Hydrodynamic models of the τ Ceti astrosphere, assuming stellar mass loss rates of M˙= 0.03 M˙⊙ (left) and M˙= 0.1 M˙⊙ (right). The top panels show neutral H density and

a Estimated NH3 production rate as a function of Venusian altitude (48 to 85 km) formed by different S0 allotropes, calculated using two established aerosol and vapor models constrained by Venusian

Intensity maps at 4.4 µm with the apertures chosen for the fit. Aperture centers and diameters are listed in Table C.1. — astro-ph.GA Context. There are only six molecules containing

The integrated intensity images of CH3OH transitions overlaid with dust continuum (black contours at σ and σ = 0.10 K). The integration intervals span from −2.5

The posteriors were derived by applying the planetary evolution and mass loss framework of ref. 32 to our measured masses and radii for planets c (red), d (orange), b (green)

(a,b) An example of the transmittance spectra taken with the full-scan mode of the SO channel of TGO/NOMAD. (c,d) An example of the transmittance spectra taken with the full-scan mode