Bibliografías temáticas / Extrasolare Planeten

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Literatura académica sobre el tema "Extrasolare Planeten"

Autor: Grafiati
Publicado: 4 de junio de 2021
Última modificación: 14 de febrero de 2022

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Artículos de revistas sobre el tema "Extrasolare Planeten"

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Bührke, Thomas. "Extrasolare Planeten werden sichtbar". Physik in unserer Zeit 40, n.º 1 (enero de 2009): 11. http://dx.doi.org/10.1002/piuz.200990001.

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Wiedemann, Günter, L. Drake Deming, Gordon L. Bjoraker y Cedric Goukenleuque. "Infrared spectroscopic search for short-period giant extrasolar planets". Symposium - International Astronomical Union 202 (2004): 133–35. http://dx.doi.org/10.1017/s0074180900217701.

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IR spectroscopy with a resolution ⋋/△⋋ ≳ 10, 000 is a powerful technique for the investigation of short-periodic giant extra-solar planets. For an unambiguous direct detection attempt one exploits the large-amplitude Doppler modulation of the planet's IR spectrum. A successful measurement of the planet's radial velocity amplitude would yield directly the planet-star mass ratio. Spectral information can be extracted if high per-pixel S/N levels are achieved.
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de Gasperin, F., T. J. W. Lazio y M. Knapp. "Radio observations of HD 80606 near planetary periastron". Astronomy & Astrophysics 644 (diciembre de 2020): A157. http://dx.doi.org/10.1051/0004-6361/202038746.

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Context. All the giant planets in the Solar System generate radio emission via electron cyclotron maser instability, giving rise most notably to Jupiter’s decametric emissions. An interaction with the solar wind is at least partially responsible for all of these Solar System electron cyclotron masers. HD 80606b is a giant planet with a highly eccentric orbit, leading to predictions that its radio emission may be enhanced substantially near periastron. Aims. This paper reports observations with the Low Frequency Array (LOFAR) of HD 80606b near its periastron in an effort to detect radio emissions generated by an electron cyclotron maser instability in the planet’s magnetosphere. Methods. The reported observations are at frequencies between 30 and 78 MHz, and they are distinguished from most previous radio observations of extrasolar planets by two factors: (i) they are at frequencies near 50 MHz, much closer to the frequencies at which Jupiter emits (ν < 40 MHz) and lower than most previously reported observations of extrasolar planets; and (ii) sensitivities of approximately a few millijanskys have been achieved, an order of magnitude or more below nearly all previous extrasolar planet observations below 100 MHz. Results. We do not detect any radio emissions from HD 80606b and use these observations to place new constraints on its radio luminosity. We also revisit whether the observations were conducted at a time when HD 80606b was super-Alfvénic relative to the host star’s stellar wind, which experience from the Solar System illustrates is a state in which an electron cyclotron maser emission can be sustained in a planet’s magnetic polar regions.
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Barnes, Rory y Richard Greenberg. "Extrasolar planet interactions". Proceedings of the International Astronomical Union 3, S249 (octubre de 2007): 469–78. http://dx.doi.org/10.1017/s1743921308016980.

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AbstractThe dynamical interactions of planetary systems may be a clue to their formation histories. Therefore, the distribution of these interactions provides important constraints on models of planet formation. We focus on each system's apsidal motion and proximity to dynamical instability. Although only ∼25 multiple planet systems have been discovered to date, our analyses in these terms have revealed several important features of planetary interactions. 1) Many systems interact such that they are near the boundary between stability and instability. 2) Planets tend to form such that at least one planet's eccentricity periodically drops to near zero. 3) Mean-motion resonant pairs would be unstable if not for the resonance. 4) Scattering of approximately equal mass planets is unlikely to produce the observed distribution of apsidal behavior. 5) Resonant interactions may be identified through calculating a system's proximity to instability, regardless of knowledge of angles such as mean longitude and longitude of periastron (e.g. GJ 317 b and c are probably in a 4:1 resonance). These properties of planetary systems have been identified through calculation of two parameters that describe the interaction. The apsidal interaction can be quantified by determining how close a planet is to an apsidal separatrix (a boundary between qualitatively different types of apsidal oscillations, e.g. libration or circulation of the major axes). This value can be calculated through short numerical integrations. The proximity to instability can be measured by comparing the observed orbital elements to an analytic boundary that describes a type of stability known as Hill stability. We have set up a website dedicated to presenting the most up-to-date information on dynamical interactions: http://www.lpl.arizona.edu/~rory/research/xsp/dynamics.
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Kramm, Ulrike, Nadine Nettelmann y Ronald Redmer. "Constraining planetary interiors with the Love number k2". Proceedings of the International Astronomical Union 6, S276 (octubre de 2010): 482–84. http://dx.doi.org/10.1017/s1743921311020898.

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AbstractFor the solar sytem giant planets the measurement of the gravitational moments J2 and J4 provided valuable information about the interior structure. However, for extrasolar planets the gravitational moments are not accessible. Nevertheless, an additional constraint for extrasolar planets can be obtained from the tidal Love number k2, which, to first order, is equivalent to J2. k2 quantifies the quadrupolic gravity field deformation at the surface of the planet in response to an external perturbing body and depends solely on the planet's internal density distribution. On the other hand, the inverse deduction of the density distribution of the planet from k2 is non-unique. The Love number k2 is a potentially observable parameter that can be obtained from tidally induced apsidal precession of close-in planets (Ragozzine & Wolf 2009) or from the orbital parameters of specific two-planet systems in apsidal alignment (Mardling 2007). We find that for a given k2, a precise value for the core mass cannot be derived. However, a maximum core mass can be inferred which equals the core mass predicted by homogeneous zero metallicity envelope models. Using the example of the extrasolar transiting planet HAT-P-13b we show to what extend planetary models can be constrained by taking into account the tidal Love number k2.
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6

Miller-Ricci, Eliza, Sara Seager y Dimitar Sasselov. "The Atmospheres of Extrasolar Super-Earths". Proceedings of the International Astronomical Union 4, S253 (mayo de 2008): 263–71. http://dx.doi.org/10.1017/s1743921308026483.

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AbstractExtrasolar super-Earths (1-10 M⊕) are likely to exist with a wide range of atmospheres. While a number of these planets have already been discovered through radial velocities and microlensing, it will be the discovery of the firsttransitingsuper-Earths that will open the door to a variety of follow-up observations aimed at characterizing their atmospheres. Super-Earths may fill a large range of parameter space in terms of their atmospheric composition and mass. Specifically, some of these planets may have high enough surface gravities to be able to retain large hydrogen-rich atmosphseres, while others will have lost most of their hydrogen to space over the planet's lifetime, leaving behind an atmosphere more closely resembling that of Earth or Venus. The resulting composition of the super-Earth atmosphere will therefore depend strongly on factors such as atmospheric escape history, outgassing history, and the level of stellar irradiation that it receives. Here we present theoretical models of super-Earth emission and transmission spectra for a variety of possible outcomes of super-Earth atmospheric composition ranging from hydrogen-rich to hydrogen-poor. We focus on how observations can be used to differentiate between the various scenarios and constrain atmospheric composition.
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7

Ehrenreich, D., A. Lecavelier des Etangs, G. Hébrard, J. M. Désert, A. Vidal-Madjar, J. C. McConnell, C. D. Parkinson, G. E. Ballester y R. Ferlet. "The hydrogen exosphere of exoplanet HD 209458b detected with HST/ACS". Proceedings of the International Astronomical Union 4, S253 (mayo de 2008): 528–31. http://dx.doi.org/10.1017/s1743921308027129.

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AbstractExospheric atomic hydrogen escaping from the planet HD 209458b provides the largest observational signature ever detected for an extrasolar planet atmosphere. We present observations of this transiting planet's extended exosphere with the Advanced Camera for Surveys on board the Hubble Space Telescope. From the two transit light curves obtained at Lyman α, we find an in-transit absorption of (8.0±5.7)%, in good agreement with previous studies. These new constraints on the size of the exosphere strengthens the evaporation scenario. Full details are provided in Ehrenreich et al. (2008).
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Shkolnik, Evgenya, David A. Bohlender, Gordon A. H. Walker y Andrew Collier Cameron. "The On/Off nature of star-planet interactions in the HD 179949 and υ And systems". Proceedings of the International Astronomical Union 3, S249 (octubre de 2007): 151–58. http://dx.doi.org/10.1017/s1743921308016530.

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AbstractEvidence suggesting an observable magnetic interaction between a star and its hot Jupiter (Porb< 7 days,a< 0.1 AU,Mpsini> 0.2MJ) appears as a cyclic variation of stellar activity synchronized to the planet's orbit. HD 179949 has been observed almost every year since 2001. Synchronicity of the Ca II H & K emission with the orbit is clearly seen in four out of six epochs, while rotational modulation withProt=7 days is apparent in the other two seasons. We observe a similar phenomenon on υ And, which displays rotational modulation (Prot=12 days) in September 2005, while in 2002 and 2003 variations appear to correlate with the planet's orbital period. This on/off nature of star-planet interaction (SPI) in the two systems is likely a function of the changing stellar magnetic field structure throughout its activity cycle. The tentative correlation between this activity in the 13 stars we have observed to date and the ratio ofMpsinito the planet's rotation period, a quantity proportional to the hot Jupiter's magnetic moment, first presented in Shkolniket al. (2005) remains viable. This work furthers the characterization of SPI, improving its potential as a probe of extrasolar planetary magnetic fields.
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Wagner, Frank W., Frank Sohl, Heike Rauer, Hauke Hussmann y Matthias Grott. "Interior structure models of terrestrial exoplanets and application to CoRoT-7 b". Proceedings of the International Astronomical Union 5, H15 (noviembre de 2009): 708–9. http://dx.doi.org/10.1017/s1743921310011105.

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AbstractIn this study, we model the internal structure of CoRoT-7b, considered as a typical extrasolar terrestrial planet, using mass and energy balance constraints. Our results suggest that the deep interior is predominantly composed of dry silicate rock, similar to the Earth's Moon. A central iron core, if present, would be relatively small and less massive (<15 wt.% of the planet's total mass) as compared to the Earth's (core mass fraction 32.6 wt.%). Furthermore, a partly molten near-surface magma ocean could be maintained, provided surface temperatures were high enough and the rock component mainly composed of Earth-like mineral phase assemblages.
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Boss, Alan P., R. Paul Butler, William B. Hubbard, Philip A. Ianna, Martin Kürster, Jack J. Lissauer, Michel Mayor et al. "Working Group on Extrasolar Planets: (Groupe De Travail Pour les Planetes Extra-Solaires)". Transactions of the International Astronomical Union 25, n.º 1 (2002): 144–46. http://dx.doi.org/10.1017/s0251107x00001383.

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Tesis sobre el tema "Extrasolare Planeten"

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Dominis, Dijana. "The role of binary stars in searches for extrasolar planets by microlensing and astrometry". Phd thesis, Universität Potsdam, 2006. http://opus.kobv.de/ubp/volltexte/2006/1081/.

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Ser, Badia Daniel del. "TFAW: Noise filtering Through the use of the Wavelet Transform in Astronomy Photometric Data". Doctoral thesis, Universitat de Barcelona, 2018. http://hdl.handle.net/10803/665320.

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The first confirmed detection of an exoplanet orbiting a main-sequence star was made in 1995, when a giant planet was found by radial velocity measurements in a four-day orbit around the nearby star 51 Pegasi by Mayor and Queloz in 1995. This finding encouraged the development of the method known as transit method that detects distant planets by measuring the small darkening of a star light curve as an orbiting planet passes between it and the Earth. The first detection of a transiting exoplanet, HD 209458 b, in 1999 by D. Charbonneau and collaborators and G. W. Henry and collaborators, and the discoveries obtained for this planet during follow- up observations (first planet with a detectable atmosphere containing oxygen and carbon, first detection of an evaporating hydrogen atmosphere and being one of the first two exoplanets to be directly observed spectroscopically) demonstrated the high scientific potential of planets discovered with this method. Transit photometry is currently the most effective and sensitive method for detecting extrasolar planets. Several surveys have taken this approach, such as the ground-based MEarth, SuperWASP, KELT, HAT-South, TFRM-PSES, NGTS or the Evryscope, as well as the space-based CoRoT, Kepler, the recently commissioned, TESS and the future PLATO missions. The photometric precision and accuracy achieved by an astronomical survey is a key factor in detecting a transiting signal or any other kind of variability. Many of the systematic variations in a given light curve are shared by light curves of other stars in the same data set. In order to remove those systematics, one can identify the objects in the field that suffer from the same kind of variations as the target (correlated noise) and then build and apply a filter based on the light curves of these comparison stars. Wavelets have unique properties that make them an ideal tool for analyzing signals of non- stationary nature. In comparison to the sine wave used in the Fourier transform, which is smooth and of infinite length, the wavelet is irregular in shape and compactly supported. Their irregular shape allows to analyze signals with discontinuities, transients, singularities and sharp changes, while their compactly supported nature allows temporal localization of the signal's features. Along this work we lay out the framework from which the main goal of this thesis, the Wavelet-based Trend Filtering Algorithm (TFAW) will be built from. TFAW is a wavelet-based modification of the Trend Filtering Algorithm developed by Kovács, Bakos and Noyes (2005). TFAW is a totally generic, Python-based, parallelized algorithm useful to improve the performance of signal detection, reconstruction and characterization, provided that a set of comparison light curves sharing the same systematics and trends as the target time series is available. differs from other wavelet-based noise-filtering algorithms in that it does not require any parametric model fitting or any extra computational method. TFAW estimates the noise contribution of the signal from its Stationary Wavelet Transform (SWT) at each iteration step and the de-noising is done through the subtraction of this contribution from the signal. TFAW de-noises the signal without modifying any of its intrinsic properties contrary to wavelet coefficient thresholding that can lead to distortions of the signal and introduce artificial oscillations or ripples around discontinuities. Tests conducted on simulated and real (coming from the TFRM-PSES, Evryscope, CoRoT and Kepler surveys) TFAW-filtered light curves show an improvement of 40% (although it can be higher) in their standard deviations with respect to the ones detrended with TFA, leading to a better characterization of the signal, without modifying its features. It improves the transit detection rate a factor 2-5 for low SNR signals with respect TFA. We demonstrate that the TFAW-filtered light curve yields better MCMC posterior distributions, diminishes the bias in the fitted transit parameters and their uncertainties and narrows the credibility intervals up to a factor 10 for simulated transits. Finally, TFAW is able to isolate the different underlying signals within a light curve with multiple periodic signals, such as multi-transit signals, transients, modulations or other kinds of stellar variabilities.
El descubrimiento del exoplaneta gigante 51 Pegasi b (detectado por Mayor y Queloz en 1995), mediante el método de las velocidades radiales, promovió el desarrollo de una nueva técnica de detección. Esta técnica, conocida como el método del tránsito, detecta exoplanetas midiendo el pequeño oscurecimiento del flujo estelar cuando el planeta pasa entre la estrella y el observador. El método del tránsito es, actualmente, el modo más eficiente y sensible para detectar planetas extrasolares. Muchas misiones han seguido este modo de observación, aquellas basadas en tierra, como MEarth, SuperWASP, KELT, HAT-South, TFRM-PSES, NGTS o el Evryscope; así como aquellas misiones espaciales como COnvection ROtation and planetary Transits (CoRoT), Kepler, TESS y la futura misión PLATO. La precisión fotométrica y la exactitud conseguida por una misión es un factor clave en la detección y caracterización de una señal correspondiente a un tránsito o a cualquier otro tipo de variabilidad. Las wavelets tienen unas propiedades que las hacen ideales para analizar señales de naturaleza no estacionaria. La forma irregular de las wavelets permite analizar señales con discontinuidades, singularidades o cambios bruscos mientras que su naturaleza compacta permite la localización temporal de las características de la señal. En este trabajo presentamos el Wavelet-based Trend Filtering Algorithm (TFAW). TFAW es un algoritmo totalmente genérico, desarrollado y paralelizado en Python basado en el Trend Filtering Algorithm (TFA) desarrollado por Kovács, Bakos y Noyes (2005). El algoritmo es útil para mejorar el rendimiento en la detección, reconstrucción y caracterización de señales astrofísicas. TFAW difiere de otros métodos de filtrado de ruido basados en wavelets en que no requiere ningún modelo de ajuste paramétrico o cualquier otro método computacional. TFAW estima la contribución de ruido de la señal a partir de su Stationary Wavelet Transform (SWT) y el filtrado se realiza eliminando esta contribución de la señal. Además, TFAW es capaz de hacer el filtrado de la señal sin modificar ninguna de sus características intrínsecas a diferencia de otros métodos como los umbrales calibrados de los coeficientes wavelet que pueden dar lugar a distorsiones de la señal o introducir oscilaciones o perturbaciones artificiales alrededor de discontinuidades. En curvas de luz simuladas, TFAW mejora la detección de tránsitos en un factor 2.5 para señales con bajo SNR. TFAW proporciona una mejor representación y caracterización de señales simuladas y reales (provenientes de las misiones TFRM-PSES, Evryscope, CoRoT y Kepler) afectadas por ruido. Así mismo, proporciona mejores probabilidades a posteriori y una disminución del bias y las incertidumbres de los parámetros ajustados mediante MCMC.
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Nascimento, Sanzia Alves do. "Propriedades f?sicas de planetas extrasolares". Universidade Federal do Rio Grande do Norte, 2008. http://repositorio.ufrn.br:8080/jspui/handle/123456789/18579.

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Made available in DSpace on 2015-03-03T15:15:22Z (GMT). No. of bitstreams: 1 SanziaAN.pdf: 964619 bytes, checksum: 25b161330259b5777dcaa8cf03c1242b (MD5) Previous issue date: 2008-04-22
Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior
ROTATION is one the most important aspects to be observed in stellar astrophysics. Here we investigate that particularly in stars with planets. This physical parameter supplies information about the distribution of angular momentum in the planetary system, as well as its role on the control of dierent phenomena, including coronal and cromospherical emission and on the ones due of tidal effects. In spite of the continuous solid advances made on the study of the characteristics and properties of planet host stars, the main features of their rotational behavior is are not well established yet. In this context, the present work brings an unprecedented study about the rotation and angular momentum of planet-harbouring stars, as well as the correlation between rotation and stellar and planetary physical properties. Our analysis is based on a sample of 232 extrasolar planets, orbiting 196 stars of dierent luminosity classes and spectral types. In addition to the study of their rotational behavior, the behavior of the physical properties of stars and their orbiting planets was also analyzed, including stellar mass and metallicity, as well as the planetary orbital parameters. As main results we can underline that the rotation of stars with planets present two clear features: stars with Tef lower than about 6000 K have slower rotations, while among stars with Tef > 6000 K we and moderate and fast rotations, though there are a few exceptions. We also show that stars with planets follow mostly the Krafts law, namely < J > / v rot. In this same idea we show that the rotation versus age relation of stars with planets follows, at least qualitatively, the Skumanich and Pace & Pasquini laws. The relation rotation versus orbital period also points for a very interesting result, with planet-harbouring stars with shorter orbital periods present rather enhanced rotation
ROTA??O ? um dos importantes aspectos a ser observado na astrof?sica estelar. Por isto, neste trabalho, investigamos este par?metro no estudo das estrelas hospedeiras de planetas. Par?metro f?sico este que fornece informa??o sobre a distribui??o do momentum angular dos sistemas planet?rios, bem como sobre o seu papel nos mais diferentes fen?menos, incluindo emiss?o cromosf?rica e coronal e sobre aqueles decorrentes de efeitos de mar?. Apesar dos cont?nuos avan?os feitos no estudo das caracter?sticas e das propriedades destes objetos, as principais caracter?sticas de seu comportamento rotat?rio ainda n?o est?o bem estabelecidas. Neste contexto, o presente trabalho traz um estudo pioneiro sobre a rota??o e o momentum angular das estrelas hospedeiras de planetas, bem como sobre a correla??o entre rota??o e par?metros f?sicos estelares e planet?rios. Nossa an?lise ? baseada em uma amostra de 232 planetas extrasolares, orbitando 196 estrelas de diferentes classes de luminosidade e tipos espectrais. Al?m do estudo do comportamento rotacional dessas estrelas, re-visitamos o comportamento das propriedades f?sicas destas estrelas e de seus planetas, incluindo a massa estelar e a metalicidade, bem como os par?metros orbitais planet?rios. Como resultados principais, podemos sublinhar que a rota??o das estrelas com planetas apresenta duas claras caracter?sticas: estrelas com Tef inferiores aproximadamente 6000 K possuem rota??es mais baixas, enquanto que entre aquelas com Tef > 6000 K encontramos rota??es modv eradas e altas, embora algumas exce??es. N?s mostramos tamb?m que as estrelas com planetas seguem, em sua maioria, a lei do Kraft, a saber < J > / v rot. Nesta mesma linha n?s mostramos que a rela??o rota??o versus idade das estrelas com planetas segue, ao menos qualitativamente, como qualquer outra estrela de campo ou de aglomerado, a lei de Skumanich e de Pace & Pasquini. Um resultado interessante a ser destacado ? a rela??o rota??o versus per?odo orbital, que aponta para uma tend?ncia de que as estrelas que abrigam planetas com per?odo orbital menores apresentam rota??es mais real?adas
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Hood, Ben Andrew Ashcom. "Extrasolar planet search and characterisation". Thesis, St Andrews, 2007. http://hdl.handle.net/10023/359.

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Howe, Alex Ryan. "Topics in Extrasolar Planet Characterization". Thesis, Princeton University, 2016. http://pqdtopen.proquest.com/#viewpdf?dispub=10167564.

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I present four papers exploring different topics in the area of characterizing the atmospheric and bulk properties of extrasolar planets. In these papers, I present two new codes, in various forms, for modeling these objects. A code to generate theoretical models of transit spectra of exoplanets is featured in the first paper and is refined and expanded into the APOLLO code for spectral modeling and parameter retrieval in the fourth paper. Another code to model the internal structure and evolution of planets is featured in the second and third papers. The first paper presents transit spectra models of GJ 1214b and other super-Earth and mini-Neptune type planets—planets with a “solid”, terrestrial composition and relatively small planets with a thick hydrogen-helium atmosphere, respectively—and fit them to observational data to estimate the atmospheric compositions and cloud properties of these planets. The second paper presents structural models of super-Earth and mini-Neptune type planets and estimates their bulk compositions from mass and radius estimates. The third paper refines these models with evolutionary calculations of thermal contraction and ultraviolet-driven mass loss. Here, we estimate the boundaries of the parameter space in which planets lose their initial hydrogen-helium atmospheres completely, and we also present formation and evolution scenarios for the planets in the Kepler-11 system. The fourth paper uses more refined transit spectra models, this time for hot jupiter type planets, to explore the methods to design optimal observing programs for the James Webb Space Telescope to quantitatively measure the atmospheric compositions and other properties of these planets.

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Carter, Andrew James. "Observation and modeling of extrasolar planets". Thesis, Open University, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.578669.

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The field of exoplanet research has currently yielded the discovery of 552 planets. This figure includes 132 transiting planets which can be studied in greater detail and have formed the cornerstone of research to characterise the exoplanet population. In particular, such studies seek to analyse the planetary atmospheres, but research has thus far yielded more questions than answers. Exoplanetary atmospheric studies have typically focussed on one planet apiece - complicating any comparative analysis as every result employs different methods and instruments. For a comprehensive, comparative study, a robust and reliable means of reducing and analysing such observations is required, along with a body of data from a single instrument. One such instrument is the Bubble Space Telescope (BST) whose NICMOS (Near Infrared Camera and Multi-Object Spectrometer) instrument has observed the transits of nine extrasolar planets across multiple wavelengths in the near-infrared. A robust pipeline has been developed to reduce all such observations using the fame techniques. This pipeline reduces grism images of an exoplanet host star across a transit event. These exposures are checked for bad pixels, flat fielded and background-subtracted before robust extraction of a transit light curve. This light curve is then detrended to remove systematic noise by application of a new technique developed in this study. Following detrending, the light curve is modelled using a be- spoke MCMC (Markov-Chain Monte-Carlo) algorithm to determine the planetary parameters. A continuum of wavelength-dependent transit light curves is also extracted, detrended and modelled to de- termine the variation in transit depth with wavelength; and .hereby infer the transmission spectrum of the planet's atmosphere. The finished pipeline has been applied to three sets of HST NIC- MOS observations covering the transits of WASP-2b, HD189733b and GJ436b. For each data set, a new set of planetary parameters has been derived and for WASP-2b and HD189733b an atmospheric transmission spectrum extracted. Both spectra show signs of atmospheric haze and molecular absorption, but also evidence of residual systematic noise, complicating analysis.
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7

Muterspaugh, Matthew Ward. "Binary star systems and extrasolar planets". Thesis, Massachusetts Institute of Technology, 2005. http://hdl.handle.net/1721.1/34646.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2005.
Includes bibliographical references (p. 121-137).
For ten years, planets around stars similar to the Sun have been discovered, confirmed, and their properties studied. Planets have been found in a variety of environments previously thought impossible. The results have revolutionized the way in which scientists understand planet and star formation and evolution, and provide context for the roles of the Earth and our own solar system. Over half of star systems contain more than one stellar component. Despite this, binary stars have often been avoided by programs searching for planets. Discovery of giant planets in compact binary systems would indirectly probe the timescales of planet formation, an important quantity in determining by which processes planets form. A new observing method has been developed to perform very high precision differntial astrometry on bright binary stars with separations in the range of 0.1 - 1.0 arcseconds. Typical measurement precisions over an hour of integration are on the order of 10 micro-arcseconds (as), enabling one to look for perturbations to the Keplerian orbit that would indicate the presence of additional components to the system. This method is used as the basis for a new program to find extrasolar planets. The Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES) is a search for giant planets orbiting either star in 50 binary systems. The goal of this search is to detect or rule out planets in the systems observed and thus place limits on any enhancements of planet formation in binaries. It is also used to measure fundamental properties of the stars comprising the binary, such as masses and distances, useful for constraining stellar models at the 10-3 level.
(cont.) This method of differential astrometry is applied to three star systems. Equulei is among the most well-studied nearby binary star systems. Results of its observation have been applied to a wide range of fundamental studies of binary systems and stellar astrophysics. PHASES data are combined with previously published radial velocity data and other previously published differential astrometry measurements to produce a combined model for the system orbit. The distance to the system is determined to within a twentieth of a parsec and the component masses are determined at the level of a percent. n Pegasi is a well-known, nearby triple star system consisting of a "wide" pair with semi-major axis 235 milli-arcseconds, one component of which is a single-line spectroscopic binary (semi-major axis 2.5 milli-arcseconds). Using high-precision differential astrometry and radial velocity observations, the masses for all three components are determined and the relative inclination between the wide and narrow pairs' orbits is found to be 43.8 ± 3.0 degrees, just over the threshold for the three body Kozai resonance. The system distance is determined to a fifth of a parsec, and is consistent with trigonometric parallax measurements. V819 Herculis is a well-studied triple star system consisting of a "wide" pair with 5.5 year period, one component of which is a 2.2-day period eclipsing single-line spectroscopic binary. Differential astrometry measurements from PHASES determine the relative inclination of the short- and long-period orbits. Finally, the prospects for finding planets that simultaneously circle both stars in a binary system are evaluated. Planet searches of this type would represent a complementary investigation to PHASES and contribute similar scientific results.
by Matthew Ward Muterspaugh.
Ph.D.
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Borgniet, Simon. "Recherche et caractérisation de planètes géantes autour d'étoiles massives et/ou jeunes de la Séquence Principale : modélisation de l'activité d'étoiles de type solaire et impact sur la détection de planètes de masse terrestre". Thesis, Université Grenoble Alpes (ComUE), 2015. http://www.theses.fr/2015GREAY063/document.

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La recherche des exoplanètes traverse aujourd'hui une période décisive. D'un côté, notre connaissance des planètes géantes gazeuses s'est considérablement développée, et l'objectif de la recherche est maintenant de caractériser leurs propriétés physiques et de mieux comprendre leurs mécanismes de formation et d'évolution. D'un autre côté, la précision et la stabilité des instruments ont atteint un niveau qui rend techniquement possible la détection de planètes telluriques situées dans la zone habitable de leur étoile. Cependant, les perturbations du signal dues à l'étoile elle-même constituent un obstacle important à cette avancée. Mon travail de thèse se situe à la rencontre de ces problématiques. Il a consisté d'une part en l'analyse de deux relevés de vitesses radiales visant des étoiles relativement exotiques pour la recherche d'exoplanètes: les étoiles naines de type AF massives. Ce travail a donné lieu à la première caractérisation de la population de planètes géantes autour de ces étoiles et a montré que les mécanismes de migration planétaire étaient au moins partiellement inhibés autour de ces étoiles par rapport aux étoiles de type FGKM. Dans un second temps, j'ai conduit les observations et l'analyse des premiers résultats de deux grands relevés de vitesses radiales débutés pendant ma thèse et visant à détecter des planètes géantes en orbite autour d'étoiles jeunes et proches. Ces étoiles jeunes sont les seules sources pour lesquelles une exploration complète des planètes géantes à toutes les séparations devient possible, par combinaison des techniques de vitesses radiales et de l'imagerie. Cette combinaison permettra de tester de manière unique les modèles de formation et d'évolution planétaire. Les résultats provisoires de ces relevés indiquent une absence de planètes géantes à très courte séparation (Jupiters chauds) autour de nos cibles. Un autre résultat intéressant est la découverte d'une binaire spectroscopique eccentrique au centre d'un système planétaire imagé à grande séparation. Pour compléter cette approche observationnelle et mieux évaluer la détectabilité des exoplanètes semblables à la Terre, j'ai étalonné et caractérisé un modèle entièrement paramétré de l'activité d'une étoile semblable au Soleil et de son impact sur les vitesses radiales. Je l'ai dans un premier temps étalonné en comparant ses résultats à ceux obtenus à partir d'observations des zones actives du Soleil, puis je l'ai utilisé pour caractériser l'impact de l'inclinaison de l'étoile sur le signal induit par l'activité. Ce modèle paramétré ouvre de très nombreuses possibilités, étant en effet potentiellement adaptable à des types d'étoiles et d'activité différents. Il permettrait ainsi de caractériser les perturbations en vitesses radiales attendues pour chaque cas testé, et donc à la fois de déterminer quelles étoiles et quels types d'activité sont les plus favorables pour la détection de planètes de masse terrestre dans la zone habitable. En explorant ces trois problématiques en apparence très diverses mais complémentaires, j'y ai retrouvé un motif commun, celui de l'importance des étoiles elles-mêmes et de la physique stellaire pour la recherche d'exoplanètes
The search for exoplanets has reached a decisive moment. On the one hand, our knowledge of giant gaseous planets has significantly developed, and the aim of the research is now to characterize their physical properties and to better understand the formation and evolution processes. On the other hand, the instrumental precision and stability have reached a level that makes it technically possible to detect telluric planets in the habitable zone of their host star. However, the signal alterations induced by the star itself definitely challenge this breakthrough. My PhD stands at the crossroads of these problems. It consisted first in the analysis of two radial velocity surveys dedicated to stars somewhat exotic to exoplanet searches: the massive AF dwarf stars. This work has led to the first characterization of the giant planet population found around these stars and has showed that the planetary migration mechanisms were at least partially inhibited around these stars compared to FGKM stars. I then made the observations and the first analysis of two radial velocity surveys dedicated to the search for giant planets around young, nearby stars. Young stars are the only sources for which a full exploration of the giant planets at all separations can be reached, through the combination of radial velocities techniques and direct imaging. Such a combination will allow to test uniquely the planetary formation and evolution processes. The first results of these surveys show an absence of giant planets at very short separations (Hot Jupiters) around our targets. Another interesting result is the detection of an eccentric spectroscopic binary at the center of a planetary system imaged at a wide separation. To complete this observational approach and better estimate the detectability of Earth-like planets, I calibrated and characterized a fully parameterized model of the activity pattern of a Sun-like star and its impact on the radial velocities. I first calibrated it by comparing it to the results obtained with observations of the solar active structures, and then characterized the impact of stellar inclination on the activity-induced signal. Such a fully parameterized model is potentially adaptable to different types of stars and of activity and would thus allow to characterize the expected radial velocity jitter for each tested case, and then allow both to determine which types of stars and of activity patterns are the most favorable for detecting Earth-like planets in the habitable zone. While investigating these three seemingly different but complementary topics, I found that they shared a basic feature, namely the importance of the stars themselves and of stellar physics in exoplanet searches
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Leigh, Christopher. "The detection and characterisation of extrasolar planets". Thesis, University of St Andrews, 2004. http://hdl.handle.net/10023/12943.

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Since the discovery of 51 Pegasi b in 1995, continued observations have indirectly identified over 110 planetary objects. These Jupiter-mass objects cause their host star to "wobble" slightly about the common centre-of-mass of the system, which is detectable as radial motion in high-precision Doppler spectroscopy. Of the known planets, approximately 20% are found to orbit within 0.1 AU of the star, whilst the transit of HD209458 has inferred the gas-giant nature of these close-in extrasolar giant planets (CEGPs). The discovery of CEGPs has produced a wave of speculative theory as to the exact nature of these objects, and how they came to exist so close to their parent star. Our spectroscopic technique provides a method of achieving the direct detection of a CEGP atmosphere, the results of which will allow us to test emerging models that aim to predict the atmospheric nature of CEGPs and may provide additional information on the orbital inclination and mass of the planet. We start with a historical review of the field of extrasolar planets, followed by an introduction to the fundamental concepts which underpin the reflection of starlight from a planet's surface. We then investigate the prospects of detecting such a reflection, before detailing the technique we have devised and applied here to two known CEGP hosts. In the first instance, r Bootis, we combined observations at the 4.2-m William Herschel telescope in 1998, 1999 and 2000. The dataset comprised 893 high-resolution échelle spectra with a total integration time of 75hr 32min spanning 17 nights. We establish an upper limit on the planet's geometric albedo p < 0.39 (at the 99.9% significance level) at the most probable orbital inclination i ~ 36 deg, assuming a grey albedo, a Venus-like phase function and a planetary radius Rp - 1.2RJup. Although a weak candidate signal appears near to the most probable radial velocity amplitude, its statistical significance is insufficient for us to claim a detection with any confidence. In the second instance, HD75289, 4 nights of VLT(UT2)/UVES observations were secured in 2003 Jan, yielding 684 high-resolution spectra with a total integration time of 26 hours. We establish an upper limit on the planet's geometric albedo p < 0.12 (to the 99.9% significance level) at the most probable orbital inclination i ~/= 60 deg, assuming a grey albedo, a Venus-like phase function and a planetary radius Rp = 1.6RJup. In both cases, we are able to rule out some combinations of the predicted planetary radius and atmospheric albedo models with high, reflective cloud decks.
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Herrero, Casas Enrique. "Stellar activity in exoplanet hosts". Doctoral thesis, Universitat de Barcelona, 2014. http://hdl.handle.net/10803/284220.

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Most of the efforts on the search and characterization of Earth-like exoplanets are currently focused on low mass stars. Some important properties related to the structure and processes in this type of stars are still unknown, so a careful characterization is essential as one of the next steps in exoplanet sciences. The characterization of stellar activity in low mass stars was carried out through several techniques that allowed us both to model and to simulate the relationships between the observational data and the stellar properties. Several empyrical relations for low mass stars allow to find correlations between certain activity indicators and the rotation period. These have permitted us to generate synthetic samples of stars with stochastic distributions of stellar and geometric properties allowing to estimate the inclination of the rotation axis from the distribution in the activity-vsini diagram. The methodology was applied to a sample of 1200 observed low mass stars and the best candidates for a targeted transit search were selected. Spot modelling techniques allow to obtain physical information about the stellar surface from time series photometric and spectroscopic data. In this work we analyse Kepler photometry of LHS 6343 A, an M-dwarf being eclipsed by a brown dwarf companion every 12.718 days, and showing photometric oscillations with the same periodicity and a phase lag of 100º from the eclipses. The accurate modeling of the Kepler data allowed to explain these oscillations with the presence of active regions appearing at a fixed longitude, thus suggesting a possible magnetic connection between both components. On the other hand, we also studied an alternative explanation for the photometric oscillations in LHS 6343 A in terms of the Doppler beaming effect, showing that this could be the main cause of the observed oscillations. Stellar activity effects are responsible for the noise observed at different amplitude and timescales on time series data. Such noise represents one of the main limitations for exoplanetary sciences. In order to characterize it, we designed a methodology to simulate the photosphere of an active rotating star through the integration of small surface elements from Phoenix atmosphere models. This allows to characterize the signal produced by activity and further study its relationship with the stellar properties, as well as the possible effects produced on exoplanet measurements. The methodology allowed us to present several strategies in order to correct or reduce the effects of spots on the photometry of exoplanet transits, as these may induce significant variations on the measurement of the planetary radius. We focused on a comprehensive analysis of HD 189733, a K5 star hosting a giant planet, which has simultaneous photometric (MOST) and spectroscopic (SOPHIE) data available. An accurate surface map was obtained using the methodology above, accurately reproducing the light curve and radial velocity observations. Such map was used in order to study the effects of activity on the exoplanet transits. We showed that the effects of spot-crossing events are significant even for mid-infrared wavelengths. Moreover, the chromatic effects of spots not occulted by the planet show a signal with a wavelength dependence and amplitude that are very similar to the signature of the atmosphere of a planet dom- inated by dust. The radial velocity theoretical curve is in agreement with the observations up to the typical instrumental systematics of SOPHIE. The results from this work conclude that it is essential to correctly model the stellar activity signals for exoplanetary sciences, and we provide some tools and strategies to characterize and reduce such effects and extract astrophysical information.
Actualment, la major part dels esforços per la cerca i caracterització d’exoplanetes de tipus terrestre es centren en aquells que orbiten estrelles de baixa massa. Algunes de les característiques importants de l’estructura i els processos d’aquest tipus d’estrelles són encara poc coneguts, i per tant és important fer-ne un estudi acurat com un dels següents passos en el camp de l’exoplanetologia. En concret, el senyal produïit pels fenòmens d’activitat estel•lar, degut a la presència de taques i fàcules, introdueix variacions en les mesures fotomètriques i espectroscòpiques amb una periodicitat modulada per la rotació de l’estrella. En aquesta tesi s’ha realitzat un estudi dels fenòmens d’activitat a la fotosfera d’estrelles de baixa massa a través de diverses tècniques que ens han permès modelitzar o bé simular les relacions entre les propietats estel•lars i les dades observables. La simulació de mostres estadístiques d’estrelles basada en les relacions conegudes entre l’activitat estel•lar i la rotació ha permés implementar una tècnica per estimar la inclinació de l’eix de les estrelles a partir de mesures espectroscòpiques, resultant en un catàleg amb les millors candidates per una cerca de planetes amb trànsits. Per a la caracterització dels fenòmens relacionats amb l’activitat i un estudi acurat dels seus efectes sobre les mesures i cerques d’exoplanetes, s’ha aprofitat la disponibilitat de dades fotomètriques de Kepler juntament amb tècniques de modelització de taques, centrant-nos particularment en l’estudi de LHS 6343 A per obtenir informació d’activitat en la seva superfície. A més, s’ha dissenyat un simulador dels efectes d’activitat a la fotosfera basat en tècniques d’integració de superfície i models d’atmosfera Phoenix, que permet obtenir sèries temporals de dades sintètiques i estudiar els efectes de les regions actives sobre les mesures de trànsits de planetes. En particular, s’ha modelat el cas de HD189733. Els resultats d’aquest treball conclouen que és essencial una correcta modelització del senyal de l’activitat estel•lar en el camp de l’exoplanetologia, i es proporcionen algunes eines i estratègies per tal de caracteritzar i corregir aquests efectes i obtenir-ne informació astrofísica.
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Libros sobre el tema "Extrasolare Planeten"

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Formation and evolution of exoplanets. Weinheim: Wiley-VCH, 2010.

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Scholz, Mathias. Planetologie extrasolarer Planeten. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-41749-8.

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Scholz, Mathias. Planetologie extrasolarer Planeten. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-662-44445-0.

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Boss, Alan. Looking for earths: The race to find new solar systems. New York: John Wiley, 1998.

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Planet quest: The epic discovery of alien solar systems. New York: Oxford University Press, 1999.

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Planet quest: The epic discovery of alien solar systems. New York: Free Press, 1997.

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Croswell, Ken. Planet quest: The epic discovery of alien solar systems. San Diego: Harcourt Brace, 1998.

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Planet quest: The epic discovery of alien solar systems. New York: Oxford University Press, 1997.

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Extrasolar planets. Berlin, GE: Springer, 2005.

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Scharf, Caleb A. Extrasolar planets and astrobiology. Sausalito, Calif: University Science Books, 2008.

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Capítulos de libros sobre el tema "Extrasolare Planeten"

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Lemmer, Boris, Benjamin Bahr y Rina Piccolo. "Extrasolare Planeten". En Quirky Quarks, 67–70. Berlin, Heidelberg: Springer Berlin Heidelberg, 2016. http://dx.doi.org/10.1007/978-3-662-50259-4_17.

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Strassmeier, Klauz G. "Extrasolare Planeten: Endlich!" En Aktive Sterne, 351–68. Vienna: Springer Vienna, 1997. http://dx.doi.org/10.1007/978-3-7091-6863-9_12.

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Scholz, Mathias. "Physischer Aufbau extrasolarer Planeten". En Planetologie extrasolarer Planeten, 285–470. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-662-44445-0_5.

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Bahr, Benjamin, Boris Lemmer y Rina Piccolo. "Extrasolar Planets". En Quirky Quarks, 66–69. Berlin, Heidelberg: Springer Berlin Heidelberg, 2016. http://dx.doi.org/10.1007/978-3-662-49509-4_17.

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Reid, I. Neill y Suzanne L. Hawley. "Extrasolar planets". En New Light on Dark Stars, 391–419. London: Springer London, 2000. http://dx.doi.org/10.1007/978-1-4471-3663-7_10.

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Ford, Dominic. "Extrasolar Planets". En The Patrick Moore Practical Astronomy Series, 205–14. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4939-0629-1_10.

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Guenther, Eike W. "Extrasolar Planets". En Cellular Origin, Life in Extreme Habitats and Astrobiology, 101–20. Dordrecht: Springer Netherlands, 2012. http://dx.doi.org/10.1007/978-94-007-4966-5_8.

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Marov, Mikhail Ya. "Extrasolar Planets". En The Fundamentals of Modern Astrophysics, 205–23. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4614-8730-2_7.

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Scholz, Mathias. "Eine kurze Geschichte der Exoplanetenforschung". En Planetologie extrasolarer Planeten, 1–18. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-662-44445-0_1.

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Scholz, Mathias. "Was ist ein Planet?" En Planetologie extrasolarer Planeten, 19–20. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-662-44445-0_2.

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Actas de conferencias sobre el tema "Extrasolare Planeten"

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Labeyrie, Antoine y Herve Le Coroller. "Extrasolar planet imaging". En SPIE Astronomical Telescopes + Instrumentation, editado por Wesley A. Traub. SPIE, 2004. http://dx.doi.org/10.1117/12.550071.

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Ferlet, Roger, N. Mebarki y J. Mimouni. "The Realm of Extrasolar Planets". En THE THIRD ALGERIAN WORKSHOP ON ASTRONOMY AND ASTROPHYSICS. AIP, 2010. http://dx.doi.org/10.1063/1.3518332.

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Tremaine, Scott. "Extrasolar Planet Orbits and Eccentricities". En THE SEARCH FOR OTHER WORLDS: Fourteenth Astrophysics Conference. AIP, 2004. http://dx.doi.org/10.1063/1.1774531.

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Bennett, David P., Ian Bond, Edward Cheng, Scott Friedman, Peter Garnavich, B. Scott Gaudi, Ronald Gilliland et al. "The Microlensing Planet Finder: completing the census of extrasolar planets in the Milky Way". En SPIE Astronomical Telescopes + Instrumentation, editado por John C. Mather. SPIE, 2004. http://dx.doi.org/10.1117/12.551305.

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Lloyd, James P., Benjamin F. Lane, Mark R. Swain, John W. Storey, Tony Travouillon, Wesley A. Traub y Christopher K. Walker. "Extrasolar planet science with the Antarctic planet interferometer". En Optical Science and Technology, SPIE's 48th Annual Meeting, editado por Daniel R. Coulter. SPIE, 2003. http://dx.doi.org/10.1117/12.506895.

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Unwin, Stephen. "Space-Based Detection of Extrasolar Planets". En Space 2005. Reston, Virigina: American Institute of Aeronautics and Astronautics, 2005. http://dx.doi.org/10.2514/6.2005-6671.

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McCarthy, Chris. "Detection and Characterization of Extrasolar Planets". En THE SEARCH FOR OTHER WORLDS: Fourteenth Astrophysics Conference. AIP, 2004. http://dx.doi.org/10.1063/1.1774492.

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Dvorak, Rudolf, Marko Robnik y Valery Romanovski. "Extrasolar planets—A challenge for Astronomy". En LET’S FACE CHAOS THROUGH NONLINEAR DYNAMICS: Proceedings of “Let’s Face Chaos Through Nonlinear Dynamics” 7th International Summer School and Conference. AIP, 2008. http://dx.doi.org/10.1063/1.3046269.

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Traub, Wesley A. "Coronagraphic telescopes for extrasolar planet searches". En Frontiers in Optics. Washington, D.C.: OSA, 2003. http://dx.doi.org/10.1364/fio.2003.thw3.

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Strojnik, Marija, Jorge L. Flores y Gonzalo Paez. "Interferometric layouts for extrasolar planet detection". En AeroSense '99, editado por Bjorn F. Andresen y Marija Strojnik. SPIE, 1999. http://dx.doi.org/10.1117/12.354490.

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Informes sobre el tema "Extrasolare Planeten"

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Macintosh, B. Direct Imaging of Warm Extrasolar Planets. Office of Scientific and Technical Information (OSTI), abril de 2005. http://dx.doi.org/10.2172/15016011.

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Evans, Julia Wilhelmsen. High-Contrast Imaging using Adaptive Optics for Extrasolar Planet Detection. Office of Scientific and Technical Information (OSTI), enero de 2006. http://dx.doi.org/10.2172/900101.

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Ullom, J., M. Cunningham, B. Macintosh, T. Miyazaki y S. Labov. ''High-Speed, Photon-Counting Camera for the Detection of Extrasolar Planets''. Office of Scientific and Technical Information (OSTI), febrero de 2003. http://dx.doi.org/10.2172/15003349.

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