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Journal articles on the topic 'Extrasolar planets'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

Lissauer, J. J., G. W. Marcy, and S. Ida. "Extrasolar planets." Proceedings of the National Academy of Sciences 97, no. 23 (2000): 12405–6. http://dx.doi.org/10.1073/pnas.210381997.

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Sasselov, Dimitar D. "Extrasolar planets." Nature 451, no. 7174 (2008): 29–31. http://dx.doi.org/10.1038/451029a.

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Lissauer, Jack J. "Extrasolar planets." Nature 419, no. 6905 (2002): 355–58. http://dx.doi.org/10.1038/419355a.

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4

Cochran, William. "Extrasolar planets." Physics World 10, no. 7 (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, no. 1 (2001): 25–32. http://dx.doi.org/10.1088/2058-7058/14/1/27.

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6

Wang, Chih-Yueh, and Yuxiang Peng. "Extrasolar Planets." Contemporary Physics 56, no. 2 (2014): 209–13. http://dx.doi.org/10.1080/00107514.2014.967724.

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7

Boss, Alan P. "Extrasolar Planets." Physics Today 49, no. 9 (1996): 32–38. http://dx.doi.org/10.1063/1.881516.

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8

Rauer, Heike, and Artie Hatzes. "Extrasolar planets and planet formation." Planetary and Space Science 55, no. 5 (2007): 535. http://dx.doi.org/10.1016/j.pss.2006.09.001.

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9

Kosso, Peter. "Detecting extrasolar planets." Studies in History and Philosophy of Science Part A 37, no. 2 (2006): 224–36. http://dx.doi.org/10.1016/j.shpsa.2005.05.001.

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10

Mayor, Michel, Alan P. Boss, Paul R. Butler, et al. "COMMISSION 53: EXTRASOLAR PLANETS." Proceedings of the International Astronomical Union 4, T27A (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

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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 (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,

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Marcy, Geoffrey W., R. Paul Butler, Steven S. Vogt, and Debra A. Fischer. "Extrasolar Planets and Prospects for Terrestrial Planets." Symposium - International Astronomical Union 213 (2004): 11–24. http://dx.doi.org/10.1017/s0074180900192903.

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Examination of ∼2000 sun–like stars has revealed 97 planets (as of 2002 Nov), all residing within our Milky Way Galaxy and within ∼200 light years of our Solar System. They have masses between 0.1 and 10 times that of Jupiter, and orbital sizes of 0.05–5 AU. Thus planets occupy the entire detectable domain of mass and orbits. News & summaries about extrasolar planets are provided at: http://exoplanets.org. These planets were all discovered by the wobble of the host stars, induced gravitationally by the planets, causing a periodicity in the measured Doppler effect of the starlight. Earth–ma

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Bond, Jade C., Dante S. Lauretta, and David P. O'Brien. "The Diversity of Extrasolar Terrestrial Planets." Proceedings of the International Astronomical Union 5, S265 (2009): 399–402. http://dx.doi.org/10.1017/s1743921310001079.

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AbstractExtrasolar planetary host stars are enriched in key planet-building elements. These enrichments have the potential to drastically alter the building blocks available for terrestrial planet formation. Here we report on the combination of dynamical models of late-stage terrestrial planet formation within known extrasolar planetary systems with chemical equilibrium models of the composition of solid material within the disk. This allows us to constrain the bulk elemental composition of extrasolar terrestrial planets. A wide variety of resulting planetary compositions exist, ranging from t

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Marcy, G. W., R. Paul Butler, and D. A. Fischer. "Doppler Detection of Extrasolar Planets." International Astronomical Union Colloquium 170 (1999): 121–30. http://dx.doi.org/10.1017/s0252921100048466.

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AbstractWe have measured the radial velocities of 540 G and K main sequence stars with a precision of 3−10 ms−1 using the Lick and Keck échelle spectrometers. We had detected 6 companions that have m sin i < 7 MJup. We announce here the discovery of a new planet around Gliese 876, found in our Doppler measurements from both Lick and Keck. This is the first planet found around an M dwarf, which indicates that planets occur around low-mass stars, in addition to solar-type stars. We combine our entire stellar sample with that of Mayor et al. to derive general properties of giant planets within

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15

McGruder, Charles H., Mark E. Everett, and Steve B. Howell. "The STARBASE Network of Telescopes and the Detection of Extrasolar Planets." International Astronomical Union Colloquium 183 (2001): 23–30. http://dx.doi.org/10.1017/s0252921100078556.

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AbstractA network of longitudinally spaced imaging telescopes is described. Due to the limitations of the radial velocity method extrasolar planets have only been found around bright stars (less than 10 mag). Employment of the network and the photometric method to detect extrasolar planets will lead to the discovery of extrasolar planets at much fainter magnitudes (less than 19 mag).

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16

Skinner, J. W., and J. Y.-K. Cho. "Modons on tidally synchronized extrasolar planets." Monthly Notices of the Royal Astronomical Society 511, no. 3 (2022): 3584–601. http://dx.doi.org/10.1093/mnras/stab2809.

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ABSTRACT We investigate modons on tidally synchronized extrasolar planet atmospheres. Modons are dynamic, coherent flow structures composed of a pair of storms with opposite signs of vorticity. Modons are important because they can divert flows and lead to recognizable weather patterns. On synchronized planets, powered by the intense irradiation from the host star, large modons reach planetary-scale in size and exhibit quasi-periodic life-cycles – chaotically moving around the planet, breaking and reforming many times over long durations (e.g. thousands of planet days). Additionally, the modon

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Barnes, Rory, and Richard Greenberg. "Extrasolar planet interactions." Proceedings of the International Astronomical Union 3, S249 (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

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Butler, R. Paul, Geoffrey W. Marcy, Debra A. Fischer, et al. "Statistical Properties of Extrasolar Planets." Symposium - International Astronomical Union 202 (2004): 3–11. http://dx.doi.org/10.1017/s0074180900217397.

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The emerging statistical properties from the first 50 extrasolar planets are startlingly different from the picture that was imagined prior to 1995. About 0.75% of nearby solar type stars harbor jovian planets in 3 to 5 day circular orbits. Another ∽7% of stars have jupiter–mass companions orbiting in eccentric orbits within 3.5 AU. The mass distribution of substellar companions rises abruptly near 5 MJup and continues increasing down to the detection limit near 1 MJup-Orbital eccentricities correlate positively with semimajor axes, even for planets beyond the tidal circularization zone within

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Deeg, Hans J., Keith Horne, Fabio Favata, et al. "Planet Detection Capabilities of the Eddington Mission." Symposium - International Astronomical Union 202 (2004): 448–50. http://dx.doi.org/10.1017/s0074180900218469.

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Eddington is a space mission for extrasolar planet finding and for asteroseismic observations. It has been selected by ESA as an F2/F3 reserve mission with a potential implementation in 2008-13. Here we describe Eddington's capabilities to detect extrasolar planets, with an emphasis on the detection of habitable planets. Simulations covering the instrumental capabilities of Eddington and the stellar distributions in potential target fields lead to predictions of about 10,000 planets of all sizes and temperatures, and a few tens of terrestrial planets that are potentially habitable. Implication

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Mishra, Ruchi, Miljenko Čemeljić, Jacobo Varela, and Maurizio Falanga. "Auroras on Planets around Pulsars." Astrophysical Journal Letters 959, no. 1 (2023): L13. http://dx.doi.org/10.3847/2041-8213/ad0f1f.

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Abstract The first extrasolar planets were discovered serendipitously, by finding the slight variation in otherwise highly regular timing of the pulses, caused by the planets orbiting a millisecond pulsar. In analogy with the solar system planets, we predict the existence of aurora on planets around millisecond pulsars. We perform the first magnetohydrodynamic simulations of magnetospheric pulsar–planet interaction and estimate the radio emission from such systems. We find that the radio emission from aurora on pulsar planets could be observable with the current instruments. We provide paramet

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Marcy, Geoffrey W., R. Paul Butler, Steven S. Vogt, et al. "Five New Extrasolar Planets." Astrophysical Journal 619, no. 1 (2005): 570–84. http://dx.doi.org/10.1086/426384.

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22

Ksanfomality, L. V. "Transits of extrasolar planets." Solar System Research 41, no. 6 (2007): 463–82. http://dx.doi.org/10.1134/s0038094607060020.

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23

Gonzalez, G. "Extrasolar planets and ETI." Astronomy & Geophysics 39, no. 6 (1998): 6.8. http://dx.doi.org/10.1093/astrog/39.6.6.8.

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24

Boss, Alan, Alain Lecavelier des Etangs, Michel Mayor, et al. "COMMISSION 53: EXTRASOLAR PLANETS." Proceedings of the International Astronomical Union 7, T28A (2011): 138–40. http://dx.doi.org/10.1017/s1743921312002712.

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Bowler, Brendan P. "Imaging Extrasolar Giant Planets." Publications of the Astronomical Society of the Pacific 128, no. 968 (2016): 102001. http://dx.doi.org/10.1088/1538-3873/128/968/102001.

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26

Ehrenreich, D. "Evaporation of extrasolar planets." EAS Publications Series 41 (2010): 429–40. http://dx.doi.org/10.1051/eas/1041035.

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27

Santos, N. C. "Extrasolar Planets: Constraints for Planet Formation Models." Science 310, no. 5746 (2005): 251–55. http://dx.doi.org/10.1126/science.1100210.

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28

Matsumura, Soko, Genya Takeda, and Fred A. Rasio. "On the Origins of Eccentric Close-in Planets." Proceedings of the International Astronomical Union 4, S253 (2008): 189–95. http://dx.doi.org/10.1017/s1743921308026409.

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AbstractStrong tidal interaction with the central star can circularize the orbits of close-in planets. With the standard tidal quality factorQof our solar system, estimated circularization timescales for close-in extrasolar planets are typically shorter than the age of the host stars. While most extrasolar planets with orbital radiia≲ 0.1 AU indeed have circular orbits, some close-in planets with substantial orbital eccentricities have recently been discovered. This new class of eccentric close-in planets implies that either their tidalQfactor is considerably higher, or circularization is prev

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29

Doyle, Laurance R., and Hans-Jörg Deeg. "Timing Detection of Eclipsing Binary Planets and Transiting Extrasolar Moons." Symposium - International Astronomical Union 213 (2004): 80–84. http://dx.doi.org/10.1017/s0074180900193027.

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We investigate the improved detection of extrasolar planets around eclipsing binaries using eclipse minima timing and extrasolar moons around transiting planets using transit timing offered by the upcoming COROT (ESA, 2005), Kepler (NASA, 2007), and Eddington (ESA 2008) spacecraft missions. Hundreds of circum-binary planets should be discovered and a thorough survey of moons around transiting planets will be accomplished by these missions.

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30

Dvorak, Rudolf, Li-Yong Zhou, and Helmut Baudisch. "Trojans in Exosystems with Two Massive Planets." Proceedings of the International Astronomical Union 8, S293 (2012): 152–58. http://dx.doi.org/10.1017/s1743921313012726.

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AbstractWe take as dynamical model for extrasolar planetary systems a central star like our Sun and two giant planets m1 and m2 like Jupiter and Saturn. We change the mass ratio μ=m2/m1 of the two large planets for a wide range of 1/16 < μ < 16. We also change the ratio between the initial semi-major axes (ν=a2/a1) in the range of 1.2 < ν < 3 to model the different architecture of extrasolar planetary systems hosting two giant planets. The results for possible Trojans (Trojan planets) in the equilateral equilibrium points of the inner planet m1 and the outer planet m2 were derived

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Kalas, Paul. "Direct imaging of massive extrasolar planets." Proceedings of the International Astronomical Union 6, S276 (2010): 279–86. http://dx.doi.org/10.1017/s1743921311020321.

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AbstractThe direct detection of an extrasolar planet can provide accurate measurements of its orbit, mass and composition, greatly improving our understanding of how planets form and evolve. Recent advances in ground-based and space-based imaging techniques have now produced the first direct images of extrasolar planets. Typically these are many-Jupiter-mass planets on wide orbits. Direct imaging therefore probes the outer architecture of planetary systems and it is highly complementary to other techniques sensitive to inner architectures. This brief review summarizes the properties of the cur

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32

Cho, James Y. K. "Atmospheric dynamics of tidally synchronized extrasolar planets." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 366, no. 1884 (2008): 4477–88. http://dx.doi.org/10.1098/rsta.2008.0177.

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Tidally synchronized planets present a new opportunity for enriching our understanding of atmospheric dynamics on planets. Subject to an unusual forcing arrangement (steady irradiation on the same side of the planet throughout its orbit), the dynamics on these planets may be unlike that on any of the Solar System planets. Characterizing the flow pattern and temperature distribution on the extrasolar planets is necessary for reliable interpretation of data currently being collected, as well as for guiding future observations. In this paper, several fundamental concepts from atmospheric dynamics

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33

Padovan, S., T. Spohn, P. Baumeister, et al. "Matrix-propagator approach to compute fluid Love numbers and applicability to extrasolar planets." Astronomy & Astrophysics 620 (December 2018): A178. http://dx.doi.org/10.1051/0004-6361/201834181.

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Context.The mass and radius of a planet directly provide its bulk density, which can be interpreted in terms of its overall composition. Any measure of the radial mass distribution provides a first step in constraining the interior structure. The fluid Love numberk2provides such a measure, and estimates ofk2for extrasolar planets are expected to be available in the coming years thanks to improved observational facilities and the ever-extending temporal baseline of extrasolar planet observations.Aims.We derive a method for calculating the Love numbersknof any object given its density profile, w

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34

Mao, Shude, Eamonn Kerins, and Nicholas J. Rattenbury. "Extrasolar planet detections with gravitational microlensing." Proceedings of the International Astronomical Union 3, S249 (2007): 25–30. http://dx.doi.org/10.1017/s1743921308016311.

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AbstractMicrolensing light curves due to single stars are symmetric and typically last for a month. So far about 4000 microlensing events have been discovered in real-time, the vast majority toward the Galactic centre. The presence of planets around the primary lenses induces deviations in the usual light curve which lasts from hours (for an Earth-mass [M⊕] planet) to days (for a Jupiter-mass [Mj] planet). Currently the survey teams, OGLE and MOA, discover and announce microlensing events in real-time, and follow-up teams (together with the survey teams) monitor selected events intensively (us

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Ida, Shigeru, and D. N. C. Lin. "Orbital migration and mass-semimajor axis distributions of extrasolar planets." Proceedings of the International Astronomical Union 3, S249 (2007): 223–32. http://dx.doi.org/10.1017/s1743921308016633.

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AbstractHere we discuss the effects of type-I migration of protoplanetary embryos on mass and semimajor axis distributions of extrasolar planets. We summarize the results of Ida & Lin (2008a, 2008b), in which Monte Carlo simulations with a deterministic planet-formation model were carried out. The strength of type-I migration regulates the distribution of extrasolar gas giant planets as well as terrestrial planets. To be consistent with the existing observational data of extrasolar gas giants, the type-I migration speed has to be an order of magnitude slower than that given by the linear t

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36

Boss, Alan P., R. Paul Butler, William B. Hubbard, et al. "Working Group on Extrasolar Planets." Proceedings of the International Astronomical Union 1, T26A (2005): 183–86. http://dx.doi.org/10.1017/s1743921306004509.

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The Working Group on Extrasolar Planets (hereafter the WGESP) was created at a meeting of the IAU Executive Council in 1999 as a Working Group of IAU Division III and was renewed for three more years at the IAU General Assembly in 2003. The charge of the WGESP is to act as a focal point for international research on extrasolar planets. The membership of the WGESP has remained unchanged for the last three years.

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37

Farrell, W. M., T. Joseph W. Lazio, M. D. Desch, T. S. Bastian, and P. Zarka. "Radio Emission from Extrasolar Planets." Symposium - International Astronomical Union 213 (2004): 73–76. http://dx.doi.org/10.1017/s0074180900193003.

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By virtue of their planetary-scale magnetic fields, the Earth and all of the gas giants in our solar system possess solar-wind deformed magnetospheres. The magnetic polar regions of these “magnetic planets” produce intense, aurora-related radio emission from solar-wind powered electron currents. Simple scaling laws suggest that Jovian-mass planets close to their host stars should produce radio emission; detecting such emission would be the first direct detection of many of these planets. We describe searches using the Very Large Array (VLA) for radio emission from the planets orbiting HD 11476

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Kumar, Varnana M., Thara N. Sathyan, T. E. Girish, P. E. Eapen, Biju Longhinos, and J. Binoy. "Inference of Magnetic Fields and Space Weather Hazards of Rocky Extrasolar Planets From a Dynamical Geophysical Model." Proceedings of the International Astronomical Union 16, S362 (2020): 175–76. http://dx.doi.org/10.1017/s174392132200148x.

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AbstractIn this paper we have inferred the magnetic shielding characteristics and space weather hazards of selected potentially habitable extrasolar planets using a dynamical geophysical model from calculations of internal heat, phases of volcanism and planetary magnetic moments. The space weather hazards on the extrasolar planet Kepler-452b orbiting around a Sun-like star are found to be a minimum which enhances the habitability probability of this planet.

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39

Pilat-Lohinger, Elke. "The ultimate cataclysm: the orbital (in)stability of terrestrial planets in exoplanet systems including planets in binaries." International Journal of Astrobiology 8, no. 3 (2009): 175–82. http://dx.doi.org/10.1017/s1473550409990164.

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AbstractThere is no doubt that stability studies are of great importance in the fascinating research of extrasolar planetary systems. Even if most of the more than 300 extrasolar planets orbit their host stars as single giant planet and build simple two-body systems, we should not exclude the possibility that these systems could host other (small) planets that have not yet been detected due to obsevational limits. Another aspect to carry out stability studies is the growing interest in the search for extraterrestrial life in the universe. The long-term stability of a planetary system is one of

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40

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 emissio

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Moses, Julianne I. "Chemical kinetics on extrasolar planets." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 372, no. 2014 (2014): 20130073. http://dx.doi.org/10.1098/rsta.2013.0073.

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Chemical kinetics plays an important role in controlling the atmospheric composition of all planetary atmospheres, including those of extrasolar planets. For the hottest exoplanets, the composition can closely follow thermochemical-equilibrium predictions, at least in the visible and infrared photosphere at dayside (eclipse) conditions. However, for atmospheric temperatures , and in the uppermost atmosphere at any temperature, chemical kinetics matters. The two key mechanisms by which kinetic processes drive an exoplanet atmosphere out of equilibrium are photochemistry and transport-induced qu

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Brown, Timothy M. "Extrasolar Planet Transit Observations—Findings and Prospects." Symposium - International Astronomical Union 202 (2004): 52–59. http://dx.doi.org/10.1017/s0074180900217452.

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We now know of one extrasolar planet, HD 209458 b, that is seen to transit the disk of its parent star, and we may expect many others to be discovered in due course. These transiting planets will be important to our understanding of planets in general because they allow many kinds of measurements of the physical properties of the planet – measurements that are not possible for less fortuitous orbital alignments. These include, among others, estimates of the density, temperature, and composition of the planetary atmosphere. Moreover, transits provide a means of detecting planets that cannot yet

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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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Schneider, J. "Photometric search for extrasolar planets." Astrophysics and Space Science 241, no. 1 (1996): 35–42. http://dx.doi.org/10.1007/bf00644213.

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Johnson, R. E., and P. J. Huggins. "Toroidal Atmospheres around Extrasolar Planets." Publications of the Astronomical Society of the Pacific 118, no. 846 (2006): 1136–43. http://dx.doi.org/10.1086/506183.

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Brogi, Matteo. "Escaping atmospheres of extrasolar planets." Science 362, no. 6421 (2018): 1360–61. http://dx.doi.org/10.1126/science.aav7010.

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Levrard, B., C. Winisdoerffer, and G. Chabrier. "FALLING TRANSITING EXTRASOLAR GIANT PLANETS." Astrophysical Journal 692, no. 1 (2009): L9—L13. http://dx.doi.org/10.1088/0004-637x/692/1/l9.

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Howard, A. W. "Observed Properties of Extrasolar Planets." Science 340, no. 6132 (2013): 572–76. http://dx.doi.org/10.1126/science.1233545.

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49

Jackson, Brian, Richard Greenberg, and Rory Barnes. "Tidal Heating of Extrasolar Planets." Astrophysical Journal 681, no. 2 (2008): 1631–38. http://dx.doi.org/10.1086/587641.

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Laughlin, G. "A Dance of Extrasolar Planets." Science 330, no. 6000 (2010): 47–48. http://dx.doi.org/10.1126/science.1196505.

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