Gijs D Mulders

@gijsmulders.com

319 Followers 60 Following

Exoplanet Astronomy Assistant Professor Santiago de Chile http://gijs.cl \m/

Jupiter and Earth, size to scale

$Water mass fraction vs disk mass for planets within the habitable zone$

$Water mass fraction vs disk mass for planets within an orbital period of 100 days$

The bimodel pattern in core mass vs semi-major axes is consistent across stellar mass

Mid mass architecture with giant planet cores at the snow line and water-rich smaller planets in the habitable zone

Drumbeat

Low mass architecture with watery super-earth cores growing inside of the snow line

High mass architecture with planet cores growing outside of the snow line

$Snow line locations for different stellar masses and disk mass fractions$

Plot of planet core mass vs semi-major axis with 50 planetary seeds and a moving snow line

Plot of planet core mass vs semi-major axis with 100 planetary seeds

Diverse population of giant (exo)planets

Jupiter with impact marks from comet Shoemaker/Levy

$Earth with a small mass fraction of water, shown as a sphere$

Many Exoplanets

Exoplanet occurrence vs age literature comparison

Young exoplanet occurrence vs orbital period

Young exoplanet occurrence vs. radius

Young exoplanet occurrence at different orbital periods, vs. Kepler

Evolution of hypothetical planetary system with sub-Neptune planets. Credit: Abigail Minnich (abbyminnich.wixsite.com/film)

TESS detection efficiency for young planets around FGK stars

A transiting planet around an active star. Credit: NASA/JPL-Caltech

Young exoplanets from TESS compared to Kepler

Artist’s impression of the TESS mission
Credits NASA/MIT

Evolutionary stages of a hypothetical planetary system over time. The planets in the system, labeled b through f, are depicted at three distinct stages: 10–100 Myr (top panel), 100 Myr–1 Gyr (middle panel), and >1 Gyr (bottom panel). This progression highlights key processes shaping the system, such as atmospheric mass loss and compositional evolution driven by stellar radiation and planetary interactions. Image credit: Abigail Minnich (abbyminnich.wixsite.com/film)

Evolution of hypothetical planetary system with sub-Neptune planets. Credit: Abigail Minnich (abbyminnich.wixsite.com/film)

Alma OT calibration error meme

Stellar mass dependence of planet formation models. Pebble accretion models match the peak in exoplanet occurrence for early M dwarfs

Average Solid Mass in Sub-Neptunes and Giant Planets as function of stellar mass, compared to protoplanetary disk dust mass

Carmenes Radial Velocity Exoplanets around late M dwarfs

Carmenes Radial Velocity Exoplanets around Early M dwarfs

Small exoplanet occurrence versus stellar effective temperature