Results 251 to 260 of about 7,037,410 (298)

Correction: Insights into Sudbury's deep architecture: a revised geodynamic model for Earth's largest ore-bearing impact structure. [PDF]

Sci Rep
Haugaard R, Spray JG, Adetunji AQ, Vayavur R, Hamilton MA, Snyder D, Cheraghi S, Ayer J, Henry K, Jørgensen TRC, Serafini G, Smith R, Gibson L.   +12 more
europepmc   +1 more source

Systems-Based Dialogue With Secondary School Students to Explore School Food Environments That Promote Healthy People and Planet. [PDF]

J Hum Nutr Diet
Browne S, Dooley A, Lovett E, Fhionnghalaigh AN, O'Neill A.   +4 more
europepmc   +1 more source

Filamentary structures in planetary nebulae

, 2005
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Composition and structure of planetary atmospheres

Space Science Reviews, 1971
Donald M Hunten
exaly   +2 more sources

Dipole structure of planetary atoms

Physical Review Letters, 1992
Using resonant multiphoton laser excitation in combination with temporarily applied electric fields we have excited high-lying planetary states in strontium. Thereby, the angular momenta were high enough to prevent penetration of the ${\mathrm{Sr}}^{++}$ core, as well as the mutual penetration of the two excited wave functions. Analysis of the spectra (
, Eichmann, , Lange, , Sandner
openaire   +2 more sources

An experiment to determine the structure of a planetary atmosphere

5th Annual Meeting and Technical Display, 1968
Planetary atmosphere structure and mean molecular weight determination from onboard measurements tested at high altitude in earth atmosphere, based on NASA ...
SIMON C. SOMMER, LAYTON YEE
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Formation of a filamentary structure in planetary nebulae

Astrophysics and Space Science, 1995
Intricate filamentary structure and multiple shell—like appearance are very common phenomena in Planetary Nebulae.
G. Pascoli, J. Leclercq
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On the radial structure of planetary rings

International Astronomical Union Colloquium, 1984
ABSTRACTA ring of particles in orbit about a planet experiences a viscous shear stress due to the radial gradient of orbital velocity. This stress tends to spread the ring with time. At low optical depth (τ ≲ 0.5), and again at high optical depth (τ ≳ 2), the shear stress is an increasing function of optical depth.
A.W. Harris, W.R. Ward
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The Structuring of Planetary Nebulae

AIP Conference Proceedings, 2005
This paper discusses some features in Planetary Nebulae and Protoplanetary Nebulae that are addressed by several works on MHD. We review different scenarios for the origin of magnetized winds, either for Protoplanetary Nebulae or Planetary Nebulae, and discusses the production of axisymmetric flows, the confinement of flows and the production of jets ...
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