18 results on '"Wuchterl, G."'
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2. Five Years of Exoplanet Observations with the CoRoT Space Observatory
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Deeg, H, Aigrain, S, Almenara, J, Alonso, R, Baglin, A, Barge, P, Bonomo, A, Borde, P, Bouchy, F, Bruntt, H, Carone, L, Carpano, S, Csizmadia, S, Deleuil, M, Diaz, R, Dvorak, R, Erikson, A, Ferraz-Mello, S, Fridlund, M, Gandolfi, D, Gillon, M, Guillot, T, Grziwa, M, Hatzes, A., Hebrard, G, Jorda, L, Lammer, H, Leger, A., Llebaria, A, Maceroni, C., Mazeh, T, Meunier, J, Moutou, C, Ofir, A, Ollivier, M, Parviainen, Hannu, Pätzold, M, Pont, F, Queloz, D, Rauer, H, Regulo, C, Renner, S, Rouan, D, Samuel, B, Santerne, A, Schneider, J., Tingley, B, Weingrill, J, Wuchterl, G, and Zucker, S
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transit method ,extrasolar planets ,CoRoT - Published
- 2012
3. Possible Projects for the Extension of CoRoT
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Cabrera, J, Csizmadia, S, Erikson, A., Dreyer, C, Fridlund, M, Günther, E, Hatzes, A., Pätzold, M, Rauer, H, and Wuchterl, G
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bright stars ,transit timing variations ,transiting planets ,CoRoT extension - Published
- 2011
4. Exoplanets from the CoRoT space mission. XVII. The hot Jupiter CoRoT-17b: a very old planet
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Csizmadia, S, Moutou, C, Deleuil, M, Cabrera, J, Fridlund, M, Gandolfi, D, Aigrain, S, Alonso, R, Almenara, J, Auvergne, M, Baglin, A, Barge, P, Bonomo, A, Borde, P, Bouchy, F, Bruntt, H, Carone, L, Carpano, S, Cavarroc, C, Cochran, W.D., Deeg, H, Diaz, R, Dvorak, R, Endl, M, Erikson, A, Ferraz-Mello, S, Fruth, T, Gazzano, J-C, Gillon, M, Guenther, E., Guillot, T, Hatzes, A, Havel, M, Hebrard, G, Jehin, E, Jorda, L, Leger, A., Llebaria, A, Lammer, H, Lovis, C, MacQueen, P.J., Mazeh, T, Ollivier, M, Pätzold, M, Queloz, D, Rauer, H, Rouan, D, Santerne, A, Schneider, J., Tingley, B, Titz-Weider, R, and Wuchterl, G
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exoplanets ,photometry ,transit method ,CoRoT-17 ,CoRoT - Published
- 2011
5. XX. CoRoT-20b: A very high density, high eccentricity transiting giant planet
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Deleuil, M., Bonomo, A. S., Ferraz-Mello, S., Erikson, A., Bouchy, F., Havel, M., Aigrain, S., Almenara, J. -M., Alonso, R., Auvergne, M., Baglin, A., Barge, P., Bordé, P., Bruntt, H., Cabrera, J., Carpano, S., Cavarroc, C., Csizmadia, Sz., Damiani, C., Deeg, H. J., Dvorak, R., Fridlund, M., Hébrard, G., Gandolfi, D., Gillon, M., Guenther, E., Guillot, T., Hatzes, A., Jorda, L., Léger, A., Lammer, H., Mazeh, T., Moutou, C., Ollivier, M., Ofir, A., Parviainen, H., Queloz, D., Rauer, H., Rodríguez, A., Rouan, D., Santerne, A., Schneider, J., Tal-Or, L., Tingley, B., Weingrill, J., and Wuchterl, G.
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Earth and Planetary Astrophysics (astro-ph.EP) ,Astrophysics::Solar and Stellar Astrophysics ,FOS: Physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery by the CoRoT space mission of a new giant planet, CoRoT-20b. The planet has a mass of 4.24 +/- 0.23 MJ and a radius of 0.84 +/- 0.04 RJ. With a mean density of 8.87 +/- 1.10 g/cm^3, it is among the most compact planets known so far. Evolution models for the planet suggest a mass of heavy elements of the order of 800 ME if embedded in a central core, requiring a revision either of the planet formation models or of planet evolution and structure models. We note however that smaller amounts of heavy elements are expected from more realistic models in which they are mixed throughout the envelope. The planet orbits a G-type star with an orbital period of 9.24 days and an eccentricity of 0.56. The star's projected rotational velocity is vsini = 4.5 +/- 1.0 km/s, corresponding to a spin period of 11.5 +/- 3.1 days if its axis of rotation is perpendicular to the orbital plane. In the framework of Darwinian theories and neglecting stellar magnetic breaking, we calculate the tidal evolution of the system and show that CoRoT-20b is presently one of the very few Darwin-stable planets that is evolving towards a triple synchronous state with equality of the orbital, planetary and stellar spin periods., Comment: 10 pages, 10 figures
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- 2011
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6. The Mass of CoRoT-7b
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Fridlund, M, Nachmani, G, Mazeh, T, Valencia, D, Hebrard, G, Carone, L, Pätzold, M, Udry, S, Bouchy, F, Deleuil, M, Moutou, C, Barge, P, Bordé, P, Deeg, H, Tingley, B, Dvorak, R, Gandolfi, D, Ferraz-Mello, S, Wuchterl, G, Guenther, E., Guillot, T, Rauer, H, Erikson, A, Cabrera, J, Csizmadia, S, Léger, A, Lammer, H, Weingrill, J, Queloz, D, Alonso, R, Rouan, D, and Schneider, J.
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planetary systems—techniques: radial velocities - Published
- 2011
7. LRa02 E2 0121: Neptune Size Candidate Turns into a Diluted Eclipsing Binary
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Tal-Or, L, Santerne, A, Mazeh, T, Bouchy, F, Moutou, C, Alonso, R, Aigrain, S, Auvergne, M, Barge, P, Bordé, P, Deeg, H, Ferraz-Mello, S, Deleuil, M, Dvorak, R, Erikson, A, Fridlund, M, Gillon, M, Gondoin, P, Guillot, T, Hatzes, A., Jorda, L, Lammer, H, Leger, A., Llebaria, A, Ollivier, M, Pätzold, M, Queloz, D, Rauer, H, Rouan, D, Schneider, J., and Wuchterl, G
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techniques: photometric ,techniques: radial velocities ,binaries: eclipsing ,planetary systems - Published
- 2011
8. The formation of HD 149026 b
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Broeg, C. and Wuchterl, G.
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Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics::Earth and Planetary Astrophysics - Abstract
Today, many extrasolar planets have been detected. Some of them exhibit properties quite different from the planets in our solar system and they have eluded attempts to explain their formation. One such case is HD 149026 b. It was discovered by Sato et al. (2005) . A transit-determined orbital inclination results in a total mass of 114 earth masses. The unusually small radius can be explained by a condensible element core with an inferred mass of 67 earth masses for the best fitting theoretical model. In the core accretion model, giant planets are assumed to form around a growing core of condensible materials. With increasing core mass, the amount of gravitationally bound envelope mass increases. This continues up to the so-called critical core mass -- the largest core allowing a hydrostatic envelope. For larger cores, the lack of static solutions forces a dynamic evolution of the protoplanet in the process accreting large amounts of gas or ejecting the envelope. This would prevent the formation of HD 149026 b. By studying all possible hydrostatic equilibria we could show that HD 149026 b can remain hydrostatic up to the inferred heavy core. This is possible if it is formed in-situ in a relatively low-pressure nebula. This formation process is confirmed by fluid-dynamic calculations using the environmental conditions as determined by the hydrostatic models. We present a quantitative in-situ formation scenario for the massive core planet HD 149026 b. Furthermore we predict a wide range of possible core masses for close-in planets like HD 149026 b. This is different from migration where typical critical core masses should be expected., 6 pages, 2 figures, letter MNRAS accepted 2007 Jan 9
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- 2007
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9. Properties of the short period CoRoT-planet population I: Theoretical planetary mass spectra for a population of stars of 0.8 to 2 solar masses and orbital periods of less then 20 days
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Wuchterl, G., Broeg, C., Krause, S., Pecnik, B., and Schoenke, J.
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Physics::Space Physics ,Astrophysics (astro-ph) ,Astrophysics::Solar and Stellar Astrophysics ,FOS: Physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Abstract
We study the planet populations in the discovery window of the CoRoT-space-telescope scheduled for launch on December 27th. We base the prediction on `first principles' calculations of planet formation in the framework of the planetesimal hypothesis. Aims: To provide a-priori planetary initial mass functions for confrontation with the CoRoT-planet discoveries in the entire range of sensitivity of the CoRoT instrument, i.e. for all giant planets and down to terrestrial planet masses. Methods: We construct a comprehensive set of static complete-equilibrium core-envelope protoplanets with detailed equations of state and opacity and radiative transfer by convection and radiation. Protoplanets are calculated for host-star masses of 0.8 to 2 solar masses and orbital periods of 1 to 16 days. We subsequently check the stability of the planetary population by a series of methods. Results: We find the static planetary populations to be stable and thus a plausible ensemble to predict the planetary IMF for orbital periods in the specified range. Conclusions: We predict bimodal planetary initial mass functions with shapes depending on orbital period. The two main maxima are around a Jupiter mass and about 50 earth masses. We predict an abundant population of Hot Neptunes and a large population of planets that fill the solar-system gap of planetary masses between Neptune and Saturn., Comment: 4 pages, 1 figure, submitted to A&A letters
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- 2007
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10. Properties of the short period CoRoT-planet population II: The impact of loss processes on planet masses from Neptunes to Jupiters
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Lammer, Helmut, Penz, T., Wuchterl, G., Lichtenegger, H. I. M., Khodachenko, M. L., Kulikov, Yu N., Giuseppina Micela, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), INAF - Osservatorio Astronomico di Palermo, Istituto Nazionale di Astrofisica (INAF), Thüringer Landessternwarte Tautenburg (TLS), Polar Geophysical Institute of Russian Academy of Sciences (PGI), Russian Academy of Sciences [Moscow] (RAS), and CoRoT
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[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,exoplanets ,Astrophysics (astro-ph) ,FOS: Physical sciences ,magnetosphere protection ,Astrophysics ,mass loss - Abstract
The orbital distance at which close-in exoplanets maintain their initial mass is investigated by modelling the maximum expected thermal and nonthermal mass loss rates over several Gyr. Depending on an exosphere formation time and the evolution of the stellar X-ray and EUV flux we expect that thermal evaporation at orbital distances less than 0.05 AU may be an efficient loss process for hydrogen-rich exoplanets with masses less than 0.25 MJup. Our results indicate that nonthermal mass loss induced by Coronal Mass Ejections of the host star can significantly erode weakly magnetized short periodic gas giants. The observed exoplanets Gliese 876d at 0.0208 AU with a mass of about 0.033 MJup and 55 Cnc e at 0.045 AU with a mass of about 0.038 MJup could be strongly eroded gas giants, while HD69830b, at 0.078 AU, HD160691d at 0.09 AU and HD69830c at 0.18 AU belonged most likely since their origin to the Neptune-mass domain. The consequences for the planetary population predicted in paper I (Wuchterl et al. 2006) for CoRoTs first field are: (1) for orbital distances less than 0.05 AU (orbital periods less than days) weakly magnetized or highly irradiated gas giants may loose a large fraction of their initial mass and completely loose their gas envelopes. (2) Observed planetary mass spectra at these periods that resemble the initial ones would indicate a major effect of magnetic field protection and so far unknown thermospheric cooling processes. (3) At distances larger than 0.05 AU the impact of loss processes is minor and the observed mass spectra should be close to the initial ones., Comment: submitted to Astron. Astrophys. Lett
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- 2007
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11. CHEOPS/ZIMPOL: a VLT instrument study for the polarimetric search of scattered light from extrasolar planets
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Gisler, D., Schmid, H.M., Thalmann, C., Povel, H.P., Stenflo, J.O., Joos, F., Feldt, M., Lenzen, R., Tinbergen, J., Gratton, R., Stuik, R., Stam, D.M., Brandner, W., Hippler, S., Turatto, M., Neuhauser, R., Dominik, C., Hatzes, A., Henning, T., Lima, J., Quirrenbach, A., Waters, L.B.F.M., Wuchterl, G., Zinnecker, H., Moorwood, A.F.M., Iye, M., and Low Energy Astrophysics (API, FNWI)
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Physics ,Ccd camera ,business.industry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Polarimetry ,Astronomy ,Polarimeter ,Polarization (waves) ,Exoplanet ,Optics ,Planet ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Scattered light ,business - Abstract
We present results from a phase A study supported by ESO for a VLT instrument for the search and investigation of extrasolar planets. The envisaged CHEOPS (CHaracterizing Extrasolar planets by Opto-infrared Polarization and Spectroscopy) instrument consists of an extreme AO system, a spectroscopic integral field unit and an imaging polarimeter. This paper describes the conceptual design of the imaging polarimeter which is based on the ZIMPOL (Zurich IMaging POLarimeter) technique using a fast polarization modulator combined with a demodulating CCD camera. ZIMPOL is capable of detecting polarization signals on the order of p=0.001% as demonstrated in solar applications. We discuss the planned implementation of ZIMPOL within the CHEOPS instrument, in particular the design of the polarization modulator. Further we describe strategies to minimize the instrumental effects and to enhance the overall measuring efficiency in order to achieve the very demanding science goals.
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- 2004
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12. The stability of ultra-compact planetary systems
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Barbara Funk, Wuchterl, G., Schwarz, R., Pilat-Lohinger, E., and Eggl, S.
13. The German Contribution to the CoRoT Mission
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Rauer, H., Erikson, A., Hatzes, A. P., Pätzold, M., Wuchterl, G., Berlin, R., Carone, L., Eigmüller, P., Eislöffel, J., Gahr, A., Guenther, E., Kabath, P., Krutz, D., Lehmann, H., Peter, Gisbert, Rohbeck, U., Russ, N., Ulmer, B., Voss, H., and Zecha, T.
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COROT ,Exoplanets
14. MEASURING THE NIGHT SKY BRIGHTNESS WITH THE LIGHTMETER
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Müller, A., Wuchterl, G., and Marc Sarazin
15. Towards Real Comparative Planetology: Synergies between Solar System Science and the Darwin Mission
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Lammer, H., Chassefiere, E., Kulikov, Y. N., Leblanc, F., Lichtenegger, H. I. M., Grießmeier, J.-M., Khodachenko, M., Stam, D., Sotin, C., Ribas, I., Selsis, F., Allard, F., Mingalev, I., Barabash, S., Gunell, H., Lundin, R., Biernat, H. K., Rucker, H. O., Westall, F., Brack, A., von Bloh, W., Franck, S., Penz, T., Stadelmann, A., Motschmann, U., Belisheva, N. K., Bérces, A., Léger, A., Cockell, C. S., Parnell, J., Arshukova, I. L., Erkaev, N. V., Konovalenko, A. A., Kallio, E., Horneck, G., Guillot, T., Morbidelli, A., Bois, E., Barge, P., Deleuil, M., Moutou, C., Forget, F., Erdi, B., Hatzes, A., Szuszkiewicz, E., Fridlund, M., Mingalev, O., Rauer, Heike, Grenfell, John Lee, Langmayr, D., Jaritz, G., Endler, S, Wuchterl, G., Hanslmaier, A., Odert, P., Leitzinger, M., Wurz, P., Lohinger, E., Dvorak, R., and Weiss, W. W.
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Exoplanets ,Planetology
16. Towards real comparative planetology: Synergies between Solar System science and the DARWIN mission
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Allard, F., Arshukova, I. L., Barabash, S., Barge, P., Siegfried Bauer, Belisheva, N. K., Biernat, H. K., Bois, E., Brack, A., Bérces, A., Chasseflère, E., Cockell, C. S., Deleuil, M., Dvorak, R., Endler, S., Erkaev, N. V., Forget, F., Franck, S., Fridlund, M., Grenfell, J. L., Grießmeier, J. -M, Guillot, T., Gunell, H., Hanslmeier, A., Hatzes, A., Horneck, G., Jaritz, G., Kallio, E., Khodachenko, M., Konovalenko, A. A., Kulikov, Yu N., Lammer, H., Langmayr, D., Leblanc, F., Leitzinger, M., Lichtenegger, H. I. M., Lundin, R., Léger, A., Mingalev, I., Mingalev, O., Morbidelli, A., Motschann, U., Moutou, C., Odert, P., Parnell, J., Penz, T., Pilat-Lohinger, E., Rauer, H., Ribas, I., Rucker, H. O., Selsis, F., Sotin, C., Stadelmann, A., Stam, D., Szuszkiewicz, E., Bloh, W., Weiss, W. W., Westall, F., Wuchterl, G., Wurz, P., and Érdi, B.
17. CoRoT-Exo-3b observations (Deleuil+, 2008)
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Deleuil, M., Deeg, H. J., Alonso, R., Bouchy, F., Rouan, D., Auvergne, M., Baglin, A., Aigrain, S., Almenara, J. M., Barbieri, M., Barge, P., Bruntt, H., Pascal Bordé, Collier, A. C., Csizmadia, S., La Reza, R., Dvorak, R., Erikson, A., Fridlund, M., Gandolfi, D., Gillon, M., Guenther, E., Guillot, T., Hatzes, A., Hebrard, G., Jorda, L., Lammer, H., Leger, A., Llebaria, A., Benoit Loeillet, Mayor, M., Mazeh, T., Moutou, C., Ollivier, M., Paetzold, M., Pont, F., Queloz, D., Rauer, H., Jodi Schneider, Shporer, A., Wuchterl, G., Zucker, S., Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 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'études spatiales et d'instrumentation en astrophysique (LESIA), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Nice Sophia Antipolis (1965 - 2019) (UNS)
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[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,ComputingMilieux_MISCELLANEOUS - Abstract
International audience
18. Transiting exoplanets from the CoRoT space mission: XV. CoRoT-15b: A brown-dwarf transiting companion
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Bouchy, F., Deleuil, M., Guillot, T., Aigrain, S., Carone, L., Cochran, W. D., Almenara, J. M., Alonso, R., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Bordé, P., Csizmadia, S., Bondt, K., Deeg, H. J., Díaz, R. F., Dvorak, R., Endl, M., Erikson, A., Ferraz-Mello, S., Fridlund, M., Davide Gandolfi, Gazzano, J. C., Gibson, N., Gillon, M., Guenther, E., Hatzes, A., Havel, M., Hébrard, G., Jorda, L., Léger, A., Lovis, C., Llebaria, A., Lammer, H., Macqueen, P. J., Mazeh, T., Moutou, C., Ofir, A., Ollivier, M., Parviainen, H., Pätzold, M., Queloz, D., Rauer, H., Rouan, D., Santerne, A., Schneider, J., Tingley, B., Wuchterl, G., Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 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, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
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Brown dwarf ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,spectroscopic ,Space (mathematics) ,01 natural sciences ,photometric ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,planetary systems ,010303 astronomy & astrophysics ,ComputingMilieux_MISCELLANEOUS ,Astrophysics::Galaxy Astrophysics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,Radius ,Orbital period ,Exoplanet ,Stars ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,radial velocities ,brown dwarfs ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery by the CoRoT space mission of a transiting brown dwarf orbiting a F7V star with an orbital period of 3.06 days. CoRoT-15b has a radius of 1.12 +0.30 -0.15 Rjup, a mass of 63.3 +- 4.1 Mjup, and is thus the second transiting companion lying in the theoretical mass domain of brown dwarfs. CoRoT-15b is either very young or inflated compared to standard evolution models, a situation similar to that of M-dwarfs stars orbiting close to solar-type stars. Spectroscopic constraints and an analysis of the lightcurve favors a spin period between 2.9 and 3.1 days for the central star, compatible with a double-synchronisation of the system., 7 pages, 6 figures, accepted in A&A
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