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28 Jul 2006: as to be expected, the figure is much lower for the 200 journals with highest cumulative impact.

30 May 2006: directEntries 2000000Mean -0.02588. RMS 17.87. -600 -400 -200 0 200 400 6001. ... directEntries 2000000Mean -0.02588. RMS 17.87. badEntries 2000000Mean 0.01601. RMS 7.586. -600 -400 -200 0 200 400 6001.

30 May 2006: Y f 5 200 -. 6 a. 250 -. 300 -. Salinity ( % o ). I I I I I I I I 34.2 34.3 3 4 4 34.5 34.6 34.7 ... 200. n E. 300. 350. I I 0.1 OC. FIGURE 8.

21 Sep 2006: 0 50 100 150 200 250 300 350 4000.25. 0.2. 0.15. ... Fea. ture. Val. ueBatch OSMINC OSM. 50 100 150 200 250 300 350 4000.

5 May 2006: Details of our finite-difference numericalcode are presented the Appendix. We used a mesh of 320 horizontal and 200 verticalintervals.

19 Apr 2006: up to 200 km in diameter) for impacts with a range ofimpact parameters and with relative velocities comparable to thoseexpected in extrasolar planetesimal discs. ... 6b), all models predict a lifetimethat is shorter than the age of the system (200 Myr)

19 Apr 2006: Compared to the fullextent of the mid-IR–emitting size of the disk (200 AU), therelatively small values of the dust FWHM sizes suggest thatthe mid-IR emission is sharply peaked ... extends out to at least a radius of 100 (200 AU) fromthe star in the

6 Dec 2006: 150 C, 200 C, 250 C, and 300 C at various nitgen pressures. ... Above 200 Cconductivity becomes almost independent of N contentits dependence on temperature declines.

13 Nov 2006: 3(b). The AFM analysis shows a w of 40,200 and 100 nm for a respective original 0.3-, 1- and 5-nmFe thickness (Figs. ... Annealing in pure NH3 (200 sccm, 0.6 mbar pressure) at500 C results in a distinctively different topography for all Fethicknesses.

19 Apr 2006: Fitting a Gaussian to therebinned 850 m data indicates that the 850 m emission has aFWHM of 19B4 0B2 and is centered on the star to within 200. ... the disk around star Fomalhaut, which has anage of 200 Myr (Wyatt & Dent 2002).