In all cases a blackish magnetic residue was left undissolved.
"Scientific American Supplement, No. 415, December 15, 1883" by Various
Only here we must have just a little residual magnetism in the field magnet to start the whole process.
"A Librarian's Open Shelf" by Arthur E. Bostwick
On moving the bar from the pole the bound magnetism is released and a part becomes residual magnetism.
"Scientific American, Volume 40, No. 13, March 29, 1879" by Various
One side of both shell and core are split for the purpose of obviating residual magnetism.
"Scientific American, Volume XXXVI., No. 8, February 24, 1877" by Various
It left a residue of black powder, which contained grains of metallic iron that were attracted by the magnet.
"The Voyage of the Vega round Asia and Europe, Volume I and Volume II" by A.E. Nordenskieold
At the start the residual magnetism of the magnet cores gives a weak field.
"How it Works" by Archibald Williams
The incepting energy influence is found in the residual magnetism.
"The Energy System of Matter" by James Weir
A machine in which the initial excitation of the field is due to the residual magnetism retained by the cores.
"Hawkins Electrical Guide, Number One" by Nehemiah Hawkins
***
For our computation, we use Nd-Fe-B magnets which have currently the higher residual magnetization (Br = 1.3 T); the density of this material is ρ = 7.4 g/cm3 .
Feasibility of a magnetic suspension for second generation Gravitational Wave interferometers
However the induced e.m. f . for 56 Ari may differ by an order of magnitude, but this remains uncertain due to poorly known magnetic ﬁeld geometry. A single-wave variation of the residual spectra is a characteristic signature for both θ Aur and 56 Ari.
The Lorentz force in atmospheres of CP stars: 56 Arietis
Residual effects of turbulence a re seen in self-gravitating molecular clouds, but they appear to be magnetically supported, with the condition rg ≃ (cid:209)PB approximately satis ﬁed.
Cosmic Magnetic Fields: from Stars and Galaxies to the Primordial Universe
The residual, besides the resolutions of each BPM, depends on the ﬂuctuations of the magnetic ﬁelds, mechanical vibrations, as well as drifts and other sy stematic effects and non-linearities.
Results from a Prototype Chicane-Based Energy Spectrometer for a Linear Collider
We investigated the impact of astrophysical residuals on the magnetic parameters with a MCMC analysis using the same data but neglecting all the three astrophysical signals.
Constraints on a Stochastic Background of Primordial Magnetic Fields with WMAP and South Pole Telescope data
In order to not introduce biases in the magnetic parameter constraints we have considered the contamination by astrophysical residuals of the SPT data.
Constraints on a Stochastic Background of Primordial Magnetic Fields with WMAP and South Pole Telescope data
We prove that the model deﬁned on Z3 with nearest neighbor coupling exhibits residual magnetic order in the horizontal direction for arbitrarily weak random ﬁeld strengths and, depending on ﬁeld strength, sufﬁciently low temperature.
Random Field Induced Order in Low Dimension I
Gibbs state by h·i = h·iσ0 Λ, the question is whether and when, in terms of β, ǫ and σ0, residual magnetic ordering occurs in the limit as Λ ↑ Zd .
Random Field Induced Order in Low Dimension I
If d ≥ 3, residual magnetic ordering occurs . • The Random Field Ising Model.
Random Field Induced Order in Low Dimension I
The resulting picture shortly after the critical point is a paramagnetic phase of localized spinons, as we can neglect tiny residual magnetic couplings between spinons for a small enough density.
Localization of spinons in random Majumdar-Ghosh chains
Indeed, due to the localization of spinons, triplet and singlet states are degenerate within an energy gap that is tiny (we observed gaps below 10−8β ) and controlled by the residual magnetic couplings between spinons.
Localization of spinons in random Majumdar-Ghosh chains
The center “thinning” of the Sirocco x-residuals (from a gaussian) by ≃ 1 µm was due to the residual magnetic ﬁeld of the Spectrometer Magnet, as Lorentz drift of the charge carriers in the strips.
Analytical and Numerical Flash-Algorithms for Track Fits
The accelerated e± move in the residual magnetic ﬁeld and the ﬁeld of waves and emit photons of energy hν ∼ γ 2¯h(c/r0) ∼ MeV.
Prompt Emission and Early Afterglows of Gamma-Ray Bursts
Here N (0, θ) is the residual density of states in the presence of a magnetic ﬁeld and θ refers to the ﬁeld orientation.
Thermal Conductivity in Vortex State of Nodal Superconductors
Within our resolution and limitation in lattice size, we observe no anomaly in the quasiparticle residue across the magnetic order-disorder phase transition (Jc /t ≃ 1.45).
Coherence scale of the two-dimensional Kondo Lattice model
***