Astrobiology18- Page

Schematic diagram showing the three stages of cooling from Bondi radius delaminations. In (a), the planet forms a Bondi radius boundary layer of thickness ∆RB with a temperature contrast ∆TB

Binary collision-induced H2–He absorption coefficient, α, normalized by the hydrogen and helium gas densities, as function of frequency in the fundamental band, at 296 K. The parato-ortho distribution, is representative

Keith Cowing Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻 Follow on

Pit on Mars – NASA Editor’s note: On Earth pits – large caves – usually formed as chambers inside of limestone due to water erosion and collapses – can host

First direct image of 14 Her c. JWST/NIRCam coronagraphic imaging of the 14 Her system with the MASKA335R coronagraph (transmission indicated by gray shaded circles). North is up, east is

Results for particle injection simulations 1 and 2, that test the scattering efficiency of a Jupiter analog (e = 0.05; top panel) compared with an eccentric Jupiter (e = 0.23;

Drake Awards Celebrate the Search for Life Beyond Earth On May 20, the SETI Institute held its annual Drake Awards event in Mountain View, CA, honoring contributions to SETI or

The inferred occurrence rates of giant planets orbiting interior to the water ice line of Sun-like stars as a function of age. Schematic decreasing, consistent, and increasing giant planet frequency

Transit depth versus wavelength for our full atmosphere model of HD209458b (Model C). We zoom in past the extent of the Hα and He I 10830 ˚A line to show

X-ray Imaging Spectroscopy Mission (XRISM) The X-ray Imaging Spectroscopy Mission (XRISM) provides the best spectral resolution with which to study Sulfur (S) K-shell photoabsorption features from the interstellar medium (ISM).