The formation of close-in planets by the slingshot model

Nagasawa, Makiko; Ida, Shigeru; Bessho, T.

doi:10.1017/s1743921308016700

Cited by 1 publication

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References 14 publications

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“…The distribution of orbital obliquities of exoplanet orbits may offer hints as to the formation mechanism of hot Jupiters. Planet-planet interactions or the Kozai mechanism could bring in giant planets formed beyond the ice line close to the star (Nagasawa et al 2008;Fabrycky and Tremaine 2007). These should change the relative orientation between the spin and orbital axes.…”

Section: Orbital Alignmentsmentioning

confidence: 99%

The Architecture of Exoplanets

Hatzes

2016

Space Sci Rev

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Prior to the discovery of exoplanets our expectations of their architecture were largely driven by the properties of our solar system. We expected giant planets to lie in the outer regions and rocky planets in the inner regions. Planets should probably only occupy orbital distances 0.3-30 AU from the star. Planetary orbits should be circular, prograde and in the same plane. The reality of exoplanets have shattered these expectations. Jupiter-mass, Neptune-mass, Superearths, and even Earth-mass planets can orbit within 0.05 AU of the stars, sometimes with orbital periods of less than one day. Exoplanetary orbits can be eccentric, misaligned, and even in retrograde orbits. Radial velocity surveys gave the first hints that the occurrence rate increases with decreasing mass. This was put on a firm statistical basis with the Kepler mission that clearly demonstrated that there were more Neptuneand Superearth-sized planets than Jupiter-sized planets. These are often in multiple, densely packed systems where the planets all orbit within 0.3 AU of the star, a result also suggested by radial velocity surveys. Exoplanets also exhibit diversity along the main sequence. Massive stars tend to have a higher frequency of planets (≈ 20-25 %) that tend to be more massive (M ≈ 5-10 M Jup ). Giant planets around low mass stars are rare, but these stars show an abundance of small (Neptune and Superearth) planets in multiple systems. Planet formation is also not restricted to single stars as the Kepler mission has discovered several circumbinary planets. Although we have learned much about the architecture of planets over the past 20 years, we know little about the census of small planets at relatively large (a > 1 AU) orbital distances. We have yet to find a planetary system that is analogous to our own solar system. The question of how unique are the properties of our own solar system remains unanswered. Advancements in the detection methods of small planets over a wide range of orbital distances is needed before we gain a complete understanding of the architecture of exoplanetary systems.

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Section: Orbital Alignmentsmentioning

confidence: 99%

The Architecture of Exoplanets

Hatzes

2016

Space Sci Rev

View full text Add to dashboard Cite

show abstract

The formation of close-in planets by the slingshot model

Cited by 1 publication

References 14 publications

The Architecture of Exoplanets

The Architecture of Exoplanets

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