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29 lis 2021 · Imaging data reveals a low albedo of both moons – Phobos: ∼0.07; Deimos: ∼0.08. Also, Phobos manifests distinct redder and bluer units, whereas the surface of Deimos is globally comparable to the Phobos redder units with localized streaks of brighter material.
High temperatures for Phobos were measured at 25 degrees Fahrenheit (-4 degrees Celsius) and lows at -170 degrees Fahrenheit (-112 degrees Celsius). This intense heat loss is likely a result of the fine dust on Phobos' surface, which is unable to retain heat.
8 gru 2017 · Phobos and Deimos bear more resemblance to asteroids than to Earth's moon. Both are tiny — the larger, Phobos, is only 14 miles across (22 kilometers), while the smaller, Deimos, is only 8...
This giant impact heats up the disk material (around ∼2000 K in temperature ) with an entropy increase of 1500 J K−1kg−1. Thus, the disk material should be mostly molten, though a tiny ∼ fraction of disk material ( <5% ) would even experience vaporization.
15 paź 2018 · Both Phobos' redder unit and Deimos indicate absorptions due to Fe-phyllosilicate near 0.65 µm (Murchie et al., 2008) and possibly olivine/pyroxene near 1 µm (Gendrin et al., 2005). Thermal infrared spectra show emission features consistent with phyllosilicates ( Giuranna et al., 2011 ).
Deimos’ density (1.471±0.166 g/cm3) is lower than Phobos’s (1.876 g/cm3). Also, while Deimos is uni-formly dark red, Phobos presents two spectral units: a “Redder Unit” (similar to Deimos) dominating most of Phobos (> 65%), and a “Bluer Unit” (red also, but significantly less so than Deimos) of more limited
18 kwi 2018 · Here, we use state-of-the-art models to determine the implied properties of a Phobos-Deimos–forming impact and whether these conditions can be met. We first simulate the accretion of moons from a circum-martian disk using a hybrid N-body model (16, 17) to constrain the disk properties needed to form Phobos-Deimos type systems. Then, we ...
