Although various reactions involved in photoexcited states of polypyridyl ruthenium(II) complexes have been extensively studied, photoisomerization of the complexes is very rare. We report the first illustration of stoichiometric photoisomerization of trans-[Ru(tpy)(pynp)OH(2)](2+) (1a) [tpy = 2,2':6',2''-terpyridine; pynp = 2-(2-pyridyl)-1,8-naphthyridine] to cis-[Ru(tpy)(pynp)OH(2)](2+) (1a') and the isolation of 1a and 1a' for X-ray crystallographic analysis. Polypyridyl ruthenium(II) aquo complexes are attracting much attention related to proton-coupled electron transfer and water oxidation catalysis. We demonstrate that the photoisomerization significantly controls the redox reactions and water oxidation catalyses involving the ruthenium(II) aquo complexes 1a and 1a'.

Water oxidation to evolve O2 in photosynthesis is catalyzed by an enzyme whose active site contains a mu-oxo-bridged manganese core. Catalytic O2 evolution has been difficult to establish by manganese-oxo complexes in homogeneous aqueous solutions. The reaction of [(OH2)(terpy)MnIII(mu-O)2MnIV(terpy)(OH2)]3+ (terpy = 2,2':6',2' '-terpyridine) (1) with a CeIV oxidant leads to the decomposition of 1 to the permanganate ion without O2 evolution in an aqueous solution but catalytically produces O2 from water when 1 is adsorbed on clay compounds. 18O-labeling experiments showed that the oxygen atoms in O2 originate exclusively from water. Catalysis of O2 evolution requires cooperation of 2 equiv of 1 adsorbed on clay compounds.

Photosynthesis produces molecular oxygen from water catalyzed by an enzyme whose active site contains a tetramanganese−oxo core of incompletely established structure. The first functional mimic of this core has been synthesized containing a cubical [Mn4O4] n + core, surrounded by six facially bridging bidentate chelates to the manganese ions ((dpp)6Mn4O4 (1); dpp- = diphenylphosphinate anion). Bond enthalpy data predict that the Mn4O4 6+ core is thermodynamically capable of releasing molecular O2, but is kinetically prevented from doing so by an activation barrier. UV light absorption into a Mn−O charge-transfer excited state (but not excitation of a Mn ligand-field excited state) efficiently releases an O2 molecule if performed in the gas phase and concomitantly releases a bridging dpp- anion and the cationic species (dpp)5Mn4O2 + (presumed Mn4O2-butterfly core type). All species were identified by high resolution mass spectrometry. This reaction proceeds with high quantum efficiency (>50%) and is the only observable reaction channel. The O2 product derived exclusively from the corner oxo's of the cube based on photochemistry of the 18O-isotopomer, ((dpp)6Mn4(18O)4. Neither O2 release nor dpp- dissociation are observed individually to occur in the excited state, indicating that O−O bond formation and O2 release require dissociation of one of the six dpp- chelates (“Jack-in-the-Box” mechanism for O2 formation). By contrast, neither O2 production nor chelate photodissociation are observed in condensed phases, presumably due to either quenching of the photoexcited state or rapid recombination of dpp- and (dpp)5Mn4O4 + in the solvent cage. Previous results show that chemical reduction of (1) in solution using hydrogen atom donors produces the deoxygenated (dpp)6Mn4O2 core and releases two water molecules as the only products. Thus the [Mn4O4] n + cubane core is an intrinsically reactive core topology that facilitates both the selective chemical reduction of two of the four oxygen atom bridges to water molecules and their photorearrangement to an O2 molecule under the control of chelation of the manganese ions by dpp-. These results may offer insight into the possible nature of the photosynthetic O2-evolving mechanism.

[1] We describe the Mars ionosphere with unprecedented detail in 3-D, as simulated by a Mars general circulation model (the Laboratoire de Météorologie Dynamique Mars GCM), and compare it with recent measurements. The model includes a number of recent extensions and improvements. Different simulations for a full Martian year have been performed. The electron density at the main ionospheric peak is shown to vary with the Sun-Mars distance and with the solar variability, both in the long-term (11 year solar cycle) and on shorter temporal scales (solar rotation). The main electronic peak is shown to be located at the same pressure level during all the Martian year. As a consequence, its altitude varies with latitude, local time, and season according to the natural expansions and fluctuations of the neutral atmosphere, in agreement with previous models. The model predicts a nighttime ionosphere due only to photochemistry. The simulated ionosphere close to the evening terminator is in agreement with observations. No effort has been made to explain the patchy ionosphere observed in the deep nightside. We have compared the modeled ionosphere with Mars Global Surveyor and Mars Advanced Radar for Subsurface and Ionosphere Sounding data. The model reproduces the solar zenith angle variability of the electron density and the altitude of the peak, although it underestimates the electron density at the main peak by about 20%. The electron density at the secondary peak is strongly underestimated by the model, probably due to a very crude representation of the X-ray solar flux. This is one of the aspects that needs a revision in future versions of the model.