The Solar System as an Exoplanetary System

Martin, Rebecca G.; Livio, Mario

doi:10.1088/0004-637x/810/2/105

Cited by 54 publications

(35 citation statements)

References 94 publications

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“…Recently, Santos et al [193] using the SWEET-Cat database also addressed the question whether very massive Jupiters tend to form at metallicities lower than their less massive counterparts. The authors found a convincing observational evidence that giant planets with masses above and below ∼4 M constitute two distinct populations 24 . They showed that the hosts of giant planets with masses < 4 M have metallicities on average higher than that of the fields stars without planets.…”

Section: Very Massive Giants and Metallicitymentioning

confidence: 96%

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Adibekyan

2019

Geosciences

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Discovery of only handful of exoplanets required to establish a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: What is the origin of that relation? what is the exact functional form of the giant planet -metallicity relation (in the metal-poor regime)?, does such a relation exist for terrestrial planets? All these question are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet -metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study lead to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: i) The hosts of sub-Jupiter mass planets (∼0.6 -0.9 M ) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be related to the longer disk lifetime and higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets. ii) Contrary to the previous claims, our data and results do not support the existence of a breakpoint planetary mass at 4 M above and below which planet formation channels are different. However, the results also suggest that planets of the same (high) mass can be formed through different channels depending on the (disk) stellar mass i.e. environmental conditions.

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Section: Very Massive Giants and Metallicitymentioning

confidence: 96%

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Adibekyan

2019

Geosciences

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“…The only clear difference is in the period of the innermost planet where the solar system is an outlier. While the lack of superearths/mini-Neptunes in the solar system is also notable (Martin & Livio 2015), earth-sized planets are not intrinsically rare, and the size of the terrestrial planets does not make the solar system an outlier in the exoplanet distribution.…”

Section: How Rare Is the Solar System?mentioning

confidence: 99%

The Exoplanet Population Observation Simulator. I. The Inner Edges of Planetary Systems

et al. 2018

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The Kepler survey provides a statistical census of planetary systems out to the habitable zone. Because most planets are non-transiting, orbital architectures are best estimated using simulated observations of ensemble populations. Here, we introduce EPOS, the Exoplanet Population Observation Simulator, to estimate the prevalence and orbital architectures of multi-planet systems based on the latest Kepler data release, DR25. We estimate that at least 42% of sun-like stars have nearly coplanar planetary systems with 7 or more exoplanets. The fraction of stars with at least one planet within 1 au could be as high as 100% depending on assumptions about the distribution of single transiting planets. We estimate an occurrence rate of planets in the habitable zone around sun-like stars of η ⊕ = 36 ± 14%. The innermost planets in multi-planet systems are clustered around an orbital period of 10 days (0.1 au), reminiscent of the protoplanetary disk inner edge or could be explained by a planet trap at that location. Only a small fraction of planetary systems have the innermost planet at long orbital periods, with fewer than ≈ 8% and ≈ 3% having no planet interior to the orbit of Mercury and Venus, respectively. These results reinforce the view that the solar system is not a typical planetary system, but an outlier among the distribution of known exoplanetary systems. We predict that at least half of the habitable zone exoplanets are accompanied by (non-transiting) planets at shorter orbital periods, hence knowledge of a close-in exoplanet could be used as a way to optimize the search for Earth-size planets in the Habitable Zone with future direct imaging missions.

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“…The vast majority of observed super-Earths are close to their parent star, although this is most likely a selection effect (Chiang & Laughlin 2013). In a recent work, Martin & Livio (2015) have shown that perhaps the main characteristic that distinguishes the solar system from the observed exoplanetary systems is the absence of super-Earths. Consequently, it is very interesting to examine the effects that the presence of a super-Earth would have had on asteroid impacts on Earth.…”

Section: Introductionmentioning

confidence: 99%

Asteroid impacts on terrestrial planets: the effects of super-Earths and the role of the ν6 resonance

Smallwood

Martin

Lepp

et al. 2017

Monthly Notices of the Royal Astronomical Society

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With N-body simulations of a planetary system with an asteroid belt we investigate how the asteroid impact rate on the Earth is affected by the architecture of the planetary system. We find that the ν 6 secular resonance plays an important role in the asteroid collision rate with the Earth. Compared to exoplanetary systems, the solar system is somewhat special in its lack of a super-Earth mass planet in the inner solar system. We therefore first consider the effects of the presence of a super-Earth in the terrestrial planet region. We find a significant effect for super-Earths with a mass of around 10 M ⊕ and a separation greater than about 0.7 AU. For a super-Earth that is interior to the Earth's orbit, the number of asteroids colliding with Earth increases the closer the super-Earth is to the Earth's orbit. This is the result of multiple secular resonance locations causing more asteroids to be perturbed onto Earth-crossing orbits. When the super-Earth is placed exterior to Earth's orbit, the collision rate decreases substantially because the ν 6 resonance no longer exists in the asteroid belt region. We also find that changing the semi-major axis of Saturn leads to a significant decrease in the asteroid collision rate, while increasing its mass increases the collision rate. These results may have implications for the habitability of exoplanetary systems.

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The Solar System as an Exoplanetary System

Cited by 54 publications

References 94 publications

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

The Exoplanet Population Observation Simulator. I. The Inner Edges of Planetary Systems

Asteroid impacts on terrestrial planets: the effects of super-Earths and the role of the ν6 resonance

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