Schwarzschild

European Southern Observatory Karl-Schwarzschild str. 2 D-85748 Garching bei Munchenl pdierick eso.org... 

The first clue to the processes which normally regulate TH activity came from experiments showing that electrical stimulation of sympathetic neurons increased the affinity of this enzyme for its co-factor and reduced its affinity for noradrenaline (for detailed reviews of this topic see Zigmond, Schwarzschild and Rittenhouse 1989 Fillenz 1993 Kaufman 1995 Kumar and Vrana 1996). Several lines of investigation showed that activation of TH was in fact paralleled by its phosphorylation and it was this process that accounted for the changes in the enzyme s kinetics (Table 8.2). 

Starke, K (1987) Presynaptic a-autoreceptors. Rev. Physiol. Biochem. Pharmacol. 107 73-146. Zhong, H and Minneman, KP (1999) i-Adrenoceptor subtypes Eur. J. Pharmacol. 375 261-276. Zigmond, RE, Schwarzschild, MA and Rittenhouse, AR (1989) Acute regulation of tyrosine hydroxylase by nerve activity and by neurotransmitters via phosphorylation. Ann. Rev. Neurosci. 12 451-461. 

European Southern Observatory, Karl-Schwarzschild-Strasse 2,... 

Max-Planck-Institut fur Astrophysik, Karl-Schwarzschild-Str. 1, Garching, Germany... 

European Southern Observatory Karl-Schwarzschild-Str. 2 85748 Garching Germany... 

A gravitationally massive object (allegedly) from which fight cannot escape. The Schwarzschild radius is the radius of the black hole that defines the event horizon the distance at which fight cannot escape... 

Schwarzschild radius The radius of a sphere into which a mass must be confined if it is to be a black hole. 

The reversing-layer picture is sometimes referred to as the Schuster-Schwarzschild model , but Arthur Schuster and Karl Schwarzschild considered more sophisticated models of radiative transfer (including scattering) than the one used here. 

At sufficiently high densities (e.g. cores of upper main-sequence stars), the > sign virtually becomes an equality (adiabatic stratification), but at lower densities (e.g. envelopes of the Sun and cooler stars) an exact calculation is very difficult and in most models a crude approximation based on mixing-length theory is used. In a situation where the chemical composition changes with depth, Eq. (5.24) (known as the Schwarzschild criterion) needs to be replaced by more complicated considerations. 

A. S. Eddington develops theory of radiative equilibrium (building on earlier work by A. Schuster and K. Schwarzschild) and applies it to internal constitution of stars. He also pioneers physics of interstellar gas. 

M. Schwarzschild, A. Sandage and others pioneer theory of stellar evolution without extensive mixing and apply it to HR diagrams of globular clusters getting ages of several Gyr, comparable to the new inverse Hubble constant. 

The relation of the radius and the expected strength of the magnetic field is listed by the use of the hypothesis in Table. 1. Then, it looks to work well for explaining the strength of the magnetic field observed for radio pulsars. However, it does not work for magnetars considering the Schwarzschild radius,... 

Table 1. Here are summarized the used models. The letter (A-E) indicates the mass and number part indicates the 1-hadronic and 2-hybrid Equations of State (EsoS). Mao denotes the gravitational mass of one NS in isolation, C is the compactness, P the orbital period, few,o the corresponding GW frequency, do the initial orbital separation and Roo the radius of one single isolated NS measured in Schwarzschild coordinates.

Department of Chemistry, University of Alberta, Edmonton, Alta., Canada T6G 2G2 Max-Planck-Institut fiir Astrophysik, Karl-Schwarzschild-Strafle 1,... 

On the basis of studies of the HR diagram in collaboration with Martin Schwarzschild, Hoyle predicted the existence of an excited state of which would serve as a resonance for the reaction 2a Be(a, Whaling... 

Both points disagree with observations The observed main sequence width requires only a moderate core mass increase (cf. Mermilliod and Maeder, 1986), the LBVs exist, and very massive WNE and WC stars are not observed (cf. references in Langer, 1987 Doom, 1987). Evolutionary calculations without overshooting avoid both discrepancies. We conclude that convective overshooting is not very efficient in massive H-burning stars, but that the Schwarzschild-criterion may be a fair approximation in order to determine the size of the convective core. 

The convective core size in very massive H-burning stars may well be approximated by the Schwarzschild criterion. 

Schwarzschild). Table 1 summarizes some data on both models. They are compatible with the findings of Woosley (1988). 

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