, Herald, D, Benz, Willy, Jehin, E, Jankowsky, F, Marsh, T R, Littlefair, S P, Bruno, G, Pagano, I, Brandeker, A, Collier-Cameron, A, Florén, H G, Hara, N, Olofsson, G, Wilson, T G, Benkhaldoun, Z, Busuttil, R, Burdanov, A, Ferrais, M, Gault, D, Gillon, M, Hanna, W, Kerr, S, Kolb, U, Nosworthy, P, Sebastian, D, Snodgrass, C, Teng, J P, de Wit, J, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Polytechnique des Sciences Avancées (IPSA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. St Andrews Centre for Exoplanet Science, University of St Andrews. School of Physics and Astronomy, Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Research Council, European Commission, and Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil)
- Subjects
MCC ,QC Physics ,Multidisciplinary ,[SDU]Sciences of the Universe [physics] ,QB Astronomy ,520 Astronomie ,3rd-DAS ,530 Physik ,AC ,QC ,QB - Abstract
Full list of authors: Morgado, B. E.; Sicardy, B.; Braga-Ribas, F.; Ortiz, J. L.; Salo, H.; Vachier, F.; Desmars, J.; Pereira, C. L.; Santos-Sanz, P.; Sfair, R.; de Santana, T.; Assafin, M.; Vieira-Martins, R.; Gomes-Junior, A. R.; Margoti, G.; Dhillon, V. S.; Fernandez-Valenzuela, E.; Broughton, J.; Bradshaw, J.; Langersek, R.; Benedetti-Rossi, G.; Souami, D.; Holler, B. J.; Kretlow, M.; Boufleur, R. C.; Camargo, J. I. B.; Duffard, R.; Beisker, W.; Morales, N.; Lecacheux, J.; Rommel, F. L.; Herald, D.; Benz, W.; Jehin, E.; Jankowsky, F.; Marsh, T. R.; Littlefair, S. P.; Bruno, G.; Pagano, I.; Brandeker, A.; Collier-Cameron, A.; Floren, H. G.; Hara, N.; Olofsson, G.; Wilson, T. G.; Benkhaldoun, Z.; Busuttil, R.; Burdanov, A.; Ferrais, M.; Gault, D.; Gillon, M.; Hanna, W.; Kerr, S.; Kolb, U.; Nosworthy, P.; Sebastian, D.; Snodgrass, C.; Teng, J. P.; de Wit, J., Planetary rings are observed not only around giant planets1, but also around small bodies such as the Centaur Chariklo2 and the dwarf planet Haumea3. Up to now, all known dense rings were located close enough to their parent bodies, being inside the Roche limit, where tidal forces prevent material with reasonable densities from aggregating into a satellite. Here we report observations of an inhomogeneous ring around the trans-Neptunian body (50000) Quaoar. This trans-Neptunian object has an estimated radius4 of 555 km and possesses a roughly 80-km satellite5 (Weywot) that orbits at 24 Quaoar radii6,7. The detected ring orbits at 7.4 radii from the central body, which is well outside Quaoar’s classical Roche limit, thus indicating that this limit does not always determine where ring material can survive. Our local collisional simulations show that elastic collisions, based on laboratory experiments8, can maintain a ring far away from the body. Moreover, Quaoar’s ring orbits close to the 1/3 spin–orbit resonance9 with Quaoar, a property shared by Chariklo’s2,10,11 and Haumea’s3 rings, suggesting that this resonance plays a key role in ring confinement for small bodies. © 2023, The Author(s), under exclusive licence to Springer Nature Limited., This work was carried out under the Lucky Star umbrella that agglomerates the efforts of the Paris, Granada and Rio teams, which is funded by the ERC under the European Community’s H2020 (ERC grant agreement no. 669416). Part of the results were obtained using CHEOPS data. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden and the UK. The CHEOPS Consortium gratefully acknowledge the support received by all the agencies, offices, universities and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. The design and construction of HiPERCAM was supported by the ERC under the European Union’s Seventh Framework Programme (FP/2007-2013) under ERC-2013-ADG grant agreement no. 340040 (HiPERCAM). HiPERCAM operations and V.S.D. are funded by the Science and Technology Facilities Council (grant no. ST/V000853/1). The GTC is installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. This work has made use of data from the ESA mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). This study was financed in part by the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant no. 465376/2014-2). This study was financed in part by CAPES - Finance Code 001. The following authors acknowledge the respective (1) CNPq grants to B.E.M. no. 150612/2020-6; F.B.-R. no. 314772/2020-0; R.V.-M. no. 307368/2021-1; M.A. nos. 427700/2018-3, 310683/2017-3 and 473002/2013-2; and J.I.B.C. nos. 308150/2016-3 and 305917/2019-6. (2) CAPES/Cofecub grant to B.E.M. no. 394/2016-05. (3) FAPERJ grant no. M.A. E-26/111.488/2013. (4) FAPESP (Fundação de Amparo à Pesquisa do Estado de São Paulo) grants to A.R.G.-J. no. 2018/11239-8 and R.S. no. 2016/24561-0. (5) CAPES-PrInt Program grant to G.B.-R. no. 88887.310463/2018-00, mobility number 88887.571156/2020-00. (6) DFG (the German Research Foundation) grant to R.S. no. 446102036. P.S-S. and R.D. acknowledge financial support by the Spanish grant no. AYA-RTI2018-098657-J-I00 ‘LEO-SBNAF’ (MCIU/AEI/FEDER, UE). J.L.O., P.S-S., R.D. and N.M. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award for the Instituto de Astrofísica de Andalucía (grant no. SEV-2017-0709), and they also acknowledge the financial support by the Spanish grant nos. AYA-2017-84637-R and PID2020-112789GB-I00, and the Proyectos de Excelencia de la Junta de Andalucía grant nos. 2012-FQM1776 and PY20-01309. G.B-R. and I.P. acknowledge support from CHEOPS ASI-INAF agreement no. 2019-29-HH.0. A.B. was supported by the SNSA. A.C.-C. and T.G.W. acknowledge support from STFC consolidated grant nos. ST/R000824/1 and ST/V000861/1, and UK Space Agency grant no. ST/R003203/1. U.K. and R.B. acknowledge support by The OpenSTEM Laboratories, an initiative funded by the Higher Education Funding Council for England and the Wolfson Foundation. J.W. gratefully acknowledges financial support from the Heising-Simons Foundation, C. Masson and P. A. Gilman for Artemis, the first telescope of the SPECULOOS network situated in Tenerife, Spain. The ULiege’s contribution to SPECULOOS has received funding from the ERC under the European Union’s Seventh Framework Programme (FP/2007-2013) (grant agreement no. 336480/SPECULOOS), from the Balzan Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant no. T.0109.20), from the University of Liege and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientique (F.R.S.-FNRS) under grant no. PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E.J. is FNRS Senior Research Associate., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).
- Published
- 2023
5. VizieR Online Data Catalog: Triton light curves from 05/10/2017 (Marques Oliveira+, 2022)
- Author
-
Marques Oliveira, J., Sicardy, B., Gomes-Junior, A. R., Ortiz, J. L., Strobel, D. F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Berard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos-Sanz, P., Morales, N., Duffard, R., Fernandez-Valenzuela, E., Castro-Tirado, A. J., Braga-Ribas, F., Morgado, B. E., Assafin, M., Camargo, J. I. B., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Filho, S., Banda-Huarca, M. V., Quispe-Huaynasi, F., Pereira, C. L., Rommel, F. L., Margoti, G., Dias-Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, R., Perez-Hoyos, S., Sanchez-Lavega, A., Rojas, J. F., Beisker, W., Kretlow, M., Herald, D., Gault, D., Bath, K.-L., Bode, H.-J., Bredner, E., Guhl, K., Haymes, T. V., Hummel, E., Kattentidt, B., Klos, O., Pratt, A., Thome, B., Avdellidou, C., Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A. A., Xilouris, E. M., Alikakos, I., Gourzelas, A., Liakos, A., Charmandaris, V., Jelinek, M., Strobl, J., Eberle, A., Rapp, K., Gahrken, B., Kowo Llik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, D., Brandis, L., Puetz, I., Perdelwitz, V., Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J.-M., Ciabattari, F., Di, Luca R., Alboresi, D., Leto, G., Zanmar Sanchez, R., Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, C., Lo Savio, R., Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., Gallego, S., Tortorelli, L., Sposetti, S., Sussenbach, J., van den Abbeel, F., Andre, P., Llibre, M., Pailler, F., Ardissone, J., Boutet, M., Sanchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J. L., Dechambre, O., Delay, P., Delcroix, M., Rousselot, L., Ferreira, J., Machado, P., Tanga, P., Rivet, J.-P., Frappa, E., Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A. N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, J.-F., Metz, F., Erpelding, D., Nougayrede, P., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Baba Aissa, D., Grigahcene, Z., Briggs, D., Broadbent, S., Denyer, P., Haigh, N. J., Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., Talbot, J., Alonso, S., Roman Reche, A., Casanova, V., Briggs, E., Iglesias-Marzoa, R., Abril Ibanez, J., Diaz, Martin M. C., Gonzalez, H., Maestre Garcia, J. L., Marchant, J., Ordonez-Etxeberria, I., Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perello, C., Cabedo, V., Goncalves, R., Ferreira, M., Marques Dias, F., Daassou, A., Barkaoui, K., Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., El Moutamid, M., Lamarche, C., Pollock, J. T., Caton, D. B., Kouprianov, V., Timerson, B. W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J.-P., Francoise, J., Mondon, B., Payet, T., Boissel, C., Castets, M., Hubbard, W. B., Hill, R., Reitsema, H. J., Mousis, O., Ball, L., Hutcheon, S., Lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., Downs, B., Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
Photometry ,Planets ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Solar system - Abstract
International audience; The data provided features all light curves from the 5 October 2017 event. The names of the files are the same names, in lower caps and with no spaces, that are presented in Figures C.1 and C.2. The first column of all files is the time in seconds, starting on 5 October 2017 00:00:00 UTC. The second column of all files is the normalised flux, where the unocculted flux oscillates around 1. (2 data files).
- Published
- 2022
6. Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations
- Author
-
Marques Oliveira, J. Sicardy, B. Gomes-Júnior, A.R. Ortiz, J.L. Strobel, D.F. Bertrand, T. Forget, F. Lellouch, E. Desmars, J. Bérard, D. Doressoundiram, A. Lecacheux, J. Leiva, R. Meza, E. Roques, F. Souami, D. Widemann, T. Santos-Sanz, P. Morales, N. Duffard, R. Fernández-Valenzuela, E. Castro-Tirado, A.J. Braga-Ribas, F. Morgado, B.E. Assafin, M. Camargo, J.I.B. Vieira-Martins, R. Benedetti-Rossi, G. Santos-Filho, S. Banda-Huarca, M.V. Quispe-Huaynasi, F. Pereira, C.L. Rommel, F.L. Margoti, G. Dias-Oliveira, A. Colas, F. Berthier, J. Renner, S. Hueso, R. Pérez-Hoyos, S. Sánchez-Lavega, A. Rojas, J.F. Beisker, W. Kretlow, M. Herald, D. Gault, D. Bath, K.-L. Bode, H.-J. Bredner, E. Guhl, K. Haymes, T.V. Hummel, E. Kattentidt, B. Klös, O. Pratt, A. Thome, B. Avdellidou, C. Gazeas, K. Karampotsiou, E. Tzouganatos, L. Kardasis, E. Christou, A.A. Xilouris, E.M. Alikakos, I. Gourzelas, A. Liakos, A. Charmandaris, V. Jelínek, M. Štrobl, J. Eberle, A. Rapp, K. Gährken, B. Klemt, B. Kowollik, S. Bitzer, R. Miller, M. Herzogenrath, G. Frangenberg, D. Brandis, L. Pütz, I. Perdelwitz, V. Piehler, G.M. Riepe, P. Von Poschinger, K. Baruffetti, P. Cenadelli, D. Christille, J.-M. Ciabattari, F. Di Luca, R. Alboresi, D. Leto, G. Zanmar Sanchez, R. Bruno, P. Occhipinti, G. Morrone, L. Cupolino, L. Noschese, A. Vecchione, A. Scalia, C. Lo Savio, R. Giardina, G. Kamoun, S. Barbosa, R. Behrend, R. Spano, M. Bouchet, E. Cottier, M. Falco, L. Gallego, S. Tortorelli, L. Sposetti, S. Sussenbach, J. Van Den Abbeel, F. André, P. Llibre, M. Pailler, F. Ardissone, J. Boutet, M. Sanchez, J. Bretton, M. Cailleau, A. Pic, V. Granier, L. Chauvet, R. Conjat, M. Dauvergne, J.L. Dechambre, O. Delay, P. Delcroix, M. Rousselot, L. Ferreira, J. MacHado, P. Tanga, P. Rivet, J.-P. Frappa, E. Irzyk, M. Jabet, F. Kaschinski, M. Klotz, A. Rieugnie, Y. Klotz, A.N. Labrevoir, O. Lavandier, D. Walliang, D. Leroy, A. Bouley, S. Lisciandra, S. Coliac, J.-F. Metz, F. Erpelding, D. Nougayrède, P. Midavaine, T. Miniou, M. Moindrot, S. Morel, P. Reginato, B. Reginato, E. Rudelle, J. Tregon, B. Tanguy, R. David, J. Thuillot, W. Hestroffer, D. Vaudescal, G. Baba Aissa, D. Grigahcene, Z. Briggs, D. Broadbent, S. Denyer, P. Haigh, N.J. Quinn, N. Thurston, G. Fossey, S.J. Arena, C. Jennings, M. Talbot, J. Alonso, S. Román Reche, A. Casanova, V. Briggs, E. Iglesias-Marzoa, R. Abril Ibáñez, J. Díaz Martín, M.C. González, H. Maestre García, J.L. Marchant, J. Ordonez-Etxeberria, I. Martorell, P. Salamero, J. Organero, F. Ana, L. Fonseca, F. Peris, V. Brevia, O. Selva, A. Perello, C. Cabedo, V. Gonçalves, R. Ferreira, M. Marques Dias, F. Daassou, A. Barkaoui, K. Benkhaldoun, Z. Guennoun, M. Chouqar, J. Jehin, E. Rinner, C. Lloyd, J. El Moutamid, M. Lamarche, C. Pollock, J.T. Caton, D.B. Kouprianov, V. Timerson, B.W. Blanchard, G. Payet, B. Peyrot, A. Teng-Chuen-Yu, J.-P. Françoise, J. Mondon, B. Payet, T. Boissel, C. Castets, M. Hubbard, W.B. Hill, R. Reitsema, H.J. Mousis, O. Ball, L. Neilsen, G. Hutcheon, S. Lay, K. Anderson, P. Moy, M. Jonsen, M. Pink, I. Walters, R. Downs, B.
- Abstract
Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range ∼8 km to ∼190 km, corresponding to pressure levels from 9 μbar down to a few nanobars. Results. (i) A pressure of 1.18 ± 0.03 μbar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 μbar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude. ©
- Published
- 2022
7. Pluto's lower atmosphere and pressure evolution from ground-based stellar occultations, 1988-2016
- Author
-
Meza, E, Sicardy, B, Assafin, M, Ortiz, JL, Bertrand, T, Lellouch, E, Desmars, J, Forget, F, Bérard, D, Doressoundiram, A, Lecacheux, J, Oliveira, JM, Roques, F, Widemann, T, Colas, F, Vachier, F, Renner, S, Leiva, R, Braga-Ribas, F, Benedetti-Rossi, G, Camargo, JIB, Dias-Oliveira, A, Morgado, B, Gomes-Júnior, AR, Vieira-Martins, R, Behrend, R, Tirado, AC, Duffard, R, Morales, N, Santos-Sanz, P, Jelínek, M, Cunniffe, R, Querel, R, Harnisch, M, Jansen, R, Pennell, A, Todd, S, Ivanov, VD, Opitom, C, Gillon, M, Jehin, E, Manfroid, J, Pollock, J, Reichart, DE, Haislip, JB, Ivarsen, KM, LaCluyze, AP, Maury, A, Gil-Hutton, R, Dhillon, V, Littlefair, S, Marsh, T, Veillet, C, Bath, K-L, Beisker, W, Bode, H-J, Kretlow, M, Herald, D, Gault, D, Kerr, S, Pavlov, H, Faragó, O, Klös, O, Frappa, E, Lavayssière, M, Cole, AA, Giles, AB, Greenhill, JG, Hill, KM, Buie, MW, Olkin, CB, Young, EF, Young, LA, Wasserman, LH, Devogèle, M, French, RG, Bianco, FB, Marchis, F, Brosch, N, Kaspi, S, Polishook, D, Manulis, I, Larbi, MAM, Benkhaldoun, Z, Daassou, A, Azhari, YE, Moulane, Y, Broughton, J, Milner, J, Dobosz, T, Bolt, G, Lade, B, Gilmore, A, Kilmartin, P, Allen, WH, Graham, PB, Loader, B, McKay, G, Talbot, J, Parker, S, Abe, L, Bendjoya, P, Rivet, J-P, Vernet, D, Fabrizio, LD, Lorenzi, V, Magazzù, A, Molinari, E, Gazeas, K, Tzouganatos, L, Carbognani, A, Bonnoli, G, Marchini, A, Leto, G, Sanchez, RZ, Mancini, L, Kattentidt, B, Dohrmann, M, Guhl, K, Rothe, W, Walzel, K, Wortmann, G, Eberle, A, Hampf, D, Ohlert, J, Krannich, G, Murawsky, G, Gährken, B, Gloistein, D, Alonso, S, Román, A, Communal, J-E, Jabet, F, Visscher, SD, Sérot, J, Janik, T, Moravec, Z, Machado, P, Selva, A, Perelló, C, Rovira, J, Conti, M, Papini, R, Salvaggio, F, Noschese, A, Tsamis, V, Tigani, K, Barroy, P, Irzyk, M, Neel, D, Godard, JP, Lanoiselée, D, Sogorb, P, Vérilhac, D, Bretton, M, Signoret, F, Ciabattari, F, Naves, R, Boutet, M, Queiroz, JD, Lindner, P, Lindner, K, Enskonatus, P, Dangl, G, Tordai, T, Eichler, H, Hattenbach, J, Peterson, C, Molnar, LA, and Howell, RR
- Subjects
Earth and Planetary Astrophysics (astro-ph.EP) ,FOS: Physical sciences ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Context. Pluto's tenuous nitrogen (N2) atmosphere undergoes strong seasonal effects due to high obliquity and orbital eccentricity, and has been recently (July 2015) observed by the New Horizons spacecraft. Goals are (i) construct a well calibrated record of the seasonal evolution of surface pressure on Pluto and (ii) constrain the structure of the lower atmosphere using a central flash observed in 2015. Method: eleven stellar occultations by Pluto observed between 2002 and 2016 are used to retrieve atmospheric profiles (density, pressure, temperature) between $\sim$5 km and $\sim$380 km altitude levels (i.e. pressures from about 10 microbar to 10 nanobar). Results: (i) Pressure has suffered a monotonic increase from 1988 to 2016, that is compared to a seasonal volatile transport model, from which tight constraints on a combination of albedo and emissivity of N2 ice are derived; (ii) A central flash observed on 2015 June 29 is consistent with New Horizons REX profiles, provided that (a) large diurnal temperature variations (not expected by current models) occur over Sputnik Planitia and/or (b) hazes with tangential optical depth of about 0.3 are present at 4-7 km altitude levels and/or (c) the nominal REX density values are overestimated by an implausibly large factor of about 20% and/or (d) higher terrains block part of the flash in the Charon facing hemisphere., 21 pages, 11 figures
- Published
- 2019
8. Lower atmosphere and pressure evolution on Pluto from ground-based stellar occultations, 1988-2016
- Author
-
Meza, E. Sicardy, B. Assafin, M. Ortiz, J.L. Bertrand, T. Lellouch, E. Desmars, J. Forget, F. Bérard, D. Doressoundiram, A. Lecacheux, J. Marques Oliveira, J. Roques, F. Widemann, T. Colas, F. Vachier, F. Renner, S. Leiva, R. Braga-Ribas, F. Benedetti-Rossi, G. Camargo, J.I.B. Dias-Oliveira, A. Morgado, B. Gomes-Júnior, A.R. Vieira-Martins, R. Behrend, R. Castro Tirado, A. Duffard, R. Morales, N. Santos-Sanz, P. Jelínek, M. Cunniffe, R. Querel, R. Harnisch, M. Jansen, R. Pennell, A. Todd, S. Ivanov, V.D. Opitom, C. Gillon, M. Jehin, E. Manfroid, J. Pollock, J. Reichart, D.E. Haislip, J.B. Ivarsen, K.M. LaCluyze, A.P. Maury, A. Gil-Hutton, R. Dhillon, V. Littlefair, S. Marsh, T. Veillet, C. Bath, K.-L. Beisker, W. Bode, H.-J. Kretlow, M. Herald, D. Gault, D. Kerr, S. Pavlov, H. Faragó, O. Klös, O. Frappa, E. Lavayssière, M. Cole, A.A. Giles, A.B. Greenhill, J.G. Hill, K.M. Buie, M.W. Olkin, C.B. Young, E.F. Young, L.A. Wasserman, L.H. Devogèle, M. French, R.G. Bianco, F.B. Marchis, F. Brosch, N. Kaspi, S. Polishook, D. Manulis, I. Ait Moulay Larbi, M. Benkhaldoun, Z. Daassou, A. El Azhari, Y. Moulane, Y. Broughton, J. Milner, J. Dobosz, T. Bolt, G. Lade, B. Gilmore, A. Kilmartin, P. Allen, W.H. Graham, P.B. Loader, B. McKay, G. Talbot, J. Parker, S. Abe, L. Bendjoya, P. Rivet, J.-P. Vernet, D. Di Fabrizio, L. Lorenzi, V. Magazzú, A. Molinari, E. Gazeas, K. Tzouganatos, L. Carbognani, A. Bonnoli, G. Marchini, A. Leto, G. Zanmar Sanchez, R. Mancini, L. Kattentidt, B. Dohrmann, M. Guhl, K. Rothe, W. Walzel, K. Wortmann, G. Eberle, A. Hampf, D. Ohlert, J. Krannich, G. Murawsky, G. Gährken, B. Gloistein, D. Alonso, S. Román, A. Communal, J.-E. Jabet, F. DeVisscher, S. Sérot, J. Janik, T. Moravec, Z. MacHado, P. Selva, A. Perelló, C. Rovira, J. Conti, M. Papini, R. Salvaggio, F. Noschese, A. Tsamis, V. Tigani, K. Barroy, P. Irzyk, M. Neel, D. Godard, J.P. Lanoiselée, D. Sogorb, P. Vérilhac, D. Bretton, M. Signoret, F. Ciabattari, F. Naves, R. Boutet, M. De Queiroz, J. Lindner, P. Lindner, K. Enskonatus, P. Dangl, G. Tordai, T. Eichler, H. Hattenbach, J. Peterson, C. Molnar, L.A. Howell, R.R.
- Abstract
Context. The tenuous nitrogen (N2) atmosphere on Pluto undergoes strong seasonal effects due to high obliquity and orbital eccentricity, and has recently (July 2015) been observed by the New Horizons spacecraft. Aims. The main goals of this study are (i) to construct a well calibrated record of the seasonal evolution of surface pressure on Pluto and (ii) to constrain the structure of the lower atmosphere using a central flash observed in 2015. Methods. Eleven stellar occultations by Pluto observed between 2002 and 2016 are used to retrieve atmospheric profiles (density, pressure, temperature) between altitude levels of ∼5 and ∼380 km (i.e. pressures from ∼10 μbar to 10 nbar). Results. (i) Pressure has suffered a monotonic increase from 1988 to 2016, that is compared to a seasonal volatile transport model, from which tight constraints on a combination of albedo and emissivity of N2 ice are derived. (ii) A central flash observed on 2015 June 29 is consistent with New Horizons REX profiles, provided that (a) large diurnal temperature variations (not expected by current models) occur over Sputnik Planitia; and/or (b) hazes with tangential optical depth of ∼0.3 are present at 4-7 km altitude levels; and/or (c) the nominal REX density values are overestimated by an implausibly large factor of ∼20%; and/or (d) higher terrains block part of the flash in the Charon facing hemisphere. © E. Meza et al. 2019.
- Published
- 2019
9. Large changes in Plutoʼs atmosphere as revealed by recent stellar occultations
- Author
-
Sicardy, B., Widemann, T., Lellouch, E., Veillet, C., Cuillandre, J.-C., Colas, F., Roques, F., Beisker, W., Kretlow, M., Lagrange, A.-M., Gendron, E., Lacombe, F., Lecacheux, J., Birnbaum, C., Fienga, A., Leyrat, C., Maury, A., Raynaud, E., Renner, S., Schultheis, M., Brooks, K., Delsanti, A., Hainaut, O. R., Gilmozzi, R., Lidman, C., Spyromilio, J., Rapaport, M., Rosenzweig, P., Naranjo, O., Porras, L., Díaz, F., Calderón, H., Carrillo, S., Carvajal, A., Recalde, E., Cavero, Gaviria L., Montalvo, C., Barría, D., Campos, R., Duffard, R., and Levato, H.
- Published
- 2003
10. The two Titan stellar occultations of 14 November 2003.
- Author
-
Sicardy, B., Colas, F., Widemann, T., Bellucci, A., Beisker, W., Kretlow, M., Ferri, F., Lacour, S., Lecacheux, J., Lellouch, E., Pau, S., Renner, S., Roques, F., Fienga, A., Etienne, C., Martinez, C., Glass, I. S., Baba, D., Nagayama, T., and Nagata, T.
- Published
- 2006
- Full Text
- View/download PDF
Catalog
Books, media, physical & digital resources
Discovery Service for Jio Institute Digital Library
For full access to our library's resources, please sign in.