Assessment of some factors influencing tool wear on the machining of glass fibre-reinforced plastics by coated cemented carbide tools

Palanikumar, K.; Davim, J. Paulo

doi:10.1016/j.jmatprotec.2008.02.020

Cited by 93 publications

(55 citation statements)

References 22 publications

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“…Finally, in both cases, the convective (Moffatt & Loper 1994), we obtain velocities of ∼35 km s −1 . For the thermodynamical conditions found in white dwarf interiors, viscosities are very small and conductivities rather high (Nandkumar & Pethick 1984). In particular, for the heavier white dwarf, the electrical conductivity is s =1.3 10 21 s −1 , the magnetic diffusivity is h =´-5.6 10 2 cm 2 s −1…”

Section: The Stellar Dynamomentioning

confidence: 99%

A Common Origin of Magnetism from Planets to White Dwarfs

Isern

Garcı́a–Berro

Külebi

et al. 2017

ApJL

111

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Isolated magnetic white dwarfs have field strengths ranging from kilogauss to gigagauss. However, the origin of the magnetic field has not been hitherto elucidated. Whether these fields are fossil, hence the remnants of original weak magnetic fields amplified during the course of the evolution of their progenitor stars, or are the result of binary interactions, or, finally, they are produced by other internal physical mechanisms during the cooling of the white dwarf itself, remains a mystery. At sufficiently low temperatures, white dwarfs crystallize. Upon solidification, phase separation of its main constituents, 12 C and 16 O, and of the impurities left by previous evolution occurs. This process leads to the formation of a Rayleigh-Taylor unstable liquid mantle on top of a solid core. This convective region, as it occurs in solar system planets like the Earth and Jupiter, can produce a dynamo able to yield magnetic fields of strengths of up to 0.1 MG, thus providing a mechanism that could explain magnetism in single white dwarfs.

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Section: The Stellar Dynamomentioning

confidence: 99%

A Common Origin of Magnetism from Planets to White Dwarfs

Isern

Garcı́a–Berro

Külebi

et al. 2017

ApJL

111

View full text Add to dashboard Cite

show abstract

“…The magnetic diffusivity is the inverse of the electrical conductivity, which in RGB stars has to be calculated carefully as certain regions are partially/ fully degenerate. Moving from nondegenerate to partially and fully degenerate regions, we calculate the magnetic diffusivity according to Spitzer (1968), Wendell et al (1987), and Nandkumar & Pethick (1984), respectively, applying a smooth interpolation in the transition regions.…”

Section: Diffusion Versus Advectionmentioning

confidence: 99%

Asteroseismic Signatures of Evolving Internal Stellar Magnetic Fields

Cantiello

Fuller

Bildsten

2016

ApJ

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Recent asteroseismic analyses indicate the presence of strong (B  10 5 G) magnetic fields in the cores of many red giant stars. Here, we examine the implications of these results for the evolution of stellar magnetic fields, and we make predictions for future observations. Those stars with suppressed dipole modes indicative of strong core fields should exhibit moderate but detectable quadrupole mode suppression. The long magnetic diffusion times within stellar cores ensure that dynamo-generated fields are confined to mass coordinates within the main-sequence (MS) convective core, and the observed sharp increase in dipole mode suppression rates above 1.5 M e is likely explained by the larger convective core masses and faster rotation of these more massive stars. In clump stars, core fields of ∼10 5 G can suppress dipole modes, whose visibility should be equal to or less than the visibility of suppressed modes in ascending red giants. High dipole mode suppression rates in low-mass (M  2 M e ) clump stars would indicate that magnetic fields generated during the MS can withstand subsequent convective phases and survive into the compact remnant phase. Finally, we discuss implications for observed magnetic fields in white dwarfs and neutron stars, as well as the effects of magnetic fields in various types of pulsating stars.

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“…Although several authors [8,[37][38][39] have studied transport properties of the crust, very few studies employed dynamical approach. At first, Horowitz et al [3,4] and recently Alcain et al [40] studied neutrino-pasta scattering adopting classical molecular dynamics.…”

Section: Introductionmentioning

confidence: 99%

Transport Properties of the Nuclear Pasta Phase with Quantum Molecular Dynamics

Nandi

Schramm

2018

ApJ

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We study the transport properties of nuclear pasta for a wide range of density, temperature and proton fractions, relevant for different astrophysical scenarios adopting a quantum molecular dynamics model. In particular, we estimate the values of shear viscosity as well as electrical and thermal conductivities by calculating the static structure factor S(q) using simulation data. In the density and temperature range where the pasta phase appears, the static structure factor shows irregular behavior. The presence of a slab phase greatly enhances the peak in S(q). However, the effect of irregularities in S(q) on the transport coefficients is not very dramatic. The values of all three transport coefficients are found to have the same orders of magnitude as found in theoretical calculations for the inner crust matter of neutron stars without the pasta phase and therefore, is in contrast to earlier speculations that a pasta layer might be highly resistive, both thermally and electrically.

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Assessment of some factors influencing tool wear on the machining of glass fibre-reinforced plastics by coated cemented carbide tools

Cited by 93 publications

References 22 publications

A Common Origin of Magnetism from Planets to White Dwarfs

A Common Origin of Magnetism from Planets to White Dwarfs

Asteroseismic Signatures of Evolving Internal Stellar Magnetic Fields

Transport Properties of the Nuclear Pasta Phase with Quantum Molecular Dynamics

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