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Social and Behavioral Sciences Commons™
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Articles 1 - 2 of 2
Full-Text Articles in Social and Behavioral Sciences
Cognitive And Social/Behavioural Development At 3-4 Years In Relation To Family Background, Edward Melhuish, Louise Quinn, Kathy Sylva, Pam Sammons, Iram Siraj-Blatchford, Brenda Taggart, Kathleen Mcsherry, Mark Mccrory
Cognitive And Social/Behavioural Development At 3-4 Years In Relation To Family Background, Edward Melhuish, Louise Quinn, Kathy Sylva, Pam Sammons, Iram Siraj-Blatchford, Brenda Taggart, Kathleen Mcsherry, Mark Mccrory
Faculty of Social Sciences - Papers (Archive)
This longitudinal study assesses the attainment and development of children followed between the ages of 3 and 7 years. Over 700 children were recruited to the study during 1998 and 1999 from 80 pre-school centres. Both qualitative and quantitative methods (including multilevel modelling) are used to explore the effects of pre-school experience on children's cognitive attainment and social/behavioural development at entry to school and any continuing effects on such outcomes up to 7 years of age. In addition to the effects of preschool experience, the study investigates the contribution to children's development of individual and family characteristics such as gender, …
The Soft X-Ray Background: Evidence For Widespread Disruption Of The Gas Haloes Of Galaxy Groups, K K S Wu, A C. Fabian, Paul E. J Nulsen
The Soft X-Ray Background: Evidence For Widespread Disruption Of The Gas Haloes Of Galaxy Groups, K K S Wu, A C. Fabian, Paul E. J Nulsen
Faculty of Engineering and Information Sciences - Papers: Part A
Almost all of the extragalactic X-ray background (XRB) at 0.25 keV can be accounted for by radio-quiet quasars, allowing us to derive an upper limit of 4 keV cm−2 s−1 sr−1 keV−1 for the remaining background at 0.25 keV. However, the XRB from the gas haloes of groups of galaxies, with gas removal resulting from cooling accounted for, exceeds this upper limit by an order of magnitude if non-gravitational heating is not included. We calculate this using simulations of halo merger trees and realistic gas density profiles, which we require to reproduce the observed gas fractions …