Absence of a metallicity effect for ultra-short-period planets

@article{Winn2017AbsenceOA,
  title={Absence of a metallicity effect for ultra-short-period planets},
  author={Joshua N. Winn and Roberto Sanchis-Ojeda and Leslie A. Rogers and Erik A. Petigura and Andrew W. Howard and Howard T. Isaacson and Geoffrey W. Marcy and Kevin C. Schlaufman and Phillip A. Cargile and Leslie Hebb},
  journal={arXiv: Earth and Planetary Astrophysics},
  year={2017}
}
Ultra-short-period (USP) planets are a newly recognized class of planets with periods shorter than one day and radii smaller than about 2 Earth radii. It has been proposed that USP planets are the solid cores of hot Jupiters that lost their gaseous envelopes due to photo-evaporation or Roche lobe overflow. We test this hypothesis by asking whether USP planets are associated with metal-rich stars, as has long been observed for hot Jupiters. We find the metallicity distributions of USP-planet and… Expand

Figures and Tables from this paper

Radius and Mass Distribution of Ultra-short-period Planets
Ultra-short-period (USP) planets are an enigmatic subset of exoplanets defined by having orbital periods <1 day. It is still not understood how USP planets form, or to what degree they differ fromExpand
Ultra-short-period Planets from Secular Chaos
Over a hundred rocky planets orbiting Sun-like stars in very short orbital periods (<1 day) have been discovered by the Kepler mission. These planets, known as ultra-short-period (USP) planets, areExpand
An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141
Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation beingExpand
Low-eccentricity migration of ultra-short-period planets in multiplanet systems
  • Bonan Pu, D. Lai
  • Physics
  • Monthly Notices of the Royal Astronomical Society
  • 2019
Recent studies suggest that ultra-short-period planets (USPs), Earth-sized planets with sub-day periods, constitute a statistically distinct sub-sample of Kepler planets: USPs have smaller radiiExpand
An ultra-short period rocky super-Earth orbiting the G2-star HD 80653
Ultra-short period (USP) planets are a class of exoplanets with periods shorter than one day. The origin of this sub-population of planets is still unclear, with different formation scenarios highlyExpand
Metallicity-dependent signatures in the Kepler planets
Using data from the California-Kepler-Survey (CKS) we study trends in planetary properties with host star metallicity for close-in planets. By incorporating knowledge of the properties of theExpand
Kepler-78 and the Ultra-Short-Period planets
Compared to the Earth, the exoplanet Kepler-78b has a similar size (1.2 $R_\oplus$) and an orbital period a thousand times shorter (8.5 hours). It is currently the smallest planet for which the mass,Expand
The Recent Research Progress of Exoplanets of Ultra-Short Periods
Abstract Ultra-short-period planets (USPs) with orbital periods of less than 1 day are emerging as a new scientific goal in the field of exoplanets. Search and identification of USPs requireExpand
Homogeneous Analysis of Hot Earths: Masses, Sizes, and Compositions
Terrestrial planets have been found orbiting Sun-like stars with extremely short periods --- some as short as 4 hours. These "ultra-short-period planets" or "hot Earths" are so strongly irradiatedExpand
Do Metal-rich Stars Make Metal-rich Planets? New Insights on Giant Planet Formation from Host Star Abundances
The relationship between the compositions of giant planets and their host stars is of fundamental interest in understanding planet formation. The solar system giant planets are enhanced above solarExpand
...
1
2
3
4
...

References

SHOWING 1-10 OF 59 REFERENCES
The Metallicities of Stars With and Without Transiting Planets
Host star metallicities have been used to infer observational constraints on planet formation throughout the history of the exoplanet field. The giant planet metallicity correlation has now beenExpand
The Planet-Metallicity Correlation
We have recently carried out spectral synthesis modeling to determine Teff, log g, v sin i, and [Fe/H] for 1040 FGK-type stars on the Keck, Lick, and Anglo-Australian Telescope planet searchExpand
A SURVEY FOR VERY SHORT-PERIOD PLANETS IN THE KEPLER DATA
We conducted a search for very short-period transiting objects in the publicly available Kepler data set. Our preliminary survey has revealed four planetary candidates, all with orbital periods lessExpand
A Super-Solar Metallicity For Stars With Hot Rocky Exoplanets
The host star metallicity provide a measure of the conditions in protoplanetary disks at the time of planet formation. Using a sample of over 20,000 Kepler stars with spectroscopic metallicities fromExpand
An abundance of small exoplanets around stars with a wide range of metallicities
TLDR
Spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission are reported, finding that planets with radii less than four Earth radii form around host stars with a wide range of metallicities (but on average a metallicity close to that of the Sun), whereas large planets preferentially form around stars with higher metallicities. Expand
A Continuum of Planet Formation Between 1 and 4 Earth Radii
It has long been known that stars with high metallicity are more likely to host giant planets than stars with low metallicity. Yet the connection between host star metallicity and the properties ofExpand
MOST 1.6 EARTH-RADIUS PLANETS ARE NOT ROCKY
The Kepler mission, combined with ground-based radial velocity (RV) follow-up and dynamical analyses of transit timing variations, has revolutionized the observational constraints onExpand
TESTING THE METAL OF LATE-TYPE KEPLER PLANET HOSTS WITH IRON-CLAD METHODS
It has been shown that F, G, and early K dwarf hosts of Neptune-sized planets are not preferentially metal-rich. However, it is less clear whether the same holds for late K and M dwarf planet hosts.Expand
Magnetospheric Truncation, Tidal Inspiral, and the Creation of Short-period and Ultra-short-period Planets
Sub-Neptunes around FGKM dwarfs are evenly distributed in log orbital period down to $\sim$10 days, but dwindle in number at shorter periods. Both the break at $\sim$10 days and the slope of theExpand
Three regimes of extrasolar planet radius inferred from host star metallicities
TLDR
The metallicities (that is, the abundances of elements heavier than hydrogen and helium) of more than 400 stars hosting 600 exoplanet candidates are reported, and it is found that the exoplanets can be categorized into three populations defined by statistically distinct metallicity regions. Expand
...
1
2
3
4
5
...