Results 51 to 60 of about 7,284,804 (245)

Low heat cement and mass concrete construction

Materiales de Construccion, 1950
No ...
Editorial
doaj   +1 more source

Cosmic Strings in Low Mass Higgs Cosmology [PDF]

, 1998
A class of grand unified theories with symmetry breaking scale of order $10^{16} GeV$ have a Higgs particle with mass in the $TeV$ scale. The cosmology of such theories is very different from usual.
Anne-Christine Davis, Barreiro, Brandenberger, Davis, Davis, Freese, Kibble, Kolb, Lazarides, Lyth, Scherrer, Warren B. Perkins   +11 more
core   +2 more sources

Semiconvective mixing in low-mass stars [PDF]

Astrophysics and Space Science, 2010
Conference Proceedings HELAS Workshop on 'Synergies between solar and stellar modelling', Rome, June 2009, Astrophys.
J. Ballot, A. Weiss, V. Silva Aguirre, Aldo Serenelli   +3 more
openaire   +3 more sources

Hierarchy of the macrozone features in Ti-6Al-4V alloy inferred from massive polycrystal plasticity calculations

Journal of Materials Research and Technology
Titanium alloys exhibit complex microstructures containing heterogeneities at different length scales. Microtextured regions (MTRs), usually called “macrozones”, exhibit grains having the same or nearly the same crystallographic orientation.
Xiaolei Chen, Lionel Germain, Stéphane Berbenni   +2 more
doaj   +1 more source

Low bone mass secondary to antipsychotic medications

Saudi Journal of Medicine and Medical Sciences, 2016
Background and Objective: Antipsychotic medications are known to cause low bone mass. The objective of this study was to assess the prevalence of osteopenia and osteoporosis secondary to patients taking antipsychotic medications.
Abdallah S Al-Omran, Mahdi S Abu-Madini, Mir Sadat-Ali, Moaad H Alfaraidy, Waleed K Shihada   +4 more
doaj   +1 more source

Low-energy neutrino physics and neutrino mass [PDF]

, 1984
Among the principal concerns in neutrino physics today are the questions of whether neutrinos are massive and, if so, whether the neutrinos emitted in a weak decay are pure or mixed quantum states. The concept of mixed neutrinos has been with us for more
Boehm, F., Vogel, P.
core   +1 more source

Vortex Mass in a Superfluid at Low Frequencies [PDF]

Physical Review Letters, 2007
An inertial mass of a vortex can be calculated by driving it round in a circle with a steadily revolving pinning potential. We show that in the low frequency limit this gives precisely the same formula that was used by Baym and Chandler, but find that the result is not unique and depends on the force field used to cause the acceleration.
David J. Thouless, James R. Anglin
openaire   +4 more sources

Low-mass companions to Hyades stars

, 2005
It is now well established that a large fraction of the low-mass stars are binaries or higher order multiples. Similarly a sizable fraction have giant planets.
A. P. Hatzes, Abt, B. Macintosh, Boesgaard, Burrows, Cayrel, Chabrier, Chauvin, Chauvin, Close, Cochran, D. B. Paulson, Dahn, Duquennoy, E. W. Guenther, Endl, Fischer, Freed, Ghez, Goto, Guenther, Guenther, Henry, J. Patience, Kirkpatrick, Lebreton, Lineweaver, Liu, Lowrance, Lowrance, Malkov, Martín, Martín, Masciadri, Masciadri, Mazeh, Mazeh, McCarthy, McCaughrean, Nakajima, Neuhäuser, Neuhäuser, Neuhäuser, Neuhäuser, Patience, Paulson, Paulson, Paulson, Perryman, Potter, Reid, Santos, Seifahrt, Stern, Tinney, Torres, Udry, W. D. Cochran, Wuchterl, Zapatero Osorio, Zucker   +60 more
core   +1 more source

High-redshift galaxies and low-mass stars [PDF]

, 2014
The sensitivity available to near-infrared surveys has recently allowed us to probe the galaxy population at z ≈ 7 and beyond. The existing Hubble Wide Field Camera 3 (WFC3) and Visible and Infrared Survey Telescope for Astronomy (VISTA) Infrared Camera (
Bremer, Malcolm N, Stanway, Elizabeth R, Wilkins, Stephen M   +2 more
core   +2 more sources

THE MASS DISTRIBUTION OF COMPANIONS TO LOW-MASS WHITE DWARFS [PDF]

The Astrophysical Journal, 2014
Measuring the masses of companions to single-line spectroscopic binary stars is (in general) not possible because of the unknown orbital plane inclination. Even when the mass of the visible star can be measured, only a lower limit can be placed on the mass of the unseen companion.
Jeff J. Andrews, Marcel A. Agüeros, Adrian M. Price-Whelan   +2 more
openaire   +4 more sources