Development of cube-textured Ni–W alloy substrates for YBCO-coated conductor

Kim, Kyu Tae; Lim, Jun Hyung; Kim, Jung Ho; Joo, Jinho; Nah, Wansoo; Ji, Bong Ki; Jun, Byung‐Hyuk; Kim, Chan-Joong; Hong, Gye-Won

doi:10.1016/j.physc.2004.02.204

Cited by 26 publications

(23 citation statements)

References 4 publications

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“…The ineffectiveness of radiation pressure as a dispersive feedback mechanism is in agreement with the analytical model of Fall et al (2010), who showed that a 10 4 M cloud requires at least ten times greater surface density than the cloud we model here for radiation pressure to become dominant. In their numerical models, Kim et al (2018) found that surface density was the important parameter in determining the feedback efficiency; photoionization dominated over radiation pressure for similar initial conditions to ours, and in general the latter only became relevant once the surface density exceeded a few times that of our cloud. Skinner & Ostriker (2015) showed that the radiation pressure from dustprocessed infrared photons was ineffective even in high-mass, high-density conditions (M > 10 5 M , Σ > 0.3 g cm −2 ), except for dust opacities corresponding to metallicities higher than found in Galactic GMCs (e.g.…”

Section: Dispersalsupporting

confidence: 55%

“…Parameter studies by Dale & Bonnell (2011) and Dale et al (2012Dale et al ( , 2013 found that the degree of dispersal was closely coupled to the initial conditions of their simulations, such as cloud mass (see also Howard et al 2017). Dispersal has also been shown to depend on initial gas surface density (Kim et al 2018), morphology (Geen et al 2018), and cluster luminosity (Geen et al 2016(Geen et al , 2018. One problem is that even the most recent models simplify the radiative transfer, for example by using the on-the-spot approximation for recombination (thus neglecting the ionizing photons re-emitted by the gas), by using simple two-step temperature schemes for neutral and ionized hydrogen, or by neglecting dust microphysics such as absorption and scattering.…”

Section: Introductionmentioning

confidence: 99%

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Massive star feedback in clusters: variation of the FUV interstellar radiation field in time and space

Ali

Harries

2019

Monthly Notices of the Royal Astronomical Society

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We investigate radiative feedback from a 34 M star in a 10 4 M turbulent cloud using three-dimensional radiation-hydrodynamics (RHD) models. We use Monte Carlo radiative transfer to accurately compute photoionization equilibrium and radiation pressure, with multiple atomic species and silicate dust grains. We include the diffuse radiation field, dust absorption/re-emission, and scattering. The cloud is efficiently dispersed, with 75 per cent of the mass leaving the (32.3 pc) 3 grid within 4.3 Myr (1.1 t ff ). This compares to all mass exiting within 1.6 Myr (0.74 t ff ) in our previously published 10 3 M cloud. At most 20 per cent of the mass is ionized, compared to 40 per cent in the lower mass model, despite the ionized volume fraction being 80 per cent in both, implying the higher mass cloud is more resilient to feedback. The total Jeans-unstable mass increases linearly up to 1500 M before plateauing after 2 Myr, corresponding to a core formation efficiency of 15 per cent. We also measure the time-variation of the far-ultraviolet (FUV) radiation field, G 0 , impinging on other cluster members, taking into account for the first time how this changes in a dynamic cluster environment with intervening opacity sources and stellar motions. Many objects remain shielded in the first 0.5 Myr whilst the massive star is embedded, after which G 0 increases by orders of magnitude. Gas motions later on cause comparable drops which happen instantaneously and last for ∼ 1 Myr before being restored. This highly variable UV field will influence the photoevaporation of protoplanetary discs near massive stars.

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Section: Dispersalsupporting

confidence: 55%

Section: Introductionmentioning

confidence: 99%

Massive star feedback in clusters: variation of the FUV interstellar radiation field in time and space

Ali

Harries

2019

Monthly Notices of the Royal Astronomical Society

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“…The most commonly used substrates for coated conductors prepared by the RABiTS method are pure nickel, or nickel alloyed with 3 at.% tungsten [5] or Ni with 5 at. % tungsten [6][7][8][9].…”

Section: Introductionmentioning

confidence: 99%

Tensile strengths and Young’s modulus of thin copper and copper-nickel (CuNi44) substrates

2008

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Abstract:In this paper we report a method to determine tensile strengths and Young's modulus of cubic biaxial textured metal tapes used as substrate materials for coated conductors (CC). Simplicity, rapidity and reproducibility of the procedure are important for the evaluation of continuous in-house productions. Our approach is based on the EN 10002-1 B tensile test method. A key role for satisfactory results is the sample preparation of 100 -250 µm thick tapes, which will be described in detail.

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“…Studies using other methods, such as cold isostatic pressing or powder metallurgy, also never emphasized this effect in a quantitative manner [8]. Research on alloy ingots made by arc plasma melting [9] have reported that Ni-W substrates had a stronger cube texture than pure Ni substrates; however, they supplied no quantitative measurements of the volume fractions of the cube component. Bhattacharjee et al [6], who used a typical powder metallurgy method to produce these alloys, have shown, quantitatively, the highly beneficial effect of W and Mo addition to Ni in increasing the volume percent of the cube component.…”

Section: Resultsmentioning

confidence: 99%

Enhancement of cube texture in Ni by the addition of W or Mo

Ray

Bhattacharjee

2007

Philosophical Magazine

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The development of cube texture after heavy cold rolling ($95%) and annealing has been studied in pure Ni, Ni-5 at% W and Ni-5 at% Mo alloys. The two Ni alloys develop a much sharper cube texture compared to pure Ni, thus indicating the beneficial effect of W or Mo addition. W and Mo enhance the cube texture intensity in Ni by decreasing the volume fraction of the rotated cube grains. The impact of W and Mo addition is seen from a very early stage of recrystallization, where rotated cube grains form in pure Ni as opposed to sharp cube-oriented grains in the two Ni alloys. The results negate the widely perceived theory of 'detrimental effect of impurities' on the development of cube texture.

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Development of cube-textured Ni–W alloy substrates for YBCO-coated conductor

Cited by 26 publications

References 4 publications

Massive star feedback in clusters: variation of the FUV interstellar radiation field in time and space

Massive star feedback in clusters: variation of the FUV interstellar radiation field in time and space

Tensile strengths and Young’s modulus of thin copper and copper-nickel (CuNi44) substrates

Enhancement of cube texture in Ni by the addition of W or Mo

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