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2. CoRoT’s first seven planets: An overview

Author

Barge P., Lammer H., Schneider J., Dvorak R., and Wuchterl G.

Subjects
Physics, QC1-999
Abstract

The up to 150 day uninterrupted high-precision photometry of about 100000 stars – provided so far by the exoplanet channel of the CoRoT space telescope – gave a new perspective on the planet population of our galactic neighbourhood. The seven planets with very accurate parameters widen the range of known planet properties in almost any respect. Giant planets have been detected at low metallicity, rapidly rotating and active, spotted stars. CoRoT-3 populated the brown dwarf desert and closed the gap of measured physical properties between standard giant planets and very low mass stars. CoRoT extended the known range of planet masses down-to 5 Earth masses and up to 21 Jupiter masses, the radii to less than 2 Earth radii and up to the most inflated hot Jupiter found so far, and the periods of planets discovered by transits to 9 days. Two CoRoT planets have host stars with the lowest content of heavy elements known to show a transit hinting towards a different planet-host-star-metallicity relation then the one found by radial-velocity search programs. Finally the properties of the CoRoT-7b prove that terrestrial planets with a density close to Earth exist outside the Solar System. The detection of the secondary transit of CoRoT-1 at the 10−5-level and the very clear detection of the 1.7 Earth radii of CoRoT-7b at 3.5 10−4 relative flux are promising evidence of CoRoT being able to detect even smaller, Earth sized planets.

Published
2011
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4. Inner southern magnetosphere observation of Mercury via SERENA ion sensors in BepiColombo mission

Author

Orsini, S., Milillo, A., Lichtenegger, H., Varsani, A., Barabash, S., Livi, S., De Angelis, E., Alberti, T., Laky, G., Nilsson, H., Phillips, M., Aronica, A., Kallio, E., Wurz, P., Olivieri, A., Plainaki, C., Slavin, J. A., Dandouras, I., Raines, J. M., Benkhoff, J., Zender, J., Berthelier, J.-J., Dosa, M., Ho, G. C., Killen, R. M., McKenna-Lawlor, S., Torkar, K., Vaisberg, O., Allegrini, F., Daglis, I. A., Dong, C., Escoubet, C. P., Fatemi, S., Fränz, M., Ivanovski, S., Krupp, N., Lammer, H., Leblanc, François, Mangano, V., Mura, A., Rispoli, R., Sarantos, M., Smith, H. T., Wieser, M., Camozzi, F., Di Lellis, A. M., Fremuth, G., Giner, F., Gurnee, R., Hayes, J., Jeszenszky, H., Trantham, B., Balaz, J., Baumjohann, W., Cantatore, M., Delcourt, D., Delva, M., Desai, M., Fischer, H., Galli, A., Grande, M., Holmström, M., Horvath, I., Hsieh, K. C., Jarvinen, R., Johnson, R. E., Kazakov, A., Kecskemety, K., Krüger, H., Kürbisch, C., Leblanc, Frederic, Leichtfried, M., Mangraviti, E., Massetti, S., Moissenko, D., Moroni, M., Noschese, R., Nuccilli, F., Paschalidis, N., Ryno, J., Seki, K., Shestakov, A., Shuvalov, S., Sordini, R., Stenbeck, F., Svensson, J., Szalai, S., Szego, K., Toublanc, D., Vertolli, N., Wallner, R., and Vorburger, A.

Published
2022
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11. Author Correction: The loss of ions from Venus through the plasma wake

Author

Barabash, S., Fedorov, A., Sauvaud, J. J., Lundin, R., Russell, C. T., Futaana, Y., Zhang, T. L., Andersson, H., Brinkfeldt, K., Grigoriev, A., Holmström, M., Yamauchi, M., Asamura, K., Baumjohann, W., Lammer, H., Coates, A. J., Kataria, D. O., Linder, D. R., Curtis, C. C., Hsieh, K. C., Sandel, B. R., Grande, M., Gunell, H., Koskinen, H. E. J., Kallio, E., Riihelä, P., Säles, T., Schmidt, W., Kozyra, J., Krupp, N., Fränz, M., Woch, J., Luhmann, J., McKenna-Lawlor, S., Mazelle, C., Thocaven, J.-J., Orsini, S., Cerulli-Irelli, R., Mura, A., Milillo, A., Maggi, M., Roelof, E., Brandt, P., Szego, K., Winningham, J. D., Frahm, R. A., Scherrer, J., Sharber, J. R., Wurz, P., and Bochsler, P.

Published
2022
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12. Correction to: SERENA: Particle Instrument Suite for Determining the Sun-Mercury Interaction from BepiColombo

Author

Orsini, S., Livi, S. A., Lichtenegger, H., Barabash, S., Milillo, A., De Angelis, E., Phillips, M., Laky, G., Wieser, M., Olivieri, A., Plainaki, C., Ho, G., Killen, R. M., Slavin, J. A., Wurz, P., Berthelier, J.-J., Dandouras, I., Kallio, E., McKenna-Lawlor, S., Szalai, S., Torkar, K., Vaisberg, O., Allegrini, F., Daglis, I. A., Dong, C., Escoubet, C. P., Fatemi, S., Fränz, M., Ivanovski, S., Krupp, N., Lammer, H., Leblanc, François, Mangano, V., Mura, A., Nilsson, H., Raines, J. M., Rispoli, R., Sarantos, M., Smith, H. T., Szego, K., Aronica, A., Camozzi, F., Di Lellis, A. M., Fremuth, G., Giner, F., Gurnee, R., Hayes, J., Jeszenszky, H., Tominetti, F., Trantham, B., Balaz, J., Baumjohann, W., Brienza, D., Bührke, U., Bush, M. D., Cantatore, M., Cibella, S., Colasanti, L., Cremonese, G., Cremonesi, L., D’Alessandro, M., Delcourt, D., Delva, M., Desai, M., Fama, M., Ferris, M., Fischer, H., Gaggero, A., Gamborino, D., Garnier, P., Gibson, W. C., Goldstein, R., Grande, M., Grishin, V., Haggerty, D., Holmström, M., Horvath, I., Hsieh, K.-C., Jacques, A., Johnson, R. E., Kazakov, A., Kecskemety, K., Krüger, H., Kürbisch, C., Lazzarotto, F., Leblanc, Frederic, Leichtfried, M., Leoni, R., Loose, A., Maschietti, D., Massetti, S., Mattioli, F., Miller, G., Moissenko, D., Morbidini, A., Noschese, R., Nuccilli, F., Nunez, C., Paschalidis, N., Persyn, S., Piazza, D., Oja, M., Ryno, J., Schmidt, W., Scheer, J. A., Shestakov, A., Shuvalov, S., Seki, K., Selci, S., Smith, K., Sordini, R., Svensson, J., Szalai, L., Toublanc, D., Urdiales, C., Varsani, A., Vertolli, N., Wallner, R., Wahlstroem, P., Wilson, P., and Zampieri, S.

Published
2021
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14. SERENA: Particle Instrument Suite for Determining the Sun-Mercury Interaction from BepiColombo

Author

Orsini, S., Livi, S. A., Lichtenegger, H., Barabash, S., Milillo, A., De Angelis, E., Phillips, M., Laky, G., Wieser, M., Olivieri, A., Plainaki, C., Ho, G., Killen, R. M., Slavin, J. A., Wurz, P., Berthelier, J.-J., Dandouras, I., Kallio, E., McKenna-Lawlor, S., Szalai, S., Torkar, K., Vaisberg, O., Allegrini, F., Daglis, I. A., Dong, C., Escoubet, C. P., Fatemi, S., Fränz, M., Ivanovski, S., Krupp, N., Lammer, H., Leblanc, François, Mangano, V., Mura, A., Nilsson, H., Raines, J. M., Rispoli, R., Sarantos, M., Smith, H. T., Szego, K., Aronica, A., Camozzi, F., Di Lellis, A. M., Fremuth, G., Giner, F., Gurnee, R., Hayes, J., Jeszenszky, H., Tominetti, F., Trantham, B., Balaz, J., Baumjohann, W., Brienza, D., Bührke, U., Bush, M. D., Cantatore, M., Cibella, S., Colasanti, L., Cremonese, G., Cremonesi, L., D’Alessandro, M., Delcourt, D., Delva, M., Desai, M., Fama, M., Ferris, M., Fischer, H., Gaggero, A., Gamborino, D., Garnier, P., Gibson, W. C., Goldstein, R., Grande, M., Grishin, V., Haggerty, D., Holmström, M., Horvath, I., Hsieh, K.-C., Jacques, A., Johnson, R. E., Kazakov, A., Kecskemety, K., Krüger, H., Kürbisch, C., Lazzarotto, F., Leblanc, Frederic, Leichtfried, M., Leoni, R., Loose, A., Maschietti, D., Massetti, S., Mattioli, F., Miller, G., Moissenko, D., Morbidini, A., Noschese, R., Nuccilli, F., Nunez, C., Paschalidis, N., Persyn, S., Piazza, D., Oja, M., Ryno, J., Schmidt, W., Scheer, J. A., Shestakov, A., Shuvalov, S., Seki, K., Selci, S., Smith, K., Sordini, R., Svensson, J., Szalai, L., Toublanc, D., Urdiales, C., Varsani, A., Vertolli, N., Wallner, R., Wahlstroem, P., Wilson, P., and Zampieri, S.

Published
2021
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26. Formation and Evolution of Protoatmospheres

Author

Massol, H., Hamano, K., Tian, F., Ikoma, M., Abe, Y., Chassefière, E., Davaille, A., Genda, H., Güdel, M., Hori, Y., Leblanc, F., Marcq, E., Sarda, P., Shematovich, V. I., Stökl, A., and Lammer, H.

Published
2016
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27. Scientific problems addressed by the Spektr-UV space project (world space Observatory—Ultraviolet)

Author

Boyarchuk, A. A., Shustov, B. M., Savanov, I. S., Sachkov, M. E., Bisikalo, D. V., Mashonkina, L. I., Wiebe, D. Z., Shematovich, V. I., Shchekinov, Yu. A., Ryabchikova, T. A., Chugai, N. N., Ivanov, P. B., Voshchinnikov, N. V., Gomez de Castro, A. I., Lamzin, S. A., Piskunov, N., Ayres, T., Strassmeier, K. G., Jeffrey, S., Zwintz, S. K., Shulyak, D., Gérard, J.-C., Hubert, B., Fossati, L., Lammer, H., Werner, K., Zhilkin, A. G., Kaigorodov, P. V., Sichevskii, S. G., Ustamuich, S., Kanev, E. N., and Kil’pio, E. Yu.

Published
2016
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29. Sun and Protosolar Nebula : Working Group Report

Author

Kallenbach, R., Robert, F., Geiss, J., Herbst, E., Lammer, H., Marty, B., Millar, T. J., Ott, U., Pepin, R.O., Kallenbach, R., editor, Encrenaz, T., editor, Geiss, J., editor, Mauersberger, K., editor, Owen, T. C., editor, and Robert, F., editor

Published
2003
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34. The PLATO 2.0 mission

Author

Rauer, H., Catala, C., Aerts, C., Appourchaux, T., Benz, W., Brandeker, A., Christensen-Dalsgaard, J., Deleuil, M., Gizon, L., Goupil, M.-J., Güdel, M., Janot-Pacheco, E., Mas-Hesse, M., Pagano, I., Piotto, G., Pollacco, D., Santos, Ċ., Smith, A., Suárez, J.-C., Szabó, R., Udry, S., Adibekyan, V., Alibert, Y., Almenara, J.-M., Amaro-Seoane, P., Eiff, M. Ammler-von, Asplund, M., Antonello, E., Barnes, S., Baudin, F., Belkacem, K., Bergemann, M., Bihain, G., Birch, A. C., Bonfils, X., Boisse, I., Bonomo, A. S., Borsa, F., Brandão, I. M., Brocato, E., Brun, S., Burleigh, M., Burston, R., Cabrera, J., Cassisi, S., Chaplin, W., Charpinet, S., Chiappini, C., Church, R. P., Csizmadia, Sz., Cunha, M., Damasso, M., Davies, M. B., Deeg, H. J., Díaz, R. F., Dreizler, S., Dreyer, C., Eggenberger, P., Ehrenreich, D., Eigmüller, P., Erikson, A., Farmer, R., Feltzing, S., Oliveira Fialho, F. de, Figueira, P., Forveille, T., Fridlund, M., García, R. A., Giommi, P., Giuffrida, G., Godolt, M., da Silva, J. Gomes, Granzer, T., Grenfell, J. L., Grotsch-Noels, A., Günther, E., Haswell, C. A., Hatzes, A. P., Hébrard, G., Hekker, S., Helled, R., Heng, K., Jenkins, J. M., Johansen, A., Khodachenko, M. L., Kislyakova, K. G., Kley, W., Kolb, U., Krivova, N., Kupka, F., Lammer, H., Lanza, A. F., Lebreton, Y., Magrin, D., Marcos-Arenal, P., Marrese, P. M., Marques, J. P., Martins, J., Mathis, S., Mathur, S., Messina, S., Miglio, A., Montalban, J., Montalto, M., P. F. G. Monteiro, M. J., Moradi, H., Moravveji, E., Mordasini, C., Morel, T., Mortier, A., Nascimbeni, V., Nelson, R. P., Nielsen, M. B., Noack, L., Norton, A. J., Ofir, A., Oshagh, M., Ouazzani, R.-M., Pápics, P., Parro, V. C., Petit, P., Plez, B., Poretti, E., Quirrenbach, A., Ragazzoni, R., Raimondo, G., Rainer, M., Reese, D. R., Redmer, R., Reffert, S., Rojas-Ayala, B., Roxburgh, I. W., Salmon, S., Santerne, A., Schneider, J., Schou, J., Schuh, S., Schunker, H., Silva-Valio, A., Silvotti, R., Skillen, I., Snellen, I., Sohl, F., Sousa, S. G., Sozzetti, A., Stello, D., Strassmeier, K. G., Švanda, M., Szabó, Gy. M., Tkachenko, A., Valencia, D., Van Grootel, V., Vauclair, S. D., Ventura, P., Wagner, F. W., Walton, N. A., Weingrill, J., Werner, S. C., Wheatley, P. J., and Zwintz, K.

Published
2014
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36. Modification of the radioactive heat budget of Earth-like exoplanets by the loss of primordial atmospheres.

Author

Erkaev, N V, Scherf, M, Herbort, O, Lammer, H, Odert, P, Kubyshkina, D, Leitzinger, M, Woitke, P, and O'Neill, C

Subjects
PALEOCLIMATOLOGY, ATMOSPHERE, INNER planets, ATMOSPHERIC models, UPPER atmosphere, GIBBS' free energy, EXTRASOLAR planets
Abstract

The initial abundance of radioactive heat producing isotopes in the interior of terrestrial planets are important drivers of its thermal evolution and the related tectonics and possible evolution to an Earth-like habitat. The moderately volatile element K can be outgassed from a magma ocean into H2-dominated primordial atmospheres of protoplanets with assumed masses between 0.55 and 1.0 M Earth at the time when the gas disc evaporated. We estimate this outgassing and let these planets grow through impacts of depleted and non-depleted material that resembles the same 40K abundance of average carbonaceous chondrites until the growing protoplanets reach 1.0 M Earth. We examine different atmospheric compositions and, as a function of pressure and temperature, calculate the proportion of K by Gibbs Free Energy minimization using the ggchem code. We find that for H2-envelopes and for magma ocean surface temperatures that are ≥ 2500 K, no K condensates are thermally stable, so that outgassed 40K can populate the atmosphere to a great extent. However, due to magma ocean turnover time and the limited diffusion of 40K into the upper atmosphere, from the entire 40K in the magma ocean only a fraction may be available for escaping into space. The escape rates of the primordial atmospheres and the dragged 40K are simulated for different stellar EUV activities with a multispecies hydrodynamic upper atmosphere evolution model. Our results show that one can expect that different initial abundances of heat producing elements will result in different thermal and tectonic histories of terrestrial planets and their habitability conditions. [ABSTRACT FROM AUTHOR]

Published
2023
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41. A comparison of global models for the solar wind interaction with Mars

Author

Brain, D., Barabash, S., Boesswetter, A., Bougher, S., Brecht, S., Chanteur, G., Hurley, D., Dubinin, E., Fang, X., Fraenz, M., Halekas, J., Harnett, E., Holmstrom, M., Kallio, E., Lammer, H., Ledvina, S., Liemohn, M., Liu, K., Luhmann, J., Ma, Y., Modolo, R., Nagy, A., Motschmann, U., Nilsson, H., Shinagawa, H., Simon, S., and Terada, N.

Published
2010
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44. Non-thermal escape of the Martian CO$_2$ atmosphere over time: constrained by Ar isotopes

Author

Lichtenegger, H., Dyadechkin, S., Scherf, M., Lammer, H., Adam, R., Kallio, E., Amerstorfer, U. V., and Jarvinen, R.

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

The ion escape of Mars' CO$_2$ atmosphere caused by its dissociation products C and O atoms is {simulated} from present time to $\sim 4.1$ billion years ago (Ga) by {numerical models of the upper atmosphere and its interaction with the solar wind}. The planetward-scattered pick-up ions are used for sputtering estimates of exospheric particles including $^{36}$Ar and $^{38}$Ar isotopes. Total ion escape, sputtering and photochemical escape rates are compared. For solar EUV fluxes $\geq$\,3 times that of today's Sun (earlier than $\sim 2.6$ Ga) ion escape becomes the dominant atmospheric non-thermal loss process until thermal escape takes over during the pre-Noachian eon (earlier than $\sim 4.0\,-\,4.1$ Ga). If we extrapolate the total escape of CO$_2$-related dissociation products back in time until $\sim$ 4.1 Ga we obtain a {maximum} theoretical equivalent to CO$_2$ partial pressure of more than {$\sim 0.4$ bar through non-thermal escape during quiet solar wind conditions}. {However, surface-atmosphere interaction and/or extreme solar events such as frequent CMEs could have increased this value even further. By including the surface as a sink, up to 0.9\,bar, or even up to 1.8\,bar in case of hidden carbonate reservoirs, could have been present at 4.1\,Ga} The fractionation of $^{36}$Ar/$^{38}$Ar isotopes through sputtering and volcanic outgassing from its initial chondritic value of 5.3, as measured in the 4.1 billion years old Mars meteorite ALH 84001, until the present day, however, can be reproduced for assumed CO$_2$ partial pressures of {$\sim0.01 -- 0.4$\,bar without, and $\sim0.4 -- 1.8$\,bar including surface sinks, and} depending on the cessation time of the Martian dynamo (assumed between 3.6\,--\,4.0 Ga) - if atmospheric sputtering of Ar started afterwards., 63 pages (including 8 pages of supplement), 21 figures and 20 tables (including 12 figures and 15 tables in the supplement), resubmitted to Icarus

Published
2021

45. Magnetic Evidence for an Extended Hydrogen Exosphere at Mercury.

Author

Schmid, D., Lammer, H., Plaschke, F., Vorburger, A., Erkaev, N. V., Wurz, P., Narita, Y., Volwerk, M., Baumjohann, W., and Anderson, B. J.

Subjects
MAGNETIC field measurements, MERCURY, MERCURY (Planet), SPACE environment, SPACE probes
Abstract

Remote observations by the Mariner 10 and MErcury Surface, Space ENvironment, GEophysics, and Ranging (MESSENGER) spacecraft have shown the existence of hydrogen in the exosphere of Mercury. However, to date the hydrogen number densities could only be estimated indirectly from exospheric models, based on the remotely observed Lyman‐α radiances for atomic H, and the detection threshold of the Mariner 10 occultation experiment for molecular H2. Here, we show the first on‐site determined altitude‐density profile of atomic H, derived from in situ magnetic field observations by MESSENGER. The results reveal an extended H exosphere with densities that are ∼1–2 orders of magnitude larger than previously predicted. Using an exospheric model that reproduces the H altitude‐density profile allows us to constrain the so far unknown H2 density at the surface, which is ∼2–3 orders of magnitude smaller than previously assumed. These findings demonstrate the importance of (a) in situ measurements supporting remote observations of Mercury's exosphere that will be realized in the near future by the BepiColombo mission and (b) that dissociation processes play a crucial role in Mercury's exosphere. Plain Language Summary: Mercury has an exosphere that contains a variety of species. So far, only two spacecraft have probed the space environment around Mercury: Mariner 10 in 1974–1975 and MErcury Surface, Space ENvironment, GEophysics, and Ranging (MESSENGER) four decades later. Optical observations by Mariner 10 and MESSENGER showed that Mercury has a thin collisionless atmosphere (exosphere) which is abundant in hydrogen. To date the hydrogen number density at Mercury could only be estimated from exospheric models that use the optical observations as constrains, since no in situ measurements of hydrogen are available to determine its exact number density. For the first time, we derive an altitude‐density profile of Mercury's H exosphere from in situ magnetic field measurements by MESSENGER. From the observations of so‐called pick‐up ion cyclotron waves in the magnetic field data, it is possible to derive the local H number density, necessary to excite these waves. The results reveal an extended atomic H exosphere with densities decreasing from ∼100 to 10 cm−3 between 2,400 and 15,000 km above the surface. The unexpected large H densities can only be explained by dissociation processes of H2 molecules. Here, we introduce an exospheric model that includes such dissociation processes, which allows us for the first time to constrain the H2 number density. The results suggests that atomic H has additional sinks near the surface, most likely through chemical reactions with OH and O, and that the photochemistry of H2O in general play an important role for Mercury's exospheric composition. Key Points: First on‐site determined hydrogen number density in Mercury's exosphereDemonstration that dissociation processes play an important role in Mercury's exosphereBased on the results, we can constrain the so far unknown and overestimated molecular surface number density of hydrogen [ABSTRACT FROM AUTHOR]

Published
2022
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46. Correction to: SERENA: Particle Instrument Suite for Determining the Sun-Mercury Interaction from BepiColombo (Space Science Reviews, (2021), 217, 1, (11), 10.1007/s11214-020-00787-3)

Author

Orsini, S. Livi, S.A. Lichtenegger, H. Barabash, S. Milillo, A. De Angelis, E. Phillips, M. Laky, G. Wieser, M. Olivieri, A. Plainaki, C. Ho, G. Killen, R.M. Slavin, J.A. Wurz, P. Berthelier, J.-J. Dandouras, I. Kallio, E. McKenna-Lawlor, S. Szalai, S. Torkar, K. Vaisberg, O. Allegrini, F. Daglis, I.A. Dong, C. Escoubet, C.P. Fatemi, S. Fränz, M. Ivanovski, S. Krupp, N. Lammer, H. Leblanc, F. Mangano, V. Mura, A. Nilsson, H. Raines, J.M. Rispoli, R. Sarantos, M. Smith, H.T. Szego, K. Aronica, A. Camozzi, F. Di Lellis, A.M. Fremuth, G. Giner, F. Gurnee, R. Hayes, J. Jeszenszky, H. Tominetti, F. Trantham, B. Balaz, J. Baumjohann, W. Brienza, D. Bührke, U. Bush, M.D. Cantatore, M. Cibella, S. Colasanti, L. Cremonese, G. Cremonesi, L. D’Alessandro, M. Delcourt, D. Delva, M. Desai, M. Fama, M. Ferris, M. Fischer, H. Gaggero, A. Gamborino, D. Garnier, P. Gibson, W.C. Goldstein, R. Grande, M. Grishin, V. Haggerty, D. Holmström, M. Horvath, I. Hsieh, K.-C. Jacques, A. Johnson, R.E. Kazakov, A. Kecskemety, K. Krüger, H. Kürbisch, C. Lazzarotto, F. Leblanc, F. Leichtfried, M. Leoni, R. Loose, A. Maschietti, D. Massetti, S. Mattioli, F. Miller, G. Moissenko, D. Morbidini, A. Noschese, R. Nuccilli, F. Nunez, C. Paschalidis, N. Persyn, S. Piazza, D. Oja, M. Ryno, J. Schmidt, W. Scheer, J.A. Shestakov, A. Shuvalov, S. Seki, K. Selci, S. Smith, K. Sordini, R. Svensson, J. Szalai, L. Toublanc, D. Urdiales, C. Varsani, A. Vertolli, N. Wallner, R. Wahlstroem, P. Wilson, P. Zampieri, S.

Subjects
GeneralLiterature_INTRODUCTORYANDSURVEY
Abstract

The original online version of this article was revised because a number of authors had the wrong affiliation number next to their names. © 2021, Springer Nature B.V.

Published
2021

47. EChO: Exoplanet characterisation observatory

Author

Tinetti, G., Beaulieu, J. P., Henning, T., Meyer, M., Micela, G., Ribas, I., Stam, D., Swain, M., Krause, O., Ollivier, M., Pace, E., Swinyard, B., Aylward, A., van Boekel, R., Coradini, A., Encrenaz, T., Snellen, I., Zapatero-Osorio, M. R., Bouwman, J., Cho, J. Y-K., Coudé de Foresto, V., Guillot, T., Lopez-Morales, M., Mueller-Wodarg, I., Palle, E., Selsis, F., Sozzetti, A., Ade, P. A. R., Achilleos, N., Adriani, A., Agnor, C. B., Afonso, C., Prieto, C. Allende, Bakos, G., Barber, R. J., Barlow, M., Batista, V., Bernath, P., Bézard, B., Bordé, P., Brown, L. R., Cassan, A., Cavarroc, C., Ciaravella, A., Cockell, C., Coustenis, A., Danielski, C., Decin, L., Kok, R. De, Demangeon, O., Deroo, P., Doel, P., Drossart, P., Fletcher, L. N., Focardi, M., Forget, F., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gaulme, P., Hernández, J. I. González, Grasset, O., Grassi, D., Grenfell, J. L., Griffin, M. J., Griffith, C. A., Grözinger, U., Guedel, M., Guio, P., Hainaut, O., Hargreaves, R., Hauschildt, P. H., Heng, K., Heyrovsky, D., Hueso, R., Irwin, P., Kaltenegger, L., Kervella, P., Kipping, D., Koskinen, T. T., Kovács, G., La Barbera, A., Lammer, H., Lellouch, E., Leto, G., Lopez Morales, M., Lopez Valverde, M. A., Lopez-Puertas, M., Lovis, C., Maggio, A., Maillard, J. P., Maldonado Prado, J., Marquette, J. B., Martin-Torres, F. J., Maxted, P., Miller, S., Molinari, S., Montes, D., Moro-Martin, A., Moses, J. I., Mousis, O., Nguyen Tuong, N., Nelson, R., Orton, G. S., Pantin, E., Pascale, E., Pezzuto, S., Pinfield, D., Poretti, E., Prinja, R., Prisinzano, L., Rees, J. M., Reiners, A., Samuel, B., Sánchez-Lavega, A., Forcada, J. Sanz, Sasselov, D., Savini, G., Sicardy, B., Smith, A., Stixrude, L., Strazzulla, G., Tennyson, J., Tessenyi, M., Vasisht, G., Vinatier, S., Viti, S., Waldmann, I., White, G. J., Widemann, T., Wordsworth, R., Yelle, R., Yung, Y., and Yurchenko, S. N.

Published
2012
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48. Transiting exoplanets from the CoRoT space mission Resolving the nature of transit candidates for the LRa03 and SRa03 fields

Author

Cavarroc, C., Moutou, C., Gandolfi, D., Tingley, B., Ollivier, M., Aigrain, S., Alonso, R., Almenara, J.-M., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Bordé, P., Bouchy, F., Cabrera, J., Carpano, S., Carone, L., Cochran, W. D., Csizmadia, S., Deeg, H. J., Deleuil, M., Díaz, R. F., Dvorak, R., Endl, M., Erikson, A., Fridlund, M., Gillon, M., Guenther, E. W., Guillot, T., Hatzes, A., Hébrard, G., Jorda, L., Léger, A., Lammer, H., Lev, T.-O., Lovis, C., MacQueen, P. J., Mazeh, T., Ofir, A., Parviainen, H., Pasternacki, T., Pätzold, M., Queloz, D., Rauer, H., Rouan, D., Samuel, B., Santerne, A., Schneider, J., Weingrill, J., and Wuchterl, G.

Published
2012
Full Text
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