Thermodynamic properties of sulphites. I. Standard heats of formation

1962 ◽  
Vol 27 (6) ◽  
pp. 1428-1437 ◽  
Author(s):  
E. Erdös
1964 ◽  
Vol 17 (10) ◽  
pp. 1063 ◽  
Author(s):  
AG Turnbull

Heats of solution in 3.83N HF have been measured for zirconium metal and for five zirconium hydrides to evaluate the following heats of formation AHf0298: ZrH2 -39.7, ZrH1.85 -38.2, ZrH1.70. -34.7, ZrH1.43 -30.05, ZrH1.23 -25.3 kcal/mole hydride. A review of heat capacity and entropy data for zirconium hydrides has enabled a good correlation to be made between calorimetric and dissociation pressure studies, so that the effect of composition on all thermodynamic properties is established.


1957 ◽  
Vol 79 (3) ◽  
pp. 561-566 ◽  
Author(s):  
J. P. McCullough ◽  
W. N. Hubbard ◽  
F. R. Frow ◽  
I. A. Hossenlopp ◽  
Guy Waddington

1967 ◽  
Vol 20 (10) ◽  
pp. 2059 ◽  
Author(s):  
AG Turnbull

Standard free energies of formation for the temperature range 298- 1000�K are calculated for C5H5, C5H6, and the biscyclopentadienyl compounds of iron, ruthenium, nickel, and magnesium by combining reported heats of formation at 298�K with calculated ideal-gas thermodynamic properties. The results are used to predict the thermodynamic feasibility of three types of reactions-the formation of biscyclopentadienyl metal compounds, their thermal decomposition, and their reduction with hydrogen. It is shown that the predictions are in agreement with qualitative chemical observations.


1979 ◽  
Vol 44 ◽  
pp. 349-355
Author(s):  
R.W. Milkey

The focus of discussion in Working Group 3 was on the Thermodynamic Properties as determined spectroscopically, including the observational techniques and the theoretical modeling of physical processes responsible for the emission spectrum. Recent advances in observational techniques and theoretical concepts make this discussion particularly timely. It is wise to remember that the determination of thermodynamic parameters is not an end in itself and that these are interesting chiefly for what they can tell us about the energetics and mass transport in prominences.


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