The case of Ross 176 is a late K-type star that hosts a promising water-world candidate planet. The star has a radius of R∗=0.569±0.020R⊙ and a mass of M⋆ = […]
In new research, University of California, Irvine astronomers describe how more than 200 known exoplanets are likely much larger than previously thought. It’s a finding that could change which distant […]
Only 40 exoplanetary systems with five or more planets are currently known. These systems are crucial for our understanding of planet formation and planet-planet interaction.
The orbital eccentricity-radius relation for small planets is indicative of the predominant dynamical sculpting processes during late-stage orbital evolution.
The Transiting Exoplanet Survey Satellite (TESS) has been highly successful in detecting planets in close orbits around low-mass stars, particularly M dwarfs.
We present the Rossiter-McLaughlin measurement of the sub-Neptune TOI-1759A b with MAROON-X. A joint analysis with MuSCAT3 photometry and nine additional TESS transits produces a sky-projected obliquity of |λ|= 4∘±18∘.
We aim to discover whether the stellar multiplicity rate may provide information on the origin of recently discovered planets in the Neptunian Desert.
This thesis constitutes an observational effort to advance our understanding of planet formation and evolution across different regimes.
Exoplanet surveys like Kepler, TESS, and K2 have shown that planetary systems are common in our galaxy.
Small temperate planets are prime targets for exoplanet studies due to their possible similarities with the rocky planets in the Solar System.
