Astrobiology2- Page

Overview of the chemical elements detected in the transmission spectra of Ultra-Hot Jupiters (UHJ). Planets are ordered by decreasing equilibrium temperature. WASP-33 b is a more challenging target due to

The HPF-SpecMatch spectra fit results for order index 5. Top: two plots showing the five best-fit stars (red) selected to compose the spectra. The size and transparency of these five

Displaying the sudden change in spectral features for oxygen-rich atmospheric spectra. Type B atmospheres spectra do not show any CH4 features, as do type C which are extremely oxygen-rich. Both

Phosphorus abundances as a function of fundamental stellar parameters for all sample stars. Upper panel: Phosphorus abundance as a function of Teff. Lower panel: Phosphorus abundance as a function of

Transformations between the ORF (blue), SRF (orange), and BRF (green), with Euler angles. The SRF and the BRF are both rotating frames, with ZS the spin axis of Venus and

State of the Cryosphere Report 2024 In the State of the Cryosphere 2024 – Lost Ice, Global Damage report, over 50 leading cryosphere scientists warn of vastly higher impacts and

Disk reflectance spectra at different stellocentric distances. a, The disk reflectance spectra at 80- 90 au (region 1, yellow), 90-105 au (region 2, orange), and 105-120 au (region 3, cyan),

Frozen Water in Young Star System HD 181327 — NASA Is frozen water scattered in systems around other stars? Astronomers have long expected it is, partially based on previous detections

Disk-averaged JWST spectra of Titan. Top, NIRSpec. Bottom, MIRI (channels 1B–3C). The main absorption and emission bands (the latter labelled with an asterisk) are shown, as well as spectral transmission