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Journal articles on the topic 'Extrasolar planets'

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Published: 4 June 2021
Last updated: 1 August 2024

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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 (October 17, 2000): 12405–6. http://dx.doi.org/10.1073/pnas.210381997.

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2

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

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3

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

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4

Cochran, William. "Extrasolar planets." Physics World 10, no. 7 (July 1997): 31–36. http://dx.doi.org/10.1088/2058-7058/10/7/30.

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5

Cameron, Andrew Collier. "Extrasolar planets." Physics World 14, no. 1 (January 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 (November 11, 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 (September 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 (April 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 (June 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, William B. Hubbard, Philip A. Ianna, Martin Kürster, Jack J. Lissauer, et al. "COMMISSION 53: EXTRASOLAR PLANETS." Proceedings of the International Astronomical Union 4, T27A (December 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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11

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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12

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–mass planets remain undetectable, but space–based missions such as Kepler, COROT and SIM may provide detections of terrestrial planets within the next decade.The number of planets increases with decreasing planet mass, indicating that nature makes more small planets than jupiter–mass planets. Extrapolation, though speculative, bodes well for an even larger number of earth–mass planets. These observations and the theory of planet formation suggests that single sun–like stars commonly harbor earth–sized rocky planets, as yet undetectable. The number of planets increases with increasing orbital distance from the host star, and most known planets reside in non–circular orbits. Many known planets reside in the habitable zone (albeit being gas giants) and most newly discovered planets orbit beyond 1 AU from their star. A population of Jupiter–like planets may reside at 5–10 AU from stars, not easily detectable at present. The sunlike star 55 Cancri harbors a planet of 4–10 Jupiter masses orbiting at 5.5 AU in a low eccentricity orbit, the first analog of our Jupiter, albeit with two large planets orbiting inward.To date, 10 multiple–planet systems have been discovered, with four revealing gravitational interactions between the planets in the form of resonances. GJ 876 has two planets with periods of 1 and 2 months. Other planetary systems are “hierarchical”, consisting of widely separated orbits. These two system architectures probably result from gravitational interactions among the planets and between the planets and the proto-planetary disk out of which they formed.
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13

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 (August 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 those that are essentially “Earth-like”, containing metallic Fe and Mg-silicates, to those that are dominated by graphite and SiC. This implies that a diverse range of terrestrial planets are likely to exist within extrasolar planetary systems.
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14

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 a few AU of these stars. Less than 1% of G and K main sequence stars harbor brown dwarf companions with masses between 5 and 70 MJup. Including Gliese 876b, 8 companions exhibit m sin i < 5 MJup which constitute the best planet candidates to date. Apparently, 4% of stars have planetary companions within the range m sin i = 0.5 to 5 MJup. Planets are distinguished from brown dwarfs by the discontinuous jump in the mass function at 5 MJup. About 2/3 of the planets orbit within just 0.3 AU due in part to their favorable detectability, but also possibly due to a real “pile up” of planets near the star. Inward orbital migration after formation may explain this, but the mechanism to stop the migration remains unclear. Five of eight planets have orbital eccentricities greater than that of our Jupiter, eJup = 0.048, and tidal circularization may explain most of the circular orbits. Thus, eccentric orbits are common and may arise from gravitational interactions with other planets, stars, or the protoplanetary disk. The planet-bearing stars are systematically metal-rich, as is the Sun, compared to the solar neighborhood.
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15

Skinner, J. W., and J. Y.-K. Cho. "Modons on tidally synchronized extrasolar planets." Monthly Notices of the Royal Astronomical Society 511, no. 3 (January 29, 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 modons transport and mix planetary-scale patches of hot and cold air around the planet, leading to high-amplitude and quasi-periodic signatures in the disc-averaged temperature flux. Hence, they induce variations of the ‘hotspot’ longitude to either side of the planet’s substellar point – consistent with observations at different epochs. The variability behaviour in our simulations broadly underscores the importance of accurately capturing vortex dynamics in extrasolar planet atmosphere modelling, particularly in understanding current observations.
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16

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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17

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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18

Butler, R. Paul, Geoffrey W. Marcy, Debra A. Fischer, Steven S. Vogt, C. G. Tinney, Hugh R. A. Jones, Alan J. Penny, and Kevin Apps. "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 0.1 AU, distinguishing planets from binary stars. The planet bearing stars are metal–rich relative to both nearby stars and to the Sun. Analogs of Solar System planets have not been detected to date as they require precision of 3 m s−1 maintained for more than a decade.
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19

Marcy, Geoffrey W., R. Paul Butler, Steven S. Vogt, Debra A. Fischer, Gregory W. Henry, Greg Laughlin, Jason T. Wright, and John A. Johnson. "Five New Extrasolar Planets." Astrophysical Journal 619, no. 1 (January 20, 2005): 570–84. http://dx.doi.org/10.1086/426384.

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20

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

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21

Gonzalez, G. "Extrasolar planets and ETI." Astronomy & Geophysics 39, no. 6 (December 1, 1998): 6.8. http://dx.doi.org/10.1093/astrog/39.6.6.8.

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22

Boss, Alan, Alain Lecavelier des Etangs, Michel Mayor, Peter Bodenheimer, Andrew Collier-Cameron, Eiichiro Kokubo, Rosemary Mardling, Dante Minniti, and Didier Queloz. "COMMISSION 53: EXTRASOLAR PLANETS." Proceedings of the International Astronomical Union 7, T28A (December 2011): 138–40. http://dx.doi.org/10.1017/s1743921312002712.

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23

Bowler, Brendan P. "Imaging Extrasolar Giant Planets." Publications of the Astronomical Society of the Pacific 128, no. 968 (August 29, 2016): 102001. http://dx.doi.org/10.1088/1538-3873/128/968/102001.

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24

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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25

Santos, N. C. "Extrasolar Planets: Constraints for Planet Formation Models." Science 310, no. 5746 (October 14, 2005): 251–55. http://dx.doi.org/10.1126/science.1100210.

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26

Deeg, Hans J., Keith Horne, Fabio Favata, C. Aerts, E. Antonello, M. Badiali, C. Catala, 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. Implications of Eddington for future larger scale missions are briefly discussed.
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27

Mishra, Ruchi, Miljenko Čemeljić, Jacobo Varela, and Maurizio Falanga. "Auroras on Planets around Pulsars." Astrophysical Journal Letters 959, no. 1 (December 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 parameters for such a detection, which would be the first radio detection of an extrasolar planet. In addition to probing the atmosphere of planets in such extreme conditions, of great interest is also the prospect of the first direct probe into the pulsar wind.
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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 (May 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 prevented by an external perturbation. Here we constrain the tidalQfactor for transiting extrasolar planets by comparing their circularization times with accurately determined stellar ages. Using estimated secular perturbation timescales, we also provide constraints on the properties of hypothetical second planets exterior to the known eccentric close-in planets.
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29

Kalas, Paul. "Direct imaging of massive extrasolar planets." Proceedings of the International Astronomical Union 6, S276 (October 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 currently imaged exoplanets, provides an update on the orbit of Fomalhaut b, and highlights the emerging phenomenon of circumplanetary disks.
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30

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 (September 23, 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, likely to be central for characterization, are discussed. Theoretical issues that need to be addressed in the near future are also highlighted.
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31

Dvorak, Rudolf, Li-Yong Zhou, and Helmut Baudisch. "Trojans in Exosystems with Two Massive Planets." Proceedings of the International Astronomical Union 8, S293 (August 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 with the aid of numerical integration. It turned out that in many configurations – depending on the mass ratios μ and the semi-major axes ratio ν – giant planets may host Trojans.
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32

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." Proceedings of the International Astronomical Union 1, T26A (December 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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33

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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34

Mao, Shude, Eamonn Kerins, and Nicholas J. Rattenbury. "Extrasolar planet detections with gravitational microlensing." Proceedings of the International Astronomical Union 3, S249 (October 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 (usually with high magnification) in order to identify anomalies caused by planets. So far four extrasolar planets have been discovered using the microlensing technique, with half a dozen new planet candidates identified in 2007 (yet to be published). Future possibilities include a network of wide-field 2m-class telescopes from the ground (which can combine survey and follow-up in the same setup) and a 1m-class survey telescope from space.
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35

Padovan, S., T. Spohn, P. Baumeister, N. Tosi, D. Breuer, Sz Csizmadia, H. Hellard, and F. Sohl. "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, which is routinely calculated from interior structure codes.Methods.We used the matrix-propagator technique, a method frequently used in the geophysical community.Results.We detail the calculation and apply it to the case of GJ 436b, a classical example of the degeneracy of mass-radius relationships, to illustrate how measurements ofk2can improve our understanding of the interior structure of extrasolar planets. We implemented the method in a code that is fast, freely available, and easy to combine with preexisting interior structure codes. While the linear approach presented here for the calculation of the Love numbers cannot treat the presence of nonlinear effects that may arise under certain dynamical conditions, it is applicable to close-in gaseous extrasolar planets like hot Jupiters, likely the first targets for whichk2will be measured.
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36

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 114762, 70 Vir, and τ Boo. Our limits are just above those predicted for the planetary emissions. We discuss the possibilities for more stringent limits and the implications that the existing observations have for the planets' radio emissions, and hence on the planetary magnetic fields and stellar wind environments.
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37

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 (October 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 theory. The introduction of type-I migration inhibits in situ formation of gas giants in habitable zones (HZs) and reduces the probability of passage of gas giants through HZs, both of which facilitate retention of terrestrial planets in HZs. We also point out that the effect of magneto-rotational instability (MRI) could lead to trapping of migrating protoplanetary embryos in the regions near an ice line in the disk and it significantly enhances formation/retention probability of gas giants against type-I migration.
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38

Moses, Julianne I. "Chemical kinetics on extrasolar planets." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 372, no. 2014 (April 28, 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 quenching. I review these disequilibrium processes in detail, discuss observational consequences and examine some of the current evidence for kinetic processes on extrasolar planets.
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39

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

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40

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

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41

Brogi, Matteo. "Escaping atmospheres of extrasolar planets." Science 362, no. 6421 (December 20, 2018): 1360–61. http://dx.doi.org/10.1126/science.aav7010.

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42

Levrard, B., C. Winisdoerffer, and G. Chabrier. "FALLING TRANSITING EXTRASOLAR GIANT PLANETS." Astrophysical Journal 692, no. 1 (January 21, 2009): L9—L13. http://dx.doi.org/10.1088/0004-637x/692/1/l9.

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43

Howard, A. W. "Observed Properties of Extrasolar Planets." Science 340, no. 6132 (May 2, 2013): 572–76. http://dx.doi.org/10.1126/science.1233545.

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44

Jackson, Brian, Richard Greenberg, and Rory Barnes. "Tidal Heating of Extrasolar Planets." Astrophysical Journal 681, no. 2 (July 10, 2008): 1631–38. http://dx.doi.org/10.1086/587641.

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45

Laughlin, G. "A Dance of Extrasolar Planets." Science 330, no. 6000 (September 30, 2010): 47–48. http://dx.doi.org/10.1126/science.1196505.

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46

Marcy, Geoffrey W., and R. Paul Butler. "DETECTION OF EXTRASOLAR GIANT PLANETS." Annual Review of Astronomy and Astrophysics 36, no. 1 (September 1998): 57–97. http://dx.doi.org/10.1146/annurev.astro.36.1.57.

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47

Kaltenegger, L., W. G. Henning, and D. D. Sasselov. "DETECTING VOLCANISM ON EXTRASOLAR PLANETS." Astronomical Journal 140, no. 5 (October 14, 2010): 1370–80. http://dx.doi.org/10.1088/0004-6256/140/5/1370.

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48

Hughes, David W. "Wobbly pursuit of extrasolar planets." Nature 391, no. 6668 (February 1998): 651–52. http://dx.doi.org/10.1038/35539.

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49

George, Samuel J. "Extrasolar planets in the classroom." Physics Education 46, no. 4 (June 29, 2011): 403–6. http://dx.doi.org/10.1088/0031-9120/46/4/004.

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50

Schewe, Phil F. "Direct imaging of extrasolar planets." Physics Today 56, no. 12 (December 2003): 9. http://dx.doi.org/10.1063/1.4796958.

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