Movement and diffusion of pore fluids in Owens Lake sediments from core OL-92 as shown by salinity and deuterium-hydrogen ratios

Author(s):  
Irving I. Friedman ◽  
James L. Bischoff ◽  
Craig A. Johnson ◽  
Scott W. Tyler ◽  
Jeffrey P. Fitts
1998 ◽  
Vol 50 (2) ◽  
pp. 113-127 ◽  
Author(s):  
Larry V. Benson ◽  
Howard M. May ◽  
Ronald C. Antweiler ◽  
Terry I. Brinton ◽  
Michaele Kashgarian ◽  
...  

The chemistry of the carbonate-free clay-size fraction of Owens Lake sediments supports the use of total organic carbon and magnetic susceptibility as indicators of stadial–interstadial oscillations. Owens Lake records of total organic carbon, magnetic susceptibility, and chemical composition of the carbonate-free, clay-size fraction indicate that Tioga glaciation began ∼24,500 and ended by ∼13,60014C yr B.P. Many of the components of glacial rock flour (e.g., TiO2, MnO, BaO) found in Owens Lake sediments achieved maximum values during the Tioga glaciation when valley glaciers reached their greatest extent. Total organic carbon and SiO2(amorphous) concentrations reached minimum values during Tioga glaciation, resulting from decreases in productivity that accompanied the introduction of rock flour into the surface waters of Owens Lake. At least 20 stadial–interstadial oscillations occurred in the Sierra Nevada between 52,600 and 14,00014C yr B.P. Total organic carbon data from a Pyramid Lake sediment core also indicate oscillations in glacier activity between >39,500 and ∼13,60014C yr B.P. Alpine glacier oscillations occurred on a frequency of ≤1900 yr in both basins, suggesting that millennial-scale oscillations occurred in California and Nevada during most of the past 52,600 yr.


1989 ◽  
Vol 25 (8) ◽  
pp. 1815-1823 ◽  
Author(s):  
R. J. Cornett ◽  
B. A. Risto ◽  
D. R. Lee

1991 ◽  
Vol 24 (4) ◽  
pp. 2330-2334
Author(s):  
R. J. Cornett ◽  
B. A. Risto
Keyword(s):  

1976 ◽  
Vol 32 ◽  
pp. 109-116 ◽  
Author(s):  
S. Vauclair

This paper gives the first results of a work in progress, in collaboration with G. Michaud and G. Vauclair. It is a first attempt to compute the effects of meridional circulation and turbulence on diffusion processes in stellar envelopes. Computations have been made for a 2 Mʘstar, which lies in the Am - δ Scuti region of the HR diagram.Let us recall that in Am stars diffusion cannot occur between the two outer convection zones, contrary to what was assumed by Watson (1970, 1971) and Smith (1971), since they are linked by overshooting (Latour, 1972; Toomre et al., 1975). But diffusion may occur at the bottom of the second convection zone. According to Vauclair et al. (1974), the second convection zone, due to He II ionization, disappears after a time equal to the helium diffusion time, and then diffusion may happen at the bottom of the first convection zone, so that the arguments by Watson and Smith are preserved.


1997 ◽  
Vol 101-103 (1-2) ◽  
pp. 479-487
Author(s):  
H v. Wensierski
Keyword(s):  

Sign in / Sign up

Export Citation Format

Share Document