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Journal articles on the topic 'Extrasolare Planeten'

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Published: 4 June 2021

Last updated: 14 February 2022

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Bührke, Thomas. "Extrasolare Planeten werden sichtbar." Physik in unserer Zeit 40, no. 1 (January 2009): 11. http://dx.doi.org/10.1002/piuz.200990001.

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Wiedemann, Günter, L. Drake Deming, Gordon L. Bjoraker, and 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, and M. Knapp. "Radio observations of HD 80606 near planetary periastron." Astronomy & Astrophysics 644 (December 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, and Richard Greenberg. "Extrasolar planet interactions." Proceedings of the International Astronomical Union 3, S249 (October 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, and Ronald Redmer. "Constraining planetary interiors with the Love number k2." Proceedings of the International Astronomical Union 6, S276 (October 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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Miller-Ricci, Eliza, Sara Seager, and Dimitar Sasselov. "The Atmospheres of Extrasolar Super-Earths." Proceedings of the International Astronomical Union 4, S253 (May 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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Ehrenreich, D., A. Lecavelier des Etangs, G. Hébrard, J. M. Désert, A. Vidal-Madjar, J. C. McConnell, C. D. Parkinson, G. E. Ballester, and R. Ferlet. "The hydrogen exosphere of exoplanet HD 209458b detected with HST/ACS." Proceedings of the International Astronomical Union 4, S253 (May 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, and 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 (October 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, and Matthias Grott. "Interior structure models of terrestrial exoplanets and application to CoRoT-7 b." Proceedings of the International Astronomical Union 5, H15 (November 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, no. 1 (2002): 144–46. http://dx.doi.org/10.1017/s0251107x00001383.

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Snellen, Ignas, Remco de Kok, Ernst de Mooij, Matteo Brogi, Bas Nefs, and Simon Albrecht. "Exoplanet atmospheres at high spectral resolution: A CRIRES survey of hot-Jupiters." Proceedings of the International Astronomical Union 6, S276 (October 2010): 208–11. http://dx.doi.org/10.1017/s1743921311020199.

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AbstractRecently, we presented the detection of carbon monoxide in the transmission spectrum of extrasolar planet HD209458b, using CRIRES, the Cryogenic high-resolution Infrared Echelle Spectrograph at ESO's Very Large Telescope (VLT). The high spectral resolution observations (R=100,000) provide a wealth of information on the planet's orbit, mass, composition, and even on its atmospheric dynamics. The new observational strategy and data analysis techniques open up a whole world of opportunities. We therefore started an ESO large program using CRIRES to explore these, targeting both transiting and non-transiting planets in carbon monoxide, water vapour, and methane. Observations of the latter molecule will also serve as a test-bed for METIS, the proposed mid-infrared imager and spectrograph for the European Extremely Large Telescope.

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Wurm, Gerhard. "Selective Aggregation Experiments on Planetesimal Formation and Mercury-Like Planets." Geosciences 8, no. 9 (August 21, 2018): 310. http://dx.doi.org/10.3390/geosciences8090310.

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Much of a planet’s composition could be determined right at the onset of formation. Laboratory experiments can constrain these early steps. This includes static tensile strength measurements or collisions carried out under Earth’s gravity and on various microgravity platforms. Among the variety of extrasolar planets which eventually form are (Exo)-Mercury, terrestrial planets with high density. If they form in inner protoplanetary disks, high temperature experiments are mandatory but they are still rare. Beyond the initial process of hit-and-stick collisions, some additional selective processing might be needed to explain Mercury. In analogy to icy worlds, such planets might, e.g., form in environments which are enriched in iron. This requires methods to separate iron and silicate at early stages. Photophoresis might be one viable way. Mercury and Mercury-like planets might also form due to the ferromagnetic properties of iron and mechanisms like magnetic aggregation in disk magnetic fields might become important. This review highlights some of the mechanisms with the potential to trigger Mercury formation.

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Alvarado-Montes, Jaime A., and Carolina García-Carmona. "Orbital decay of short-period gas giants under evolving tides." Monthly Notices of the Royal Astronomical Society 486, no. 3 (April 16, 2019): 3963–74. http://dx.doi.org/10.1093/mnras/stz1081.

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Abstract The discovery of many giant planets in close-in orbits and the effect of planetary and stellar tides in their subsequent orbital decay have been extensively studied in the context of planetary formation and evolution theories. Planets orbiting close to their host stars undergo close encounters, atmospheric photoevaporation, orbital evolution, and tidal interactions. In many of these theoretical studies, it is assumed that the interior properties of gas giants remain static during orbital evolution. Here, we present a model that allows for changes in the planetary radius as well as variations in the planetary and stellar dissipation parameters, caused by the planet’s contraction and change of rotational rates from the strong tidal fields. In this semi-analytical model, giant planets experience a much slower tidal-induced circularization compared to models that do not consider these instantaneous changes. We predict that the eccentricity damping time-scale increases about an order of magnitude in the most extreme case for too inflated planets, large eccentricities, and when the planet’s tidal properties are calculated according to its interior structural composition. This finding potentially has significant implications on interpreting the period–eccentricity distribution of known giant planets as it may naturally explain the large number of non-circularized, close period currently known. Additionally, this work may help to constrain some models of planetary interiors, and contribute to a better insight about how tides affect the orbital evolution of extrasolar systems.

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Cowen, Ron. "Atom & cosmos: It came from another galaxy: Extrasolar planet's origin traced to beyond milky way." Science News 178, no. 13 (December 9, 2010): 11. http://dx.doi.org/10.1002/scin.5591781312.

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Poser, Anna Julia, Nadine Nettelmann, and Ronald Redmer. "The Effect of Clouds as an Additional Opacity Source on the Inferred Metallicity of Giant Exoplanets." Atmosphere 10, no. 11 (October 30, 2019): 664. http://dx.doi.org/10.3390/atmos10110664.

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Atmospheres regulate the planetary heat loss and therefore influence planetary thermal evolution. Uncertainty in a giant planet’s thermal state contributes to the uncertainty in the inferred abundance of heavy elements it contains. Within an analytic atmosphere model, we here investigate the influence that different cloud opacities and cloud depths can have on the metallicity of irradiated extrasolar gas giants, which is inferred from interior models. In this work, the link between inferred metallicity and assumed cloud properties is the thermal profile of atmosphere and interior. Therefore, we perform coupled atmosphere, interior, and evolution calculations. The atmosphere model includes clouds in a much simplified manner; it includes long-wave absorption but neglects shortwave scattering. Within that model, we show that optically thick, high clouds have negligible influence, whereas deep-seated, optically very thick clouds can lead to warmer deep tropospheres and therefore higher bulk heavy element mass estimates. For the young hot Jupiter WASP-10b, we find a possible enhancement in inferred metallicity of up to 10% due to possible silicate clouds at ∼0.3 bar. For WASP-39b, whose observationally derived metallicity is higher than predicted by cloudless models, we find an enhancement by at most 50%. However, further work on cloud properties and their self-consistent coupling to the atmospheric structure is needed in order to reduce uncertainties in the choice of model parameter values, in particular of cloud opacities.

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Tabeshian, Maryam, and Paul A. Wiegert. "Detection and Characterization of Extrasolar Planets through Mean-motion Resonances. II. The Effect of the Planet’s Orbital Eccentricity on Debris Disk Structures." Astrophysical Journal 847, no. 1 (September 15, 2017): 24. http://dx.doi.org/10.3847/1538-4357/aa831f.

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"Water Found in Extrasolar Planet's Atmosphere." Physics Today, 2007. http://dx.doi.org/10.1063/pt.5.021018.

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