transport and influence of angular momentum in collapsing

Giant molecular clouds

2 Apparently the angular momentum is transferred away from the collapsing star " 2 (emphases added) To solve this problem magnetic fields are invoked in the disks of the young stars They are anchored to convection zones and are theoretically used to couple out angular momentum

Numerical Solution of Blood Flow and Mass Transport

The simultaneous effect of flexible wall and multiple stenoses on the flow and mass transfer of blood is investigated through numerical computation and simulations The solution is obtained using the Marker and Cell technique on an axisymmetric model of Newtonian blood flow The results compare favorably with physical observations where the pulsatile boundary condition and double stenoses

Characteristics of the Outer Rainband Stratiform

Idealized numerical simulations are conducted in this study to comparatively investigate the characteristics of the stratiform sector in the outer rainbands of tropical cyclones (TCs) in lower- and upper-layer vertical wind shear (VWS) with moderate magnitude Consistent with the results in previous studies the outer rainband stratiform sector of the TCs simulated in both experiments is

Frontiers

The formation of a protostellar disc is a natural outcome during the star formation process As gas in a molecular cloud core collapses under self-gravity the angular momentum of the gas will slow its collapse on small scales and promote the formation of a protostellar disc Although the angular momenta of dense star-forming cores remain to be fully characterized observationally existing

Astronomy Final Exam Practice Flashcards

c the laws of conservation of energy and conversation of angular momentum ensure that any rotating collapsing cloud will end up as a spinning disk d the sun formed first and as it grew in size it spread into a disk rather like the way a ball of dough can be flattened into a pizza by spinning it

Explosion Mechanisms of Core

2019-7-17Nevertheless angular momentum transferred to the PNS by hydrodynamical flows during the development of the explosion and in the postexplosion accretion phase is unlikely to be sufficient to account for the estimated NS birth spin periods of order ∼10 ms which seems to require rotation of the collapsing stellar core (36 250) Explaining a

Heger Langer Woosley Presupernova Evolution of

Angular Momentum Transport Following Endal Sofia (1978) and Pinsonneault et al (1989) we formulate the transport of angular momentum as a diffusive process (Endal Sofia 1978) where is the turbulent viscosity and i the specific angular momentum of a shell at mass coordinate m

Formation of Disc Galaxies

In previous SPH simulations strong outward transport of angular momentum has led to the formation of disc-like systems with much smaller angular momenta than observed in real disc galaxies Here we investigate whether this problem can be circumvented if feedback processes prevent disc

Giant molecular clouds

2 Apparently the angular momentum is transferred away from the collapsing star " 2 (emphases added) To solve this problem magnetic fields are invoked in the disks of the young stars They are anchored to convection zones and are theoretically used to couple out angular momentum

JabRef references

2013-11-29Abstract: As a rapidly rotating neutron star spins down due to the loss of its angular momentum its central density increases and the nuclear matter in its core converts to quark matter which leads to a drastic decrease of the stellar moment of inertia and even results in an era of spin-up of the pulsar (Glendenning Pei amp Weber 1997) We

Modeling and simulation of pore‐scale multiphase

1 INTRODUCTION [2] Fluids play a critical role in a wide range of geological processes For example hydration and dehydration processes are common and they are often coupled with fracturing and fluid flow [Jamtveit et al 2000 Strating and Vissers 1991] Because diffusion coefficients are usually small and the time required for diffusive transport through a distance of l is proportional

[1301 3004] The influence of turbulence during

2013-1-14Abstract: [Abridged] Theoretical and numerical studies of star formation have shown that magnetic field (B) has a strong influence on both disk formation and fragmentation even a relatively low B can prevent these processes However very few studies investigated the combined effects of B and turbulence We study the effects of turbulence in magnetized core collapse focusing on the magnetic

Gravitational Waves from Gravitational Collapse

2011-1-20Gravitational-wave emission from stellar collapse has been studied for nearly four decades Current state-of-the-art numerical investigations of collapse include those that use progenitors with more realistic angular momentum profiles properly treat microphysics issues account for general relativity and examine non-axisymmetric effects in three dimensions

Gravitational Waves from Gravitational Collapse

2003-3-10Gravitational wave emission from stellar collapse has been studied for more than three decades Current state-of-the-art numerical investigations of collapse include those that use progenitors with more realistic angular momentum profiles properly treat microphysics issues account for general relativity and examine non-axisymmetric effects in three dimensions

Journal of Fluid Mechanics

Journal of Fluid Mechanics - Professor M G Worster Journal of Fluid Mechanics is the leading international journal in the field and is essential reading for all those concerned with developments in fluid mechanics It publishes authoritative articles covering theoretical computational and experimental investigations of all aspects of the mechanics of fluids

Influence of angular momentum on transport

In the present work the influence of intrinsic angular momentum on transport coefficients in a single-component gas flow is studied on the basis of the generalized Chapman–Enskog method A self-consistent set of flow equations is derived both for an inviscid and viscous flow approximations

Fragmentation and the initial mass function

2018-11-28star clearly this depends on how effectively angular momentum can be transported outward in or removed from the disk The mechanisms that might transfer angular momentum in protostellar disks have been reviewed by Larson (1989) If the mass

[1301 3004] The influence of turbulence during

2013-1-14Abstract: [Abridged] Theoretical and numerical studies of star formation have shown that magnetic field (B) has a strong influence on both disk formation and fragmentation even a relatively low B can prevent these processes However very few studies investigated the combined effects of B and turbulence We study the effects of turbulence in magnetized core collapse focusing on the magnetic

The impact of magnetic fields on single and binary star

2011-6-24Second if a protostellar disc is gravitationally unstable (but not so strongly as to fragment) spiral density waves are likely to be the dominant angular momentum transport mechanism within the accretion disc (Lodato Rice 2004 2005 Fromang et al 2004)

Incidence of stellar rotation on the explosion mechanism

2018-11-27Angular momentum budget: from progenitor rotation to pulsar spin 2 3 Large uncertainties on angular momentum transport processes Hydrodynamical instabilities in collapsing cores Dynamical influence of rotation on one-armed instabilities

Journal of Fluid Mechanics

Journal of Fluid Mechanics - Professor M G Worster Journal of Fluid Mechanics is the leading international journal in the field and is essential reading for all those concerned with developments in fluid mechanics It publishes authoritative articles covering theoretical computational and experimental investigations of all aspects of the mechanics of fluids

Characteristics of the Outer Rainband Stratiform

Idealized numerical simulations are conducted in this study to comparatively investigate the characteristics of the stratiform sector in the outer rainbands of tropical cyclones (TCs) in lower- and upper-layer vertical wind shear (VWS) with moderate magnitude Consistent with the results in previous studies the outer rainband stratiform sector of the TCs simulated in both experiments is

JabRef references

2013-11-29Abstract: As a rapidly rotating neutron star spins down due to the loss of its angular momentum its central density increases and the nuclear matter in its core converts to quark matter which leads to a drastic decrease of the stellar moment of inertia and even results in an era of spin-up of the pulsar (Glendenning Pei amp Weber 1997) We