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Reflections on Dr. King
Frady\u27s latest examines civil rights leader\u27s life, legac
High resolution spectroscopy of Pluto's atmosphere: detection of the 2.3 m CH bands and evidence for carbon monoxide
The goal is to determine the composition of Pluto's atmosphere and to
constrain the nature of surface-atmosphere interactions.
We perform high--resolution spectroscopic observations in the 2.33--2.36
m range, using CRIRES at the VLT.
We obtain (i) the first detection of gaseous methane in this spectral range,
through lines of the + and + bands (ii) strong
evidence (6- confidence) for gaseous CO in Pluto. For an isothermal
atmosphere at 90 K, the CH and CO column densities are 0.75 and 0.07 cm-am,
within factors of 2 and 3, respectively. Using a physically--based thermal
structure model of Pluto's atmosphere also satisfying constraints from stellar
occultations, we infer CH and CO mixing ratios q=
0.6% (consistent with results from the 1.66 m range) and
q = 0.5. The CO atmospheric abundance is
consistent with its surface abundance. As for Triton, it is probably controlled
by a thin, CO-rich, detailed balancing layer resulting from seasonal transport
and/or atmospheric escape.Comment: Astronomy and Astrophysics Letters, in pres
Io: IUE observations of its atmosphere and the plasma torus
Two of the main components of the atmosphere of Io, neutral oxygen and sulfur, were detected with the IUE. Four observations yield brightnesses that are similar, regardless of whether the upstream or the downstream sides of the torus plasma flow around Io is observed. A simple model requires the emissions to be produced by the interaction of O and S columns in the exospheric range with 2 eV electrons. Cooling of the 5 eV torus electrons is required prior to their interaction with the atmosphere of Io. Inconsistencies in the characteristics of the spectra that cannot be accounted for in this model require further analysis with improved atomic data. The Io plasma torus was monitored with the IUE. The long-term stability of the warm torus is established. The observed brightnesses were analyzed using a model of the torus, and variations of less than 30 percent in the composition are observed, the quantitative results being model dependent
Hybrid protoneutron stars with the MIT bag model
We study the hadron-quark phase transition in the interior of protoneutron
stars. For the hadronic sector, we use a microscopic equation of state
involving nucleons and hyperons derived within the finite-temperature
Brueckner-Bethe-Goldstone many-body theory, with realistic two-body and
three-body forces. For the description of quark matter, we employ the MIT bag
model both with a constant and a density-dependent bag parameter. We calculate
the structure of protostars with the equation of state comprising both phases
and find maximum masses below 1.6 solar masses. Metastable heavy hybrid
protostars are not found.Comment: 12 pages, 9 figures submitted to Phys. Rev.
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