Extrasolar Planets: Constraints for Planet Formation Models

Santos, N. C.; Benz, W.; Mayor, M.

doi:10.1126/science.1100210

Cited by 42 publications

(39 citation statements)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Thus, either the planetary migration is more pronounced for high [Fe/H] (which is in agreement with simulations; e.g., see Livio & Pringle 2003) or giant planets of this cluster may form close to stars ( 1 AU ) in high-metallicity environments. We recall that for ½Fe/ H > 0, the most accredited formation theory is core accretion ( Fischer & Valenti 2005;Santos et al 2005). Note also that the distribution of the MPS planets in the a-[ Fe/H] plane is somehow opposite to the overall observed trend: without them the correlation would be even more pronounced.…”

Section: Cluster C2mentioning

confidence: 81%

See 1 more Smart Citation

Extrasolar Planet Taxonomy: A New Statistical Approach

Marchi

2007

ApJ

View full text Add to dashboard Cite

In this paper we present the guidelines for an extrasolar planet taxonomy. The discovery of an increasing number of extrasolar planets showing a vast variety of planetary parameters, such as Keplerian orbital elements, and environmental parameters, such as stellar masses, spectral types, and metallicity, prompts the development of a planetary taxonomy. In this work, via principal component analysis followed by hierarchical clustering analysis, we report the definition of five robust groups of planets. We also discuss the physical relevance of such analysis, which may provide a valid basis for disentangling the role of the several physical parameters involved in the processes of planet formation and subsequent evolution. For instance, we were able to divide the hot Jupiters into two main groups on the basis of their stellar masses and metallicities. Moreover, for some groups, we find strong correlations among metallicity, semimajor axis, and eccentricity. The implications of these findings are discussed.

show abstract

Section: Cluster C2mentioning

confidence: 81%

“…We found significant correlation (see also below) between M p -e, a-e, and M p -a. However, overall correlations have been widely analyzed elsewhere and are not discussed here (e.g., Santos et al 2005 and references therein).…”

Section: Multivariate Analysis and Dimensional Scaling Of Epsmentioning

confidence: 99%

Extrasolar Planet Taxonomy: A New Statistical Approach

Marchi

2007

ApJ

View full text Add to dashboard Cite

show abstract

“…The parent stars of exo-planets have higher metallicity [Santos 2005]. They have a higher abundance of elements heavier than hydrogen and helium.…”

Section: Conditions Conducive To Exo-planet Growthmentioning

confidence: 99%

“…Planet bearing Extra Solar Systems invariably have an environment rich in metal [Santos 2005]. The stars with twice the metallicity have 25% chance of harbouring a planet whereas stars with Sun's metallicity has only 5% chance.…”

Section: Evolution Of Solar System Building Materialsmentioning

confidence: 99%

Enigma of the Birth and Evolution of Solar Systems May Be Solved by Invoking Planetary-Satellite Dynamics

Sharma¹

2012

Space Science

View full text Add to dashboard Cite

“…Interactions between an embedded planet and a gaseous disk (Goldreich 1980) ; Further Astronomers and Astrophysicists have identified two migration modes (Santos 2005, Lin et al 1986, Ward 1997 Chondrule formation continued up to 3My from the beginning. In first 4.2±1.3My , the large sized asteroids of size bigger than 500Km are formed.…”

Section: The Discovery Of First Extra-solar System(lissauer 2002)mentioning

confidence: 99%

The Architectural Design Rules of Solar Systems Based on the New Perspective

Sharma

2010

Earth Moon Planets

View full text Add to dashboard Cite

In this paper I present a new perspective of the birth and evolution of Planetary Systems. This new perspective presents an all encompassing and self consistent Paradigm of the birth and evolution of the solar systems. In doing so it redefines astronomy and rewrites astronomical principles. Kepler and Newton defined a stable and non-evolving elliptical orbits. While this perspective defines a collapsing or expanding spiral orbit of planets except for Brown Dwarfs. Brown Dwarfs are significant fraction of the central star. Hence they rapidly evolve from non-Keplerian state to the end point which is a Keplerian state where it is in stable elliptical orbits. On the basis of the Lunar Laser Ranging Data released by NASA on the Silver Jubilee Celebration of Man's Landing on Moon on 21st July 1969-1994, theoretical formulation of Earth-Moon tidal interaction was carried out and Planetary Satellite Dynamics was established. It was found that this mathematical analysis could as well be applied to Star and Planets system and since every star could potentially contain an extra-solar system, hence we have a large ensemble of exoplanets to test our new perspective on the birth and evolution of solar systems. Till date 403 exoplanets have been discovered in 390 extra-solar systems by radial velocity method, by transiting planet method, by gravitational lensing method, by direct imaging method and by timing method. I have taken 12 single planet systems , 4 Brown Dwarf -Star systems and 2 Brown Dwarf pairs. Following architectural design rules are corroborated through this study of exoplanets. All planets are born at inner Clarke's Orbit what we refer to as inner geo-synchronous orbit in case of Earth-Moon System. The inner Clarke's Orbit is an orbit of unstable equilibrium. By any perturbative force such as cosmic particles or radiation pressure, the planet gets tipped long of aG1 or short of aG1. Here aG1 is inner Clarke's Orbit. If planet is long of aG1 then it is said to be in extra-synchronous orbit. Here Gravitational Sling Shot effect is in play. In gravity assist planet fly-by maneuver in space flights, gravitational sling shot is routinely used to boost the space craft to its destination. The exoplanet can either be launched on death spiral as CLOSE HOT JUPITERS or can be launched on an expanding spiral path as the planets in our Solar System are. In death spiral, exoplanet less than 5 mJ will get pulverized and vaporized in close proximity to the host star. If the mass is between 5 mJ and 7.5 mJ then it will be partially vaporized and partially engulfed by the host star and if it is greater than 7.5 mJ , then it will be completely ingested by the host star. In the process the planet will deposit all its material and angular momentum in the Host Star. This will leave tell-tale imprints of ingestion: in such cases host Star will have higher 7Li, host star will become a rapidly rotating progenitor and the host star will have excess IR. All these have been confirmed by observations of Transiting Planets. It was...

show abstract

Extrasolar Planets: Constraints for Planet Formation Models

Cited by 42 publications

References 62 publications

Extrasolar Planet Taxonomy: A New Statistical Approach

Extrasolar Planet Taxonomy: A New Statistical Approach

Enigma of the Birth and Evolution of Solar Systems May Be Solved by Invoking Planetary-Satellite Dynamics

The Architectural Design Rules of Solar Systems Based on the New Perspective

Contact Info

Product

Resources

About