Detecting the Signatures of Uranus and Neptune
arXiv:1104.5014 · doi:10.1016/j.icarus.2011.04.023
Abstract
With more than 15 years since the the first radial velocity discovery of a planet orbiting a Sun-like star, the time baseline for radial velocity surveys is now extending out beyond the orbit of Jupiter analogs. The sensitivity to exoplanet orbital periods beyond that of Saturn orbital radii however is still beyond our reach such that very few clues regarding the prevalence of ice giants orbiting solar analogs are available to us. Here we simulate the radial velocity, transit, and photometric phase amplitude signatures of the solar system giant planets, in particular Uranus and Neptune, and assess their detectability. We scale these results for application to monitoring low-mass stars and compare the relative detection prospects with other potential methods, such as astrometry and imaging. These results quantitatively show how many of the existing techniques are suitable for the detection of ice giants beyond the snow line for late-type stars and the challenges that lie ahead for the detection true Uranus/Neptune analogues around solar-type stars.
20 pages, 4 figures, accepted for publication in Icarus
References in corpus (20)
- Direct Imaging of Multiple Planets Orbiting the Star HR 8799
- Characteristics of planetary candidates observed by Kepler, II: Analysis of the first four months of data
- Images of a fourth planet orbiting HR 8799
- Kepler Input Catalog: Photometric Calibration and Stellar Classification
- Planet formation around stars of various masses: The snow line and the frequency of giant planets
- Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
- A laser frequency comb that enables radial velocity measurements with a precision of 1 cm s
- High-precision wavelength calibration of astronomical spectrographs with laser frequency combs
- Transiting exoplanets from the CoRoT space mission I - CoRoT-Exo-1b: a low-density short-period planet around a G0V star
- Rapid Formation of Gas Giant Planets around M Dwarf Stars
- Self-Consistent Model Atmospheres and the Cooling of the Solar System's Giant Planets
- Constraining Orbital Parameters Through Planetary Transit Monitoring
- The Formation of Ice Giants in a Packed Oligarchy: Instability and Aftermath
- Selection Functions in Doppler Planet Searches
- The Jupiter Twin HD 154345b
- Forming Jupiter, Saturn, Uranus and Neptune in Few Million Years by Core Accretion
- Giant Planet Formation by Disk Instability in Low Mass Disks?
- On the Inclination Dependence of Exoplanet Phase Signatures
- Simulations for Multi-Object Spectrograph Planet Surveys
- Observational Window Functions in Planet Transit Surveys
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- The Fundamental Connections Between the Solar System and Exoplanetary Science
- The Transit Transmission Spectrum of a Cold Gas Giant Planet
- Distinguishing Between Stellar and Planetary Companions With Phase Monitoring
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- An ice giant exoplanet interpretation of the anomaly in microlensing event OGLE-2011-BLG-0173
- Stellar Parameters for HD 69830, a Nearby Star with Three Neptune Mass Planets and an Asteroid Belt
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