Lava planets likely did not form in their current orbits, instead migrating inward via orbital decay, which influenced the evolution of their magma oceans.
Lava planet
Posted inAstrogeology, Exoplanets, -moons, -comets, Status Report, Stellar Cartography
The Role Of Inner Disk Edges In Shaping Ultra-short-period Planet Systems Around Late M Dwarfs
Close-in rocky planets are the most common type of exoplanets around late M dwarfs, ranging from more temperate worlds to highly irradiated lava planets with molten surfaces, and many theoretical […]
Posted inAstrogeology, Atmospheres, Climate, Weather, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Lava / magma ocean / Volcanic Worlds, Status Report
The Effect of Tidal Heating and Volatile Budgets on the Outgassed Atmosphere of 55 Cancri e
55 Cancri e is a ∼8 Gyr rocky world (1.95 R⊕, 8.8 M⊕) orbiting a K-type star. JWST observations suggest a carbon-dominated atmosphere (CO2/CO) over a global magma ocean (>3000 […]
Posted inAstrogeology, Atmospheres, Climate, Weather, Biogeochemical Cycles & Geobiology, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Lava / magma ocean / Volcanic Worlds, Status Report
Rock Vapour Is Opaque: Implications For Dynamics And Observations Of Lava Planets
Extreme instellation on lava planets causes the rocky surface to melt and vaporize. Because the rock vapour composition is intrinsically tied to the mantle, atmospheric characterization of lava planets can […]
Posted inAstrochemistry, Atmospheres, Climate, Weather, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Status Report
SpeCT: A state-of-the-art Tool To Calculate Correlated-k Tables And Continua Of CO2-H2O-N2 Gas Mixtures
A key challenge in modeling (exo)planetary atmospheres lies in generating extensive opacity datasets that cover the wide variety of possible atmospheric composition, pressure, and temperature conditions.
Posted inAstrogeology, Biogeochemical Cycles & Geobiology, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Lava / magma ocean / Volcanic Worlds, Press Release
Melting Planets Reveal The Internal History Of Rocky Worlds
An international research team, led by scientists from the Institut de Physique du Globe de Paris (IPGP) in collaboration with researchers from Canada and the United Kingdom, reveals in a […]
Posted inAstrogeology, Atmospheres, Climate, Weather, Biogeochemical Cycles & Geobiology, Habitable Zones, Lava / magma ocean / Volcanic Worlds, Status Report, Water/Hycean Worlds & Oceanography
Thermal Evolution Of Lava Planets
Rocky planets are thought to form with a magma ocean that quickly solidifies. The horizontal and vertical extent of this magma ocean depends on the interior thermal evolution of the […]
Posted inAtmospheres, Climate, Weather, Biogeochemical Cycles & Geobiology, Imaging & Spectroscopy, Lava / magma ocean / Volcanic Worlds, Status Report
Clouds On Partial Atmospheres Of Lava Planets And Where To Find Them
With dayside temperatures hot enough to sustain a magma ocean and a silicate atmosphere, lava planets are the best targets to study the atmosphere of a rocky world.
Posted inAstrogeology, Atmospheres, Climate, Weather, Biogeochemical Cycles & Geobiology, Exoplanets, -moons, -comets, Press Release
Young Earth-like Planet With Lava Oceans
Astronomers have discovered an extreme Earth-like planet that likely hosts lava oceans as it roasts next to its sun-like star near the Big Dipper constellation.
![Compositional evolution of lava planets interiors from an initial homogeneous molten state. Chemical fractionation occurs during planetary solidification because rock-forming elements do not have the same affinities for liquid and solid phases. For instance, FeO prefers to remain in the liquid rather than being incorporated in the solids. (a and b) Initial conditions. The magma ocean is well mixed and nearly entirely molten. The composition of the magma ocean corresponds to the bulk planet’s composition, i.e., 6% of FeO (BSE composition). This is the global magma ocean stage. (c and d) Onset of the mushy stage. The MO crystal fraction is about 50%. Iron-rich solids accumulate in the deep mantle. The most liquid part of the planet shows a FeO content of 10%. (e-f) End of the mushy stage. The FeO concentration of the MO reaches its maximum, 12%. (g-h) Solid-state stage. The iron-rich shallow magma ocean has been buried in the deep mantle. The day-side shallow magma ocean has a concentration of about about 2%. The solid mantle is strongly layered. Iron-rich solids remelts to form a basal magma ocean. -- astro-ph.EP]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2023/08/Lava-planets.png?resize=1200%2C720&ssl=1)
Posted inAstrogeology, Biogeochemical Cycles & Geobiology, Caves, Craters, Mountains, Subsurface, Lava Tubes, Exoplanets, -moons, -comets, Io, Status Report
Lava Planets Interior Dynamics Govern The Long-term Evolution Of Their Magma Oceans
Lava planets are rocky exoplanets that orbit so close to their host star that their day-side is hot enough to melt silicate rock. Their short orbital periods ensure that lava […]