TRAPPIST-1

Predicting the Long-term Stability of Compact Multiplanet Systems

Predicting the Long-term Stability of Compact Multiplanet Systems

We combine analytical understanding of resonant dynamics in two-planet systems with machine learning techniques to train a model capable of robustly classifying stability in compact multi-planet systems over long timescales of 109 orbits.

Fossils

Biosignatures May Reveal a Wealth of New Data Locked Inside Old Fossils

Biosignatures May Reveal a Wealth of New Data Locked Inside Old Fossils

Step aside, skeletons -- a new world of biochemical "signatures" found in all kinds of ancient fossils is revealing itself to paleontologists, providing a new avenue for insights into major evolutionary questions.

Extrasolar Planets

The Role of Clouds on the Depletion of Methane and Water Dominance in the Transmission Spectra of Irradiated Exoplanets

The Role of Clouds on the Depletion of Methane and Water Dominance in the Transmission Spectra of Irradiated Exoplanets

Observations suggest an abundance of water and paucity of methane in the majority of observed exoplanetary atmospheres. We isolate the effect of atmospheric processes to investigate possible causes.

Oceanic Research

A New Look At Deep Sea Microbes

A New Look At Deep Sea Microbes

Microbial cells are found in abundance in marine sediments beneath the ocean and make up a significant amount of the total microbial biomass on the planet.

Enceladus

A Pole-to-Equator Ocean Overturning Circulation on Enceladus

A Pole-to-Equator Ocean Overturning Circulation on Enceladus

Enceladus is believed to have a saltwater global ocean with a mean depth of at least 30~km, heated from below at the ocean-core interface and cooled at the top, where the ocean loses heat to the icy lithosphere above.

TRAPPIST-1

Water Transport Throughout The TRAPPIST-1 System: The Role Of Planetesimals

Water Transport Throughout The TRAPPIST-1 System: The Role Of Planetesimals

Observational data suggest that a belt of planetesimals is expected close to the snow line in protoplanetary disks. Assuming there is such a belt in TRAPPIST-1 system, we examine possibilities of water delivery to the planets via planetesimals from the belt.

Habitable Zones & Global Climate

Habitability Models for Planetary Sciences

Habitability Models for Planetary Sciences

Habitability has been generally defined as the capability of an environment to support life. Ecologists have been using Habitat Suitability Models (HSMs) for more than four decades to study the habitability of Earth from local to global scales.

Impact events

Atmospheric Erosion By Giant Impacts Onto Terrestrial Planets: A Scaling Law for any Speed, Angle, Mass, and Density

Atmospheric Erosion By Giant Impacts Onto Terrestrial Planets: A Scaling Law for any Speed, Angle, Mass, and Density

We present a new scaling law to predict the loss of atmosphere from planetary collisions for any speed, angle, impactor mass, target mass, and body compositions, in the regime of giant impacts onto broadly terrestrial planets with relatively thin atmospheres.

Extrasolar Planets

The Dynamic Proto-atmospheres Around Low-Mass Planets With Eccentric Orbits

The Dynamic Proto-atmospheres Around Low-Mass Planets With Eccentric Orbits

Protoplanets are able to accrete primordial atmospheres when embedded in the gaseous protoplanetary disk. The formation and structure of the proto-atmosphere are subject to the planet--disk environment and orbital effects.

Habitable Zones & Global Climate

Sensitivity Of The Atmospheric Water Cycle Within The Habitable Zone Of A Tidally-Locked, Earth-like Exoplanet

Sensitivity Of The Atmospheric Water Cycle Within The Habitable Zone Of A Tidally-Locked, Earth-like Exoplanet

Synchronously orbiting, tidally-locked exoplanets with a dayside facing their star and a permanently dark nightside orbiting dim stars are prime candidates for habitability. Simulations of these planets often show the potential to maintain an Earth-like climate with a complete hydrological cycle.

Astrochemistry

Graphene Molecules Contributing to the Infrared Bands of Carbon Rich Planetary Nebulae

Graphene Molecules Contributing to the Infrared Bands of Carbon Rich Planetary Nebulae

It is well known since 2010 that fullerene C60 is widespread through the interstellar space. Also, it is well known that graphene is a source material for synthesizing fullerene. Here, we simply assume the occurrence of graphene in space.

More top stories from July.