Gotowe bibliografie tematyczne / Extrasolar planets

Gotowa bibliografia na temat „Extrasolar planets”

Autor: Grafiati
Data publikacji: 4 czerwca 2021
Data aktualizacji: 1 sierpnia 2024

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Artykuły w czasopismach na temat "Extrasolar planets"

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Lissauer, J. J., G. W. Marcy i S. Ida. "Extrasolar planets". Proceedings of the National Academy of Sciences 97, nr 23 (17.10.2000): 12405–6. http://dx.doi.org/10.1073/pnas.210381997.

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Sasselov, Dimitar D. "Extrasolar planets". Nature 451, nr 7174 (styczeń 2008): 29–31. http://dx.doi.org/10.1038/451029a.

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Lissauer, Jack J. "Extrasolar planets". Nature 419, nr 6905 (wrzesień 2002): 355–58. http://dx.doi.org/10.1038/419355a.

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Cochran, William. "Extrasolar planets". Physics World 10, nr 7 (lipiec 1997): 31–36. http://dx.doi.org/10.1088/2058-7058/10/7/30.

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Cameron, Andrew Collier. "Extrasolar planets". Physics World 14, nr 1 (styczeń 2001): 25–32. http://dx.doi.org/10.1088/2058-7058/14/1/27.

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Wang, Chih-Yueh, i Yuxiang Peng. "Extrasolar Planets". Contemporary Physics 56, nr 2 (11.11.2014): 209–13. http://dx.doi.org/10.1080/00107514.2014.967724.

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Boss, Alan P. "Extrasolar Planets". Physics Today 49, nr 9 (wrzesień 1996): 32–38. http://dx.doi.org/10.1063/1.881516.

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Rauer, Heike, i Artie Hatzes. "Extrasolar planets and planet formation". Planetary and Space Science 55, nr 5 (kwiecień 2007): 535. http://dx.doi.org/10.1016/j.pss.2006.09.001.

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Kosso, Peter. "Detecting extrasolar planets". Studies in History and Philosophy of Science Part A 37, nr 2 (czerwiec 2006): 224–36. http://dx.doi.org/10.1016/j.shpsa.2005.05.001.

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Mayor, Michel, Alan P. Boss, Paul R. Butler, William B. Hubbard, Philip A. Ianna, Martin Kürster, Jack J. Lissauer i in. "COMMISSION 53: EXTRASOLAR PLANETS". Proceedings of the International Astronomical Union 4, T27A (grudzień 2008): 181–82. http://dx.doi.org/10.1017/s1743921308025465.

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Commission 53 on Extrasolar Planets was created at the 2006 Prague General Assembly of the IAU, in recognition of the outburst of astronomical progress in the field of extrasolar planet discovery, characterization, and theoretical work that has occurred since the discovery of the pulsar planets in 1992 and the discovery of the first planet in orbit around a solar-type star in 1995. Commission 53 is the logical successor to the IAU Working Group on Extrasolar Planets WG-ESP, which ended its six years of existence in August 2006. The founding president of Commission 53 is Michael Mayor, in honor of his seminal contributions to this new field of astronomy. The vice-president is Alan Boss, the former chair of the WG-ESP, and the members of the Commission 53 Organizing Committee are the other former members of the WG-ESP.
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Rozprawy doktorskie na temat "Extrasolar 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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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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Hood, Ben Andrew Ashcom. "Extrasolar planet search and characterisation". Thesis, St Andrews, 2007. http://hdl.handle.net/10023/359.

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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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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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Doellinger, Michaela. "Hunting for extrasolar planets around K giants". Diss., lmu, 2008. http://nbn-resolving.de/urn:nbn:de:bvb:19-99700.

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Nikku, Madhusudhan 1980. "Retrieval of atmospheric properties of extrasolar planets". Thesis, Massachusetts Institute of Technology, 2009. http://hdl.handle.net/1721.1/63006.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, 2009.
Cataloged from PDF version of thesis.
Includes bibliographical references (p. 133-137).
We present a new method to retrieve molecular abundances and temperature profiles from exoplanet atmosphere photometry and spectroscopy. Our method allows us to run millions of 1-D atmosphere models in order to cover the large range of allowed parameter space. In order to run such a large number of models, we have developed a parametric pressure-temperature (P-T) profile coupled with line-by-line radiative transfer, hydrostatic equilibrium, and energy balance, along with prescriptions for non-equilibrium molecular composition and energy redistribution. The major difference from traditional 1-D radiative transfer models is the parametric P-T profile, which essentially means adopting energy balance only at the top of the atmosphere and not in each layer. We see the parametric P-T model as a parallel approach to the traditional exoplanet atmosphere models that rely on several free parameters to encompass unknown absorbers and energy redistribution. The parametric P-T profile captures the basic physical features of temperature structures in planetary atmospheres (including temperature inversions), and reproduces a wide range of published P-T profiles, including those of solar system planets. We apply our temperature and abundance retrieval method to two exoplanets which have the best data available, HD 189733b and HD 209458b. For each planet, we compute - 107 atmospheric spectra on a grid in the parameter space, and report contours of the error surface, given the data. For the day-side of HD 189733b, we place constraints on the atmospheric properties based on three different data sets available. Our best-fit models to one of the data sets allow for very efficient daynight energy redistribution in HD 189733b. The different constraints on molecular abundances confirm the presence of H20, CH4 , CO and CO 2 in HD 189733b. Our results also rule out the presence of a thermal inversion in this planet. The model constraints due to the different data sets indicate that the planetary atmosphere is variable, both, in its energy redistribution state and in the chemical abundances. The variability is evident in the data; some key observations with different instruments at the same wavelength differ at the - 2- level. If, on the other hand, the differences in data represent underestimated errors, and if all the data sets have to be reconciled simultaneously, then we are unable to make specific constraints on the molecular abundances or on the temperature profile, beyond identification of molecules and the presence or absence of a thermal inversion. For HD 209458b, we confirm and constrain a thermal inversion in the day-side atmosphere, and the data allows for very efficient day-night redistribution of energy. We report detection of CO, CH4 and CO 2 on the dayside of HD 209458b, along with placing an upper-limit on the amount of H2 0. We also report atmospheric models for three transiting exoplanets with limited data: TrES-2, HAT-P-7b, GJ 436b. For TrES-2 and HAT-P-7b, where only four observations each are available, we find that the data can be fit with models with and without thermal inversions, if we make no assumptions of chemical equilibrium. Finally, in this work, we report the first steps towards developing a parameter estimation procedure for exoplanetary atmospheres. We demonstrate with simulated data that our model can be used with a formal Bayesian parameter estimation algorithm, like MCMC, to place constraints on the atmospheric properties of hot Jupiters.
by Nikku, Madhusudhan.
Ph.D.
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Kipping, D. M. "The transits of extrasolar planets with moons". Thesis, University College London (University of London), 2011. http://discovery.ucl.ac.uk/1306758/.

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The search for extrasolar planets is strongly motivated by the goal of characterizing how frequent habitable worlds and life may be within the Galaxy. Whilst much effort has been spent on searching for Earth-like planets, large moons may also be common, temperate abodes for life as well. The methods to detect extrasolar moons, or “exomoons” are more subtle than their planetary counterparts and in this thesis I aim to provide a method to find such bodies in transiting systems, which offer the greatest potential for detection. Before one can search for the tiny perturbations to the planetary signal, an understanding of the planetary transit must be established. Therefore, in Chapters 3 to 5 I discuss the transit model and provide several new insights. Chapter 4 presents new analytic expressions for the times of transit minima and the transit duration, which will be critical in the later search for exomoons. Chapter 5 discusses two sources of distortion to the transit signal, namely blending (with a focus on the previously unconsidered self-blending scenario) and light curve smearing due to long integration times. I provide methods to compensate for both of these effects, thus permitting for the accurate modelling of the planetary transit light curve. In Chapter 6, I discuss methods to detect exomoons through their gravitational influence on the host planet, giving rise to transit timing and duration variations (TTV and TDV). The previously known TTV effect is updated with a new model and the associated critical problems are outlined. I then predict a new effect, TDV, which solves these problems, making exomoon detection viable. Chapter 7 presents a feasibility study for detecting habitable-zone exomoons with Kepler, where it is found that moons down to 0.2M⊕ are detectable. Finally, conclusions and future work are discussed in Chapter 8.
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Gaudi, B. Scott. "Microlensing and the search for extrasolar planets /". The Ohio State University, 2000. http://rave.ohiolink.edu/etdc/view?acc_num=osu1488199501405399.

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Lewis, Nikole Kae. "Atmospheric Circulation of Eccentric Extrasolar Giant Planets". Diss., The University of Arizona, 2012. http://hdl.handle.net/10150/242352.

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This dissertation explores the three-dimensional coupling between radiative and dynamical processes in the atmospheres of eccentric extrasolar giant planets GJ436b, HAT-P-2b, and HD80606b. Extrasolar planets on eccentric orbits are subject to time-variable heating and probable non-synchronous rotation, which results in significant variations in global circulation and thermal patterns as a function of orbital phase. Atmospheric simulations for the low eccentricity (e=0.15) Neptune sized planet GJ436b reveal that when Neptune-like atmospheric compositions are assumed day/night temperature contrasts and equatorial jet speeds are significantly increased relative to models that assume a solar-like composition. Comparisons between our theoretical light curves and recent observations support a high metallicity atmosphere with disequilibrium carbon chemistry for GJ436b. The analysis of full-orbit light curve observations at 3.6 and 4.5 microns of the HAT-P-2 system reveal swings in the planet's temperature of more than 900 K during its significantly eccentric (e=0.5) orbit with a four to six hour offset between periapse passage and the peak of the planet's observed flux. Comparisons between our atmospheric model of HAT-P-2b and the observed light curves indicate an increased carbon to oxygen ratio in HAT-P-2b's atmosphere compared to solar values. Atmospheric simulations of the highly eccentric (e=0.9) HD80606b show that flash-heating events completely alter planetary thermal and jet structures and that assumptions about the rotation period of this planet could affect the shape of light curve observations near periapse. Our simulations of HD80606b also show the development an atmospheric shock on the nightside of the planet that is associated with an observable thermal signature in our theoretical light curves. The simulations and observations presented in this dissertation mark an important step in the exploration of atmospheric circulation on the more than 300 exoplanets known to possess significantly non-zero eccentricities.
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Książki na temat "Extrasolar planets"

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Deeg, Hans, Juan Antonio Belmonte i Antonio Aparicio, red. Extrasolar Planets. Cambridge: Cambridge University Press, 2007. http://dx.doi.org/10.1017/cbo9780511536533.

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

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von Braun, Kaspar, i Tabetha Boyajian. Extrasolar Planets and Their Host Stars. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-61198-3.

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R, Dvorak, red. Extrasolar planets: Formation, detection and dynamics. Weinheim [Germany]: Wiley-VCH, 2008.

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R, Dvorak, red. Extrasolar planets: Formation, detection and dynamics. Weinheim [Germany]: Wiley-VCH, 2008.

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World Book, Inc. Alien planets. Chicago, IL: World Book, 2010.

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Inc, World Book, red. Alien planets. Chicago, IL: World Book, 2010.

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Goldsmith, Donald. Worlds unnumbered: The search for extrasolar planets. Sausalito, Calif: University Science Books, 1997.

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Kipping, David M. The Transits of Extrasolar Planets with Moons. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-22269-6.

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service), SpringerLink (Online, red. The Transits of Extrasolar Planets with Moons. Berlin, Heidelberg: Springer-Verlag Berlin Heidelberg, 2011.

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Części książek na temat "Extrasolar planets"

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Marov, Mikhail Ya. "Extrasolar Planets". W 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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Guenther, Eike W. "Extrasolar Planets". W 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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Reid, I. Neill, i Suzanne L. Hawley. "Extrasolar planets". W 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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Bahr, Benjamin, Boris Lemmer i Rina Piccolo. "Extrasolar Planets". W 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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Ford, Dominic. "Extrasolar Planets". W 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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Khare, Pushpa. "Extrasolar Planets". W Astronomers' Universe, 83–92. Cham: Springer International Publishing, 2023. http://dx.doi.org/10.1007/978-3-031-29639-0_5.

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Hanslmeier, Arnold. "Water on Extrasolar Planets?" W Water in the Universe, 129–51. Dordrecht: Springer Netherlands, 2011. http://dx.doi.org/10.1007/978-90-481-9984-6_6.

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Kipping, David M. "Extrasolar Moons". W The Transits of Extrasolar Planets with Moons, 25–35. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-22269-6_2.

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Poppenhaeger, Katja. "Extrasolar Planets and Star-Planet Interaction". W Handbook of X-ray and Gamma-ray Astrophysics, 3347–64. Singapore: Springer Nature Singapore, 2024. http://dx.doi.org/10.1007/978-981-19-6960-7_84.

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Poppenhaeger, Katja. "Extrasolar Planets and Star-Planet Interaction". W Handbook of X-ray and Gamma-ray Astrophysics, 1–19. Singapore: Springer Nature Singapore, 2022. http://dx.doi.org/10.1007/978-981-16-4544-0_84-1.

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Streszczenia konferencji na temat "Extrasolar planets"

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

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Dvorak, Rudolf, Marko Robnik i Valery Romanovski. "Extrasolar planets—A challenge for Astronomy". W 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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Unwin, Stephen. "Space-Based Detection of Extrasolar Planets". W 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". W THE SEARCH FOR OTHER WORLDS: Fourteenth Astrophysics Conference. AIP, 2004. http://dx.doi.org/10.1063/1.1774492.

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Spreeuw, Hanno, Jean-Mathias Griessmeier i Philippe Zarka. "Predictions for Radio Emission from Extrasolar Planets". W Bursts, Pulses and Flickering: wide-field monitoring of the dynamic radio sky. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.056.0007.

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Meinel, Aden B., i Marjorie P. Meinel. "Infrared and the search for extrasolar planets". W San Diego, '91, San Diego, CA, redaktorzy Bjorn F. Andresen, Marija Scholl i Irving J. Spiro. SPIE, 1991. http://dx.doi.org/10.1117/12.48730.

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Ireland, Michael J. "Detecting extrasolar planets with sparse aperture masking". W SPIE Astronomical Telescopes + Instrumentation, redaktorzy Françoise Delplancke, Jayadev K. Rajagopal i Fabien Malbet. SPIE, 2012. http://dx.doi.org/10.1117/12.928884.

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Redmer, Ronald, Nadine Nettelmann, Ulrike Kramm, Bastian Holst, Winfried Lorenzen, Martin French, Mark Elert i in. "INTERIOR OF SOLAR AND EXTRASOLAR GIANT PLANETS". W SHOCK COMPRESSION OF CONDENSED MATTER 2009: Proceedings of the American Physical Society Topical Group on Shock Compression of Condensed Matter. AIP, 2009. http://dx.doi.org/10.1063/1.3295290.

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Ivanov, V. D., C. Caceres, D. Naef, E. Mason, F. Selman, C. Melo, D. Minniti i in. "High-cadence transit timing observations of extrasolar planets". W HIGH TIME RESOLUTION ASTROPHYSICS: The Universe at Sub-Second Timescales. AIP, 2008. http://dx.doi.org/10.1063/1.2896949.

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Parry, Ian R., Esperanza Carrasco i Frederick G. Watson. "Multifiber photometry: a technique for detecting extrasolar planets". W 1994 Symposium on Astronomical Telescopes & Instrumentation for the 21st Century, redaktorzy David L. Crawford i Eric R. Craine. SPIE, 1994. http://dx.doi.org/10.1117/12.176815.

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Raporty organizacyjne na temat "Extrasolar planets"

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

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

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

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Możesz być także zainteresowany rozszerzonymi bibliografiami na temat „Extrasolar planets” dla poszczególnych typów źródeł:
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