Astrobiology28- Page

A thick plume of sand and dust from the Sahara Desert is seen in these images blowing from the west coast of Africa across the Atlantic Ocean. Larger image Sandstorms,

Darkening of the Global Ocean. (A) The rate change (units per year) in the diffuse attenuation coefficient for downwelling irradiance at 490 nm measured from MODIS Aqua between 2003 and

Reflected light (top row) and polarized light (bottom row) spectra for various homogeneous, cloud-free planets with different surface types. The wavelength-dependent spectral features of desert, forest, and polar surfaces are

Condensation of major rock-forming phases from a gas of solar composition at P = 10-3 bar (modified after Davis and Richter, 2007). The first phases to form upon cooling are

Left: Map of the Orion Molecular Cloud (OMC) complex obtained with the IRAM 30m telescope in CO 2–1. The data are taken from Berné et al. . We indicate the

Overlook crater” near the summit of Kilauea Volcano — USGS It is important that we are able to accurately model the atmospheres of (exo)planets. This is because atmospheres play a

Triplet potential energy surface for the reaction of C with CH3CHO with geometries and energies calculated at the M06-2X/aug-cc-pVTZ level (energy values in black). Certain structures close in energy to

This artist’s conception shows a disk of dust and gas surrounding a young star with a large cavity carved out by a forming giant planet. The warm methanol gas tracing

TOI-6894b Exoplanet – artist’s impression Credit University of Warwick/Mark Garlick The host star, TOI-6894, is a red dwarf with only 20% the mass of the Sun, typical of the most