Flocculants

Burkert, H.; Hartmann, Jürgen

doi:10.1002/14356007.a11_251

Cited by 6 publications

(6 citation statements)

References 44 publications

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“…FT-IR spectra were recorded on a Nicolet Impact 400 spectrometer using KBr pellets. 1 H and 13 C NMR spectra were acquired on a Bruker AMX spectrometer in D 2 O. The viscosity of the samples was measured by means of a rotational rheometer RS 150 (Haake, Germany) at 25 l 0.1 8C using the DG 41 Ti measuring container.…”

Section: Measurementsmentioning

confidence: 99%

“…Only soluble starch derivatives have been able to maintain their market position in certain fields. [1,2] At present, most of the commercially available starch derivatives have a low degree of substitution (DS a 0.2). [3 -5] In this context our interest was focused on the preparation of starch derivatives with high DS values and controlled distribution of the functional groups.…”

Section: Introductionmentioning

confidence: 99%

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Starch Derivatives of High Degree of Functionalization, 8. Synthesis and Flocculation Behavior of Cationic Starch Polyelectrolytes

Haack

Heinze²,

Oelmeyer

et al. 2002

Macromol. Mater. Eng.

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Section: Measurementsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Starch Derivatives of High Degree of Functionalization, 8. Synthesis and Flocculation Behavior of Cationic Starch Polyelectrolytes

Haack

Heinze²,

Oelmeyer

et al. 2002

Macromol. Mater. Eng.

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“…Major merger simulations (Mihos and Hernquist 1996) demonstrate that the gas rapidly settles, on a short dynamical time-scale, into a central, self-gravitating disk. By that time, the progenitor black holes will also have merged in the centre by dynamical friction (Burkert & Sunyaev 2000). The inner disk has Keplerian rotation as the gravitational potential is dominated by the mass of the black halo.…”

Section: A Model Of Self-regulated Black Hole Growthmentioning

confidence: 99%

Star Formation–Regulated Growth of Black Holes in Protogalactic Spheroids

Burkert

Silk

2001

The Astrophysical Journal

102

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The observed relation between central black hole mass and spheroid velocity dispersion is interpreted in terms of a self-regulation model that incorporates a viscous Keplerian accretion disk to feed the black hole, embedded in a massive, self-gravitating star forming disk that eventually populates the spheroid. The model leads to a constant ratio between black hole mass and spheroid mass which is equal to the inverse of the critical Reynolds number for the onset of turbulence in the accretion disk surrounding the central black hole. Applying the fundamental plane correlation for spheroids, we find that the black hole mass has a power-law dependence on the spheroid velocity dispersion with a slope in the range of 4-5. We explain the larger scatter in the Magorrian relation with respect to the black hole mass-spheroid velocity dispersion relationship as a result of secular evolution of the spheroid that primarily affects its luminosity and to a much lesser extent its velocity dispersion.

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“…They suggest that this fundamental relation holds over a span of mass covering nearly nine orders of magnitude. Although the exact physical meaning of certain density threshold values is not clear (see discussion in Burkert & Hartmann 2012), this empirical relation provides an interesting opportunity to compare different star formation regions. In the compilation of observational data of Lada et al (2012), there is a gap of about four orders of magnitude (in cloud mass) between the local Galactic clouds and the external galaxies.…”

Section: Total Fir Luminositymentioning

confidence: 99%

Herschel far-infrared observations of the Carina Nebula Complex. - III: Detailed cloud structure and feedback effects

Roccatagliata,

Preibisch,

Ratzka

et al. 2013

Preprint

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Context. The star formation process in large clusters/associations can be strongly influenced by the feedback from high mass stars. Whether the resulting net effect of the feedback is predominantly negative (cloud dispersal) or positive (triggering of star formation due to cloud compression) is still an open question. Aims. The Carina Nebula complex (CNC) represents one of the most massive star-forming regions in our Galaxy. We use our Herschel far-infrared observations to study the properties of the clouds over the entire area of the CNC (with a diameter of ≈ 3.2 • , which corresponds to ≈ 125 pc at the distance of 2.3 kpc). The good angular resolution (10 ′′ − 36 ′′ ) of the Herschel maps corresponds to physical scales of 0.1 -0.4 pc, and allows us to analyze the small-scale (i.e. clump-size) structures of the clouds. Methods. The full extent of the CNC was mapped with PACS and SPIRE in the 70, 160, 250, 350, and 500 µm bands. We determine temperatures and column densities at each point in this maps by modeling the observed far-infrared spectral energy distributions. We also derive a map showing the strength of the UV radiation field. We investigate the relation between the cloud properties and the spatial distribution of the high-mass stars, and compute total cloud masses for different density thresholds. Results. Our Herschel maps resolve, for the first time, the small-scale structure of the dense clouds over the entire spatial extent of the CNC. Several particularly interesting regions, including the prominent pillars south of η Car, are analyzed in detail. We compare the cloud masses derived from the Herschel data to previous mass estimates based on sub-mm and molecular line data. Our maps also reveal a peculiar "wave"-like pattern in the northern part of the Carina Nebula. Finally, we characterize two prominent cloud complexes at the periphery of our Herschel maps, which are probably molecular clouds in the Galactic background. Conclusions. We find that the density and temperature structure of the clouds in most parts of the CNC is dominated by the strong feedback from the numerous massive stars, rather than random turbulence. Comparing the cloud mass and the star formation rate derived for the CNC to other Galactic star forming regions suggests that the CNC is forming stars in an particularly efficient way. We suggest this to be a consequence of triggered star formation by radiative cloud compression.

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Flocculants

Abstract: The article contains sections titled: 1. Introduction 2. Classification of Flocculants … Show more

Cited by 6 publications

References 44 publications

Starch Derivatives of High Degree of Functionalization, 8. Synthesis and Flocculation Behavior of Cationic Starch Polyelectrolytes

Starch Derivatives of High Degree of Functionalization, 8. Synthesis and Flocculation Behavior of Cationic Starch Polyelectrolytes

Star Formation–Regulated Growth of Black Holes in Protogalactic Spheroids

Herschel far-infrared observations of the Carina Nebula Complex. - III: Detailed cloud structure and feedback effects

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