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Your search keyword '"Rodler, F."' showing total 8 results
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8 results on '"Rodler, F."'

1. A planet in a polar orbit of 1.4 solar-mass star

Author

Guenther E.W., Cusano F., Deeg H., Gandolfi D., Geier S., Grziwa S., Heber U., Tal-Or L., Sebastian D., and Rodler F.

Subjects
Physics, QC1-999
Abstract

Although more than a thousand transiting extrasolar planets have been discovered, only very few of them orbit stars that are more massive than the Sun. The discovery of such planets is interesting, because they have formed in disks that are more massive but had a shorter life time than those of solar-like stars. Studies of planets more massive than the Sun thus tell us how the properties of the proto-planetary disks effect the formation of planets. Another aspect that makes these planets interesting is that they have kept their original orbital inclinations. By studying them we can thus find out whether the orbital axes planets are initially aligned to the stars rotational axes, or not. Here we report on the discovery of a planet of a 1.4 solar-mass star with a period of 5.6 days in a polar orbit made by CoRoT. This new planet thus is one of the few known close-in planets orbiting a star that is substantially more massive than the Sun.

Published
2015
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2. High precision radial velocities in the near-infrared domain: Status and prospects

Author

Fiorenzano A.M., Lima J., Amorim A., Moitinho A., Valdivielso L., Esparza P., Béjar V.J.S., Rodler F., Deshpande R., del Burgo C., Zapatero Osorio M.R., Martín E.L., Guenther E., Magazzu A., and Tata R.

Subjects
Physics, QC1-999
Abstract

The extension of the highly successful Doppler technique into the near-infrared (0.9–2.5 μm) is highly desirable as it would open the possibility for searches for extra-solar planets around young stars, very low-mass stars and brown dwarfs. Here we review the current status of this technique and discuss future prospects with particular emphasis on challenging problems for the next decade.

Published
2011
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3. Improving the radial velocity precision of NIRSPEC data

Author

Deshpande R., Zapatero Osorio M.R., Martín E.L., Rodler F., and del Burgo C.

Subjects
Physics, QC1-999
Abstract

We present an approach to improve the radial velocity precision of NIRSPEC data (spectral resolution R = λ/Δλ ≈ 22,000) by using a self-calibration approach. We demonstrate that the accuracy can be significantly improved by deconvolving the spectra and using the telluric lines as a long-term stable wavelength reference.

Published
2011
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4. Radial velocity observations of VB10

Author

Rodler F., Burgo C. del, Osorio M.R. Zapatero, Martin E., Deshpande R., and Montgomery M.M.

Subjects
Physics, QC1-999
Abstract

VB 10 is the smallest star known to harbor a planet according to the recent astrometric study of Pravdo & Shaklan [1]. Here we present near-infrared (J-band) radial velocity of VB 10 performed from high resolution (R~20,000) spectroscopy (NIRSPEC/KECK II). Our results [2] suggest radial velocity variability with amplitude of ~1 km/s, a result that is consistent with the presence of a massive planet companion around VB10 as found via long-term astrometric monitoring of the star by Pravdo & Shaklan. Employing an entirely different technique we verify the results of Pravdo & Shaklan.

Published
2011
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5. HD15082b, a short-period planet orbiting an A-star

Author

Lodieu N., Smalley B., Rodler F., Cameron A.C., Guenther E.W., Endl M., and Reif K.

Subjects
Physics, QC1-999
Abstract

Most of the known transiting extrasolar planets orbit slowly rotating F, G or K stars. In here we report on the detection of a transiting planet orbiting the bright, rapidly rotating A5 star HD15082, recently made by SuperWASP. Time resolved spectroscopic observations taken during transit show a hump caused by the planet crossing the line profile. From the analysis of the spectra, we derive the radius of the planet and find that it is orbiting retrograde in respect to the spin of the star. Because of its small distance from an A5 star, this planet must be one of the hottest planets known, which makes it relatively easy to detect it in the IR. We thus tried to detect it using the TNG but did not succeed. Using direct imaging, we search for possible companions, and found one candidate.

Published
2011
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6. III.7 Planets orbiting stars more massive than the Sun

Author

Guenther, E.W., Sebastian, D., Gandolfi, D., Montañés-Rodríguez, P., Geier, S., Csizmadia, S., Cusano, F., Deeg, H.J., Fridlund, M., Grziwas, S., Heber, U., Heuser, C., Rodler, F., Tal-Or, L., CoRoT-team, Team Corot, and Team Corot

Subjects
Physics, Kepler-47, Stars, Planet, K-type main-sequence star, Astronomy, Internal heating, Habitability of orange dwarf systems
Published
2016

7. The δ scuti star FG vir. V. The 2002 photometric multisite campaign

Author

Breger, M., Rodler, F., Pretorius, M.L., Martín-Ruiz, S., Amado, P.J., Costa, V., Garrido, R., López, De, Coca, P., Olivares, I., Rodríguez, E., Rolland, A., Tshenye, T., Handler, G., Poretti, E., Sareyan, J.P., Alvarez, M., Kilmartin, P.M., Zima, W., Austrian Science Fund, Junta de Andalucía, Dirección General de Investigación Científica y Técnica, DGICT (España), Consejo Superior de Investigaciones Científicas (España), European Commission, Laboratoire Gemini (LG), 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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Delta, Blazhko effect, oscillations [Stars], FOS: Physical sciences, Astrophysics, Star (graph theory), RR Lyrae variable, 01 natural sciences, variables: δ Sct [Stars], Consistency (statistics), 0103 physical sciences, Modulation (music), Stars: variables: δ Sct, Stars: oscillations, individual: FG Vir [Stars], 010303 astronomy & astrophysics, Physics, Stars: individual: FG Vir, 010308 nuclear & particles physics, Astrophysics (astro-ph), photometric [Techniques], Astronomy and Astrophysics, Amplitude, Space and Planetary Science, Techniques: photometric
Abstract

A high-accuracy multisite campaign was carried out from 2002 January to May with a photometric coverage of 398 hours at five observatories. The concentration on a few selected sites gives better consistency and accuracy than collecting smaller amounts from a larger number of sites. 23 frequencies were detected with a high statistical significance. 6 of these are new. The 17 frequencies found in common with the 1992-1995 data are the modes with highest amplitudes. This indicates that the pulsation spectrum of FG Vir is relatively stable over the ten-year period. Two frequencies have variable amplitudes and phases from year to year as well as during 2002. These were both found to be double modes with close frequencies. For the mode at 12.15 c/d this leads to an apparent modulation with a time scale of about 129d. The close frequencies at 12.15 c/d are composed of a radial and a nonradial mode, suggesting a similarity with the Blazhko Effect seen in RR Lyrae stars., Comment: 8 pages, 4 figures, 2 tables

Published
2004
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8. A giant exoplanet orbiting a very-low-mass star challenges planet formation models

Author

Jesus M. Carro, A. Guijarro, F. Hernández Otero, Javier López-Santiago, E. Mirabet, Eduardo L. Martín, Hugo M. Tabernero, H. Martínez-Rodríguez, Antonio Claret, Martin Kürster, Florian Rodler, Birgit Fuhrmeister, M. Llamas, Z. M. Berdiñas, Thomas Henning, A. Rosich, Otmar Stahl, Guillem Anglada-Escudé, Luigi Mancini, E. W. Guenther, P. Huke, L. González-Cuesta, Ralf Launhardt, F. F. Bauer, Ignasi Ribas, D. Baroch, E. N. Johnson, M. Lafarga, Grzegorz Nowak, Priyanka Chaturvedi, M. Ammler-von Eiff, M. R. Zapatero Osorio, V. Wolthoff, E. Rodriguez, L. F. Sarmiento, E. Sánchez-Blanco, Luisa Lara, C. del Burgo, M. López del Fresno, Artie P. Hatzes, S. Lalitha, M. Kehr, Simon Tulloch, F. J. Lázaro, D. Montes, J. Klüter, Melvyn B. Davies, F. J. Aceituno, S. Martin-Ruiz, R. González-Peinado, Juan Luis Cano, Francesc Vilardell, Aviv Ofir, F. J. Abellán, J. Colomé, C. Cardona Guillén, Mathias Zechmeister, Urs Mall, D. Hintz, Richard P. Nelson, I. M. Ferro, V. M. Passegger, M. Cortés-Contreras, P. Martín-Fernández, M. Brinkmöller, Evangelos Nagel, Michael Perryman, Ovidio Rabaza, Jose Antonio Pascual, A. Kaminski, M. Perger, Gilles Bergond, D. Pérez Medialdea, Remo Burn, J. I. González Hernández, B. Arroyo-Torres, Rafael Luque, Martin Schlecker, Armin Huber, A. Fernández-Martín, M. J. López-González, S. Sabotta, G. Veredas, A. Ramón Ballesta, E. González-Álvarez, Fei Yan, Holger Mandel, J. Kemmer, J. I. Vico-Linares, S. Becerril-Jarque, Jorge Sanz-Forcada, Paula Sarkis, R. P. Hedrosa, Rafael Rebolo, J. Stürmer, A. Sánchez-López, Trifon Trifonov, F. Labarga, Jürgen H. M. M. Schmitt, Núria Casasayas-Barris, Alexandre Emsenhuber, Sebastian Schafer, J. A. Marín Molina, Alexander J. Mustill, Anders Johansen, H. Magán Madinabeitia, Hubert Klahr, F. J. Alonso-Floriano, S. V. Jeffers, I. Gallardo Cava, E. de Juan, Andreas Schweitzer, Peter H. Hauschildt, Ricardo Dorda, P. Redondo, M. Azzaro, M. Salz, M. Abril, Juan Carlos Suárez, Hans-Walter Rix, Carlos Cifuentes, Walter Seifert, M. L. García Vargas, Pedro J. Amado, J. Winkler, R. Hernández Arabí, S. Sadegi, I. Hermelo, A. Rodríguez Trinidad, G. Holgado, Karl Wagner, Vianak Naranjo, S. Czesla, M. Kim, D. Benítez, Sabine Reffert, A. Pavlov, Lluis Gesa, Nicolas Lodieu, Lisa Nortmann, D. Galadí-Enríquez, A. Moya, Andreas Quirrenbach, Jose A. Caballero, J. Aceituno, Enrique Herrero, Juan Carlos Morales, E. Casal, Emilio Marfil, Enrique Solano, Diana Kossakowski, E. Díez-Alonso, J.-L. Lizon, J. F. López Salas, M. Lampón, M. C. Cárdenas, P. Schöfer, Ansgar Reiners, R. Calvo-Ortega, T. Stuber, R. Antona, A. Garcia-Piquer, Lev Tal-Or, N. Labiche, Alfredo Sota, Ana Pérez-Calpena, David Barrado, Enric Palle, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, S. Stock, M. Fernandez, Chris Mordasini, E. de Guindos, S. Pedraz, H.-J. Hagen, Jaime Guardia, A. Klutsch, M. A. Sánchez Carrasco, Christopher Marvin, V. Casanova, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Morales, J. C. [0000-0003-0061-518X], Mustill, A. J. [0000-0002-2086-3642], Ribas, I. [0000-0002-6689-0312], Davies, M. B. [0000-0001-6080-1190], Bauer, F. F. [0000-0003-1212-5225], Herrrero, E. [0000-0001-8602-6639], Rodríguez, E. [0000-0001-6827-9077], López González, M. J. [0000-0001-8104-5128], Rodríguez López, C. [0000-0001-5559-7850], Guenther, E. W. [0000-0002-9130-6747], López Santiago, J. [0000-0003-2402-8166], Kaminski, A. [0000-0003-0203-8208], Montes, D. [0000-0002-7779-238X], Baroch, D. [0000-0001-7568-5161], Alonso Floriano, F. J. [0000-0003-1202-5734], Ammler-von Eiff, M. [0000-0001-9565-1698], Anglada Escudé, G. [0000-0002-3645-5977], Barrado, D. [0000-0002-5971-9242], Becerril Jarque, S. [0000-0001-9009-1150], Díez Alonso, E. [0000-0002-5826-9892], Passegger, V. M. [0000-0002-8569-7243], Bergond, G. [0000-0003-3132-9215], Burn, R. [0000-0002-9020-7309], García Vargas, M. L. [0000-0002-2058-3528], Amado, P. J. [0000-0002-8388-6040], Cano, J. [0000-0003-1984-5401], Cardona Guillén, C. [0000-0002-2198-4200], Carro, J. [0000-0002-0838-3603], Abellán, F. J. [0000-0002-5724-1636], Chaturvedi, P. [0000-0002-1887-1192], Sabotta, S. [0000-0001-9078-5574], Cifuentes, C. [0000-0003-1715-5087], Colomé, J. [0000-0002-1678-2241], Arroyo Torres, B. [0000-0002-3392-4694], Emsenhuber, A. [0000-0002-8811-1914], Fuhrmeister, B. [0000-0001-8321-5514], Berdiñas, Z. M. [0000-0002-6057-6461], González Álvarez, E. [0000-0002-4820-2053], González Hernández, J. I. [0000-0002-0264-7356], Calvo Ortega, R. [0000-0003-3693-6030], Guàrdia, J. [0000-0002-7191-9001], Guijarro, A. [0000-0001-5518-1759], Lara, L. M. [0000-0002-7184-920X], Casasayas Barris, N. [0000-0002-2891-8222], Hermelo, I. [0000-0001-9178-694X], Hintz, D. [0000-0002-5274-2589], López del Fresno, M. [0000-0002-9479-7780], Czesla, S. [0000-0002-4203-4773], Johnson, E. [0000-0003-2260-5134], De Juan Fernández, E. [0000-0002-9382-4505], Kehr, M. [0000-0002-7420-7368], Galadí Enríquez, D. [0000-0003-4946-5653], Klüter, J. [0000-0002-3469-5133], González Cuesta, L. [0000-0002-1241-5508], Klutsch, A. [0000-0001-7869-3888], Labarga, F. [0000-0002-7143-0206], González Peinado, R. [0000-0002-6658-8930], Launhardt, R. [0000-0002-8298-2663], Lizon, J. L. [0000-0001-8928-2566], De Guindos, E. [0000-0002-8124-9101], Magan Madinabeitia, H. [0000-0003-1243-4597], Manici, L. [0000-0002-9428-8732], Huke, P. [0000-0001-5913-2743], Marín Molina, J. A. [0000-0002-3525-0806], Martín, E. [0000-0002-1208-4833], Rabaza, O. [0000-0003-2766-2103], Kim, M. [0000-0001-6218-2004], Martínez Rodríguez, H. [0000-0002-1919-228X], Marvin, C. J. [0000-0002-2249-2611], Rodríguez Trinidad, A. [0000-0002-3356-8634], Lampón, M. [0000-0002-0183-7158], Naranjo, V. [0000-0003-0097-1061], Nelson, R. [0000-0002-9687-8779], Nortmann, L. [0000-0001-8419-8760], Lodieu, N. [0000-0002-3612-8968], Ofir, A. [0000-0002-9152-5042], Aceituno, F. J. [0000-0001-8074-4760], Pascual Granado, J. [0000-0003-0139-6951], Pedraz, S. [0000-0003-1346-208X], Marfil, E. [0000-0001-8907-4775], Ramón Ballesta, A. [0000-0002-4323-0610], Redondo, P. G. [0000-0001-5992-5778], Martín Ruiz, S. [0000-0002-9006-7182], Sadegi, S. [0000-0001-9897-6121], Sánchez Carrasco, M. A. [0000-0001-5533-3660], Moya, A. [0000-0003-1665-5389], Sanz Forcada, J. [0000-0002-1600-7835], Sarkis, P. [0000-0001-8128-3126], Vilardell, F. [0000-0003-0441-1504], Nowak, G. [0000-0002-7031-7754], Schäfer, S. [0000-0001-8597-8048], Schlecker, M. [0000-0001-8355-2107], Béjar, V. J. S. [0000-0002-5086-4232], Pérez Calpena, A. [0000-0001-7361-9240], Schöfer, P. [0000-0002-5969-3708], Solano, E. [0000-0003-1885-5130], Sota, A. [https://orcid.org/0000-0002-9404-6952], Rodler, F. [0000-0003-0650-5723], Stuber, T. [0000-0003-2185-0525], García Piquer, A. [0000-0002-6872-4262], Suárez, J. C. [0000-0003-3649-8384], Tabernero, H. [0000-0002-8087-4298], Sánchez López, A. [0000-0002-0516-7956], Winkler, J. [0000-0003-0568-8820], Yan, F. [0000-0001-9585-9034], Sarmiento, L. F. [0000-0002-8475-9705], Luque, R. [0000-0002-4671-2957], Perger, M. [0000-0001-7098-0372], Schmitt, J. H. M. M. [0000-0003-2554-9916], Klahr, H. [0000-0002-8227-5467], Mordasini, C. [0000-0002-1013-2811], Aceituno, J. [0000-0003-0487-1105], Stock, S. [0000-0002-1166-9338], Cortés Contreras, M. [0000-0003-3734-9866], Lafarga, M. [0000-0002-8815-9416], Nagel, E. [0000-0002-4019-3631], Tulloch, S. [0000-0003-0840-8521], Reffert, S. [0000-0002-0460-8289], Rosich, A. [0000-0002-9141-3067], Trifonov, T. [0000-0002-0236-775X], Zapatero Osorio, M. R. [0000-0001-5664-2852], Israel Science Foundation (ISF), Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Swiss National Science Foundation (SNSF), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR), European Research Council (ERC), Generalitat de Catalunya, Deutsche Forschungsgemeinschaft (DFG), Queen Mary University of London, Consejo Nacional de Ciencia y Tecnología (CONACYT), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Israel Science Foundation, Consejo Nacional de Ciencia y Tecnología (México), German Centre for Air and Space Travel, European Research Council, German Research Foundation, National Science Foundation (US), Swiss National Science Foundation, Science and Technology Facilities Council (UK), Knut and Alice Wallenberg Foundation, Spanish Ministry for Science, Ramón y Cajal programa, Israel Science Foundation grant, CONICYT-FONDECYT/Chile Postdoctorado, Deutsches Zentrum fur Luft-un Raumfahrt (DLR), Italian Minister of Instruction, Mexican national council for science and technology, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, German Science Foundation (DFG) Research Unit, Priority Programs SPP, Exploring the Diversity of Extrasolar Planets, Swiss National Science Foundation under grant, Queen Mary University of London Scholarship and STFC, Spanish MCIU FPI-SO predoctoral contract, and European Research Council under the European Union Horizon 2020 research and innovation program

Subjects
010504 meteorology & atmospheric sciences, Gas giant, 530 Physics, FOS: Physical sciences, Minimum mass, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Multidisciplinary, 520 Astronomy, Giant planet, Astronomy, Planetary system, 620 Engineering, Accretion (astrophysics), Exoplanet, Orbit, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science, This research was supported by the following programs, grants, and fellowships: Spanish Ministry for Science, Innovation and Universities (MCIU) ESP2014-54062-R, ESP2014-54362P, AYA2015-69350-C3-2-P, BES-2015-074542, AYA2016-79425-C3-1/2/3-P, ESP2016-76076-R, ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87143-R, ESP2017-87676-C05-02-R, ESP-2017-87676-2-2, RYC-2012-09913 (>Ramon y Cajal> program), and FPU15/01476; Israel Science Foundation grant 848/16, CONICYT-FONDECYT/Chile Postdoctorado 3180405; Deutsches Zentrum fur Luft-un Raumfahrt (DLR) 50OW0204 and 50OO1501; Italian Minister of Instruction, University and Research (MIUR), FFABR 2017; University of Rome Tor Vergata, >Mission: Sustainability 2016> fund; European Research Council under the European Union Horizon 2020 research and innovation program 694513; Mexican national council for science and technology CONACYT, CVU 448248; the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709); Generalitat de Catalunya/CERCA program; Fondo Europeo de Desarollo Regional (FEDER); German Science Foundation (DFG) Research Unit FOR2544 >Blue Planets around Red Stars> and Priority Programs SPP 1833, >Building a Habitable Earth> and SPP 1992, >Exploring the Diversity of Extrasolar Planets> NSF grants PHY17-48958 and PHY-1607761; Swiss National Science Foundation under grant BSGIO_155816 >PlaneltsInTime' and within the framework of the NCCR PlanetS; Queen Mary University of London Scholarship and STFC Consolidated Grant ST/P000592/1; Spanish MCIU FPI-SO predoctoral contract BES-2017-082610 and the Knut and Alice Wallenberg Foundation.

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