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Perceived importance and didactic difficulty of chemistry education: Insights from Czech teachers

open access: yesThe Curriculum Journal, EarlyView.
Abstract This empirical study examines how chemistry teachers in lower and upper secondary schools in the Czech Republic evaluate the content of the chemistry curriculum, focussing on its perceived importance and didactic difficulty. Based on a quantitative survey (N = 146), the study provides insight into the pedagogical content knowledge of ...
Jitka Lorenzová   +6 more
wiley   +1 more source

Exploring the extremes: The cosmic laboratory. [PDF]

open access: yesInnovation (Camb)
Huang Y, He S, Ge L, Li Z, Mao Y, Liu J.
europepmc   +1 more source

Surface hydration‐induced damage in tight oil‐bearing sandy conglomerate reservoirs

open access: yesDeep Underground Science and Engineering, EarlyView.
A series of techniques such as X‐ray diffraction, scanning electron microscopy, energy‐dispersive spectroscopy, conductivity tests, and infrared thermal imaging were used. The key findings are the identification of a two‐stage surface hydration process and the elucidation of the effects of various minerals and elements on the hydration process ...
Anbang Zhao   +5 more
wiley   +1 more source

Gravitational-wave constraints on the pair-instability mass gap and nuclear burning in massive stars. [PDF]

open access: yesNat Astron
Antonini F   +7 more
europepmc   +1 more source
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Neutron star crusts

Physical Review Letters, 1993
We calculate properties of neutron star matter at subnuclear densities using an improved nuclear Hamiltonian. Nuclei disappear and the matter becomes uniform at a density of about 0.6n(s), where n(s) of about 0.16/cu fm is the saturation density of nuclear matter. As a consequence, the mass of matter in the crusts of neutron stars is only about half as
, Lorenz, , Ravenhall, , Pethick
openaire   +2 more sources

Neutron star matter

Nuclear Physics A, 1971
Abstract The matter in neutron stars is essentially in its ground state and ranges in density up to and beyond 3 × 10 14 g/cm 3 , the density of nuclear matter. Here we determine the constitution of the ground state of matter and its equation of state in the regime from 4.3 × 10 11 g/cm 3 where free neutrons begin to “drip” out of the nuclei, up ...
GORDON BAYM   +2 more
openaire   +1 more source

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