Log in

Relevant bibliographies by topics / Giant gaseous planets

Contents

Journal articles

Academic literature on the topic 'Giant gaseous planets'

Author: Grafiati

Published: 20 April 2024

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Consult the lists of relevant articles, books, theses, conference reports, and other scholarly sources on the topic 'Giant gaseous planets.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Journal articles on the topic "Giant gaseous planets"

1

Veras, Dimitri, and Jim Fuller. "Tidal circularization of gaseous planets orbiting white dwarfs." Monthly Notices of the Royal Astronomical Society 489, no. 2 (2019): 2941–53. http://dx.doi.org/10.1093/mnras/stz2339.

Full text

Abstract:

ABSTRACT A gas giant planet which survives the giant branch stages of evolution at a distance of many au and then is subsequently perturbed sufficiently close to a white dwarf will experience orbital shrinkage and circularization due to star–planet tides. The circularization time-scale, when combined with a known white dwarf cooling age, can place coupled constraints on the scattering epoch as well as the active tidal mechanisms. Here, we explore this coupling across the entire plausible parameter phase space by computing orbit shrinkage and potential self-disruption due to chaotic f-mode exci

APA, Harvard, Vancouver, ISO, and other styles

2

Boss, Alan P. "Metallicity and Planet Formation: Models." Proceedings of the International Astronomical Union 5, S265 (2009): 391–98. http://dx.doi.org/10.1017/s1743921310001067.

Full text

Abstract:

AbstractPlanets typically are considerably more metal-rich than even the most metal-rich stars, one indication that planet formation must differ greatly from star formation. There is general agreement that terrestrial planets form by the collisional accumulation of solids composed of heavy elements in the inner regions of protoplanetary disks. Two competing mechanisms exist for the formation of giant planets, core accretion and disk instability, though hybrid combinations are possible as well. In core accretion, a higher metallicity in the protoplanetary disk leads directly to larger core mass

APA, Harvard, Vancouver, ISO, and other styles

3

Guenel, M., S. Mathis, and F. Remus. "Unravelling tidal dissipation in gaseous giant planets." Astronomy & Astrophysics 566 (June 2014): L9. http://dx.doi.org/10.1051/0004-6361/201424010.

Full text

APA, Harvard, Vancouver, ISO, and other styles

4

Carleo, Ilaria, Paolo Giacobbe, Gloria Guilluy, et al. "The GAPS Programme at TNG XXXIX. Multiple Molecular Species in the Atmosphere of the Warm Giant Planet WASP-80 b Unveiled at High Resolution with GIANO-B ^∗." Astronomical Journal 164, no. 3 (2022): 101. http://dx.doi.org/10.3847/1538-3881/ac80bf.

Full text

Abstract:

Abstract Detections of molecules in the atmosphere of gas giant exoplanets allow us to investigate the physico-chemical properties of the atmospheres. Their inferred chemical composition is used as tracer of planet formation and evolution mechanisms. Currently, an increasing number of detections is showing a possible rich chemistry of the hotter gaseous planets, but whether this extends to cooler giants is still unknown. We observed four transits of WASP-80 b, a warm transiting giant planet orbiting a late-K dwarf star with the near-infrared GIANO-B spectrograph installed at the Telescopio Naz

APA, Harvard, Vancouver, ISO, and other styles

5

Raymond, Sean N. "Terrestrial planet formation in extra-solar planetary systems." Proceedings of the International Astronomical Union 3, S249 (2007): 233–50. http://dx.doi.org/10.1017/s1743921308016645.

Full text

Abstract:

AbstractTerrestrial planets form in a series of dynamical steps from the solid component of circumstellar disks. First, km-sized planetesimals form likely via a combination of sticky collisions, turbulent concentration of solids, and gravitational collapse from micron-sized dust grains in the thin disk midplane. Second, planetesimals coalesce to form Moon- to Mars-sized protoplanets, also called “planetary embryos”. Finally, full-sized terrestrial planets accrete from protoplanets and planetesimals. This final stage of accretion lasts about 10-100 Myr and is strongly affected by gravitational

APA, Harvard, Vancouver, ISO, and other styles

6

Boss, Alan P. "Modes of Gaseous Planet Formation." Symposium - International Astronomical Union 202 (2004): 141–48. http://dx.doi.org/10.1017/s0074180900217725.

Full text

Abstract:

The discovery of gas giant planets around nearby stars has launched a new era in our understanding of the formation and evolution of planetary systems. However, none of the over four dozen companions detected to date strongly resembles Jupiter or Saturn: their inferred masses range from sub-Saturn-mass to 10 Jupiter-masses or more, while their orbits extend from periods of a few days to a few years. Given this situation, it seems prudent to re-examine mechanisms for gas giant planet formation. The two extreme cases are top-down or bottom-up. The latter is the core accretion mechanism, long fav

APA, Harvard, Vancouver, ISO, and other styles

7

Mayor, M., D. Naef, F. Pepe, et al. "HD 83443: a system with two Saturns." Symposium - International Astronomical Union 202 (2004): 84–86. http://dx.doi.org/10.1017/s0074180900217543.

Full text

Abstract:

We report the discovery of an extrasolar planetary system with two Saturnian planets around the star HD 83443. The new planetary system is unusual by more than one aspect, as it contains two very low–mass gaseous giant planets, both on very tight orbits. Among the planets detected so far, the inner planet has the smallest semi–major axis (0.038 AU) and period (2.985 days) whereas the outer planet is the lightest one with m2 sin i = 0.53 MSat. A preliminary dynamical study confirms the stability of the system.

APA, Harvard, Vancouver, ISO, and other styles

8

Masset, Frédéric S. "Planetary migration in gaseous protoplanetary disks." Proceedings of the International Astronomical Union 3, S249 (2007): 331–46. http://dx.doi.org/10.1017/s1743921308016797.

Full text

Abstract:

AbstractTides come from the fact that different parts of a system do not fall in exactly the same way in a non-uniform gravity field. In the case of a protoplanetary disk perturbed by an orbiting, prograde protoplanet, the protoplanet tides raise a wake in the disk which causes the orbital elements of the planet to change over time. The most spectacular result of this process is a change in the protoplanet's semi-major axis, which can decrease by orders of magnitude on timescales shorter than the disk lifetime. This drift in the semi-major axis is called planetary migration. In a first part, w

APA, Harvard, Vancouver, ISO, and other styles

9

Bitsch, Bertram, Andre Izidoro, Anders Johansen, et al. "Formation of planetary systems by pebble accretion and migration: growth of gas giants." Astronomy & Astrophysics 623 (March 2019): A88. http://dx.doi.org/10.1051/0004-6361/201834489.

Full text

Abstract:

Giant planets migrate though the protoplanetary disc as they grow their solid core and attract their gaseous envelope. Previously, we have studied the growth and migration of an isolated planet in an evolving disc. Here, we generalise such models to include the mutual gravitational interaction between a high number of growing planetary bodies. We have investigated how the formation of planetary systems depends on the radial flux of pebbles through the protoplanetary disc and on the planet migration rate. Our N-body simulations confirm previous findings that Jupiter-like planets in orbits outsi

APA, Harvard, Vancouver, ISO, and other styles

10

Hansen, Bradley M. S. "Formation of exoplanetary satellites by pull-down capture." Science Advances 5, no. 10 (2019): eaaw8665. http://dx.doi.org/10.1126/sciadv.aaw8665.

Full text

Abstract:

The large size and wide orbit of the recently announced exomoon candidate Kepler-1625b-i are hard to explain within traditional theories of satellite formation. We show that these properties can be reproduced if the satellite began as a circumstellar co-orbital body with the original core of the giant planet Kepler-1625b. This body was then drawn down into a circumplanetary orbit during the rapid accretion of the giant planet gaseous envelope, a process termed “pull-down capture.” Our numerical integrations demonstrate the stability of the original configuration and the capture process. In thi

APA, Harvard, Vancouver, ISO, and other styles

More sources

We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!