Blood Coagulation

Fasano, Antonio; Sequeira, Adélia

doi:10.1007/978-3-319-60513-5_2

Cited by 7 publications

(15 citation statements)

References 233 publications

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“…Pasquali et al (2006) confirmed these trends in a sample of 18 elliptical galaxies from the Hubble Space Telescope (HST) Ultra-deep Field (UDF). Wyatt (1953) also found evidence of isophote twisting in elliptical galaxies (see also Fasano & Bonoli 1989;Nieto et al 1992;Lauer et al 2005). These observations are consistent with bright ellipticals being triaxial systems with varying triaxiality as a function of radius, which in projection appears as isophote twisting (e.g., Romanowsky & Kochanek 1998).…”

Section: Physical Effectsmentioning

confidence: 66%

“…Aside from systematics, there are physical reasons why different shape measurements can give different results. Several studies of bright elliptical galaxies have found evidence for ellipticity gradients and isophote twisting with radius (see, e.g., Wyatt 1953;di Tullio 1978di Tullio , 1979Kormendy 1982;Fasano & Bonoli 1989;Nieto et al 1992;Romanowsky & Kochanek 1998;Lauer et al 2005;Pasquali et al 2006). di Tullio (1978, 1979 first found environment-dependence of ellipticity gradients.…”

Section: Physical Effectsmentioning

confidence: 99%

“…Several studies have also detected isophote twists in small samples of elliptical galaxies, whereby the position angle in the measured galaxy shape changes with radius (Wyatt 1953;Abramenko 1978;Kormendy 1982;Fasano & Bonoli 1989;Nieto et al 1992;Lauer et al 2005). The isophote twisting may originate from varying triaxiality of galaxies with radii (see, e.g., Romanowsky & Kochanek 1998) though Kormendy (1982) pointed out that the outer regions of galaxies are more susceptible to tidal fields, which can result in isophote twisting.…”

Section: Introductionmentioning

confidence: 97%

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Intrinsic alignments of BOSS LOWZ galaxies – II. Impact of shape measurement methods

Singh

Mandelbaum

2016

Mon. Not. R. Astron. Soc.

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Measurements of intrinsic alignments of galaxy shapes with the large-scale density field, and the inferred intrinsic alignments model parameters, are sensitive to the shape measurement methods used. In this paper we measure the intrinsic alignments of the Sloan Digital Sky Survey-III (SDSS-III) Baryon Oscillation Spectroscopic Survey (BOSS) LOWZ galaxies using three different shape measurement methods (reGaussianization, isophotal, and de Vaucouleurs), identifying a variation in the inferred intrinsic alignments amplitude at the 40% level between these methods, independent of the galaxy luminosity or other properties. We also carry out a suite of systematics tests on the shapes and their two-point correlation functions, identifying a pronounced contribution from additive PSF systematics in the de Vaucouleurs shapes. Since different methods measure galaxy shapes at different effective radii, the trends we identify in the intrinsic alignments amplitude are consistent with the interpretation that the outer regions of galaxy shapes are more responsive to tidal fields, resulting in isophote twisting and stronger alignments for isophotal shapes. We observe environment dependence of ellipticity, with brightest galaxies in groups being rounder on average compared to satellite and field galaxies. We also study the anisotropy in intrinsic alignments measurements introduced by projected shapes, finding effects consistent with predictions of the nonlinear alignment model and hydrodynamic simulations. The large variations seen using the different shape measurement methods have important implications for intrinsic alignments forecasting and mitigation with future surveys.

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Section: Physical Effectsmentioning

confidence: 66%

Section: Physical Effectsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

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Intrinsic alignments of BOSS LOWZ galaxies – II. Impact of shape measurement methods

Singh

Mandelbaum

2016

Mon. Not. R. Astron. Soc.

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“…The first term in the solution (34) after accounting for Equations (40) and (41) coincides with the quasi-steady-state solutions (46) and (47), respectively, whereas the second term in (34) describes the transient process.…”

Section: Analysis Of the Quasi-steady-state Oscillationsmentioning

confidence: 96%

“…Periodic solutions of the bioheat equation were investigated in [38]. The harmonic point source in the bioheat equation was used in therapeutic hypotermia [39,40]; applications of the time-harmonic impact in ultrasound surgery were studied in [41].…”

Section: Introductionmentioning

confidence: 99%

Time-Fractional Diffusion-Wave Equation with Mass Absorption in a Sphere under Harmonic Impact

2019

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The time-fractional diffusion equation with mass absorption in a sphere is considered under harmonic impact on the surface of a sphere. The Caputo time-fractional derivative is used. The Laplace transform with respect to time and the finite sin-Fourier transform with respect to the spatial coordinate are employed. A graphical representation of the obtained analytical solution for different sets of the parameters including the order of fractional derivative is given.

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Hemorheology: Non-Newtonian Constitutive Models for Blood Flow Simulations

Sequeira¹

2018

Lecture Notes in Mathematics

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Blood Coagulation

Cited by 7 publications

References 233 publications

Intrinsic alignments of BOSS LOWZ galaxies – II. Impact of shape measurement methods

Intrinsic alignments of BOSS LOWZ galaxies – II. Impact of shape measurement methods

Time-Fractional Diffusion-Wave Equation with Mass Absorption in a Sphere under Harmonic Impact

Hemorheology: Non-Newtonian Constitutive Models for Blood Flow Simulations

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