Spatial information from stellar X-ray coronae can be inferred by use of scaling laws from the solar corona. This requires measurement of the physical parameters temperature and density. We concentrate on the newly available density measurements from line fluxes of X-ray lines measured for a large sample of 64 grating spectra of 42 stellar coronae obtained with Chandra and XMM-Newton. Line counts of strong H-like and He-like ions and FeXXI lines were measured with the CORA line fitting tool by Ness and Wichmann 2002. Densities are estimated from He-like f/i flux ratios of OVII and NeIX representing only cooler (1-6MK) plasma components. The densities scatter between log n_e = 9.5-11 from the OVII triplet and between log n_e = 10.5-12 from the NeIX triplet, but we caution that the latter triplet may be biased by contamination from FeXIX and FeXXI lines. We find that low-activity stars tend to show densities of no more than a few times 10^10cm^-3, whereas no definitive trend is found for the more active stars. Investigating the densities of the hotter plasma with various FeXXI line ratios, we found no consistent proof for the presence of very high densities. This result is in line with constant pressure in the emitting active regions. We focus on the commonly used RTV78 scaling law to derive loop lengths from temperatures and densities assuming loop-like structures as identical building blocks. We derive emitting volumes from direct measurements of ion-specific emission measures and densities. Available volumes are calculated from the loop-lengths and stellar radii. The ratios of these volumes depict volume filling factors, which we find similar up to 0.1 for all stages of activity for OVII and increasing for NeIX.