3,396 research outputs found
cAMP-Inhibits Cytoplasmic Phospholipase A(2) and Protects Neurons against Amyloid-beta-Induced Synapse Damage
A key event in Alzheimer’s disease (AD) is the production of amyloid-β (Aβ) peptides and the loss of synapses. In cultured neurons Aβ triggered synapse damage as measured by the loss of synaptic proteins. α-synuclein (αSN), aggregates of which accumulate in Parkinson’s disease, also caused synapse damage. Synapse damage was associated with activation of cytoplasmic phospholipase A2 (cPLA2), an enzyme that regulates synapse function and structure, and the production of prostaglandin (PG) E2. In synaptosomes PGE2 increased concentrations of cyclic adenosine monophosphate (cAMP) which suppressed the activation of cPLA2 demonstrating an inhibitory feedback system. Thus, Aβ/αSN-induced activated cPLA2 produces PGE2 which increases cAMP which in turn suppresses cPLA2 and, hence, its own production. Neurons pre-treated with pentoxifylline and caffeine (broad spectrum phosphodiesterase (PDE) inhibitors) or the PDE4 specific inhibitor rolipram significantly increased the Aβ/αSN-induced increase in cAMP and consequently protected neurons against synapse damage. The addition of cAMP analogues also inhibited cPLA2 and protected neurons against synapse damage. These results suggest that drugs that inhibit Aβ-induced activation of cPLA2 and cross the blood–brain barrier may reduce synapse damage in AD
Collapse of a Molecular Cloud Core to Stellar Densities: The First Three-Dimensional Calculations
We present results from the first three-dimensional calculations ever to
follow the collapse of a molecular cloud core (~ 10^{-18} g cm^{-3}) to stellar
densities (> 0.01 g cm^{-3}). The calculations resolve structures over 7 orders
of magnitude in spatial extent (~ 5000 AU - 0.1 R_\odot), and over 17 orders of
magnitude in density contrast. With these calculations, we consider whether
fragmentation to form a close binary stellar system can occur during the second
collapse phase. We find that, if the quasistatic core that forms before the
second collapse phase is dynamically unstable to the growth of non-axisymmetric
perturbations, the angular momentum extracted from the central regions of the
core, via gravitational torques, is sufficient to prevent fragmentation and the
formation of a close binary during the subsequent second collapse.Comment: ApJ Letters, in press (will appear in Nov 20 issue; available from
the ApJ Rapid Release web page). 7 pages, incl. 5 figures. Also available at
http://www.mpia-hd.mpg.de/theory/bat
The formation of close binary systems
A viable solution to the origin of close binary systems, unaccounted for in
recent theories, is presented. Fragmentation, occurring at the end of the
secondary collapse phase (during which molecular hydrogen is dissociating), can
form binary systems with separations less than 1 au. Two fragmentation modes
are found to occur after the collapse is halted. The first consists of the
fragmentation of a protostellar disc due to rotational instabilities in a
protostellar core, involving both an and an mode. This
fragmentation mechanism is found to be insensitive to the initial density
distribution: it can occur in both centrally condensed and uniform initial
conditions. The second fragmentation mode involves the formation of a rapidly
rotating core at the end of the collapse phase which is unstable to the
axisymmetric perturbations. This core bounces into a ring which quickly
fragments into several components. The binary systems thus formed contain less
than 1 per cent of a solar mass and therefore will need to accrete most of
their final mass if they are to form a binary star system. Their orbital
properties will thus be determined by the properties of the accreted matter.Comment: 6 pages, uuencoded compressed postscript file (containing 2 figures
The Origin of the Initial Mass Function and Its Dependence on the Mean Jeans Mass in Molecular Clouds
We investigate the dependence of stellar properties on the mean thermal Jeans
mass in molecular clouds. We compare the results from the two largest
hydrodynamical simulations of star formation to resolve the fragmentation
process down to the opacity limit, the first of which was reported by Bate,
Bonnell & Bromm. The initial conditions of the two calculations are identical
except for the radii of the clouds, which are chosen so that the mean densities
and mean thermal Jeans masses of the clouds differ by factors of nine and
three, respectively. We find that the denser cloud, with the lower mean thermal
Jeans mass, produces a higher proportion of brown dwarfs and has a lower
characteristic (median) mass of the stars and brown dwarfs. This dependence of
the initial mass function (IMF) on the density of the cloud may explain the
observation that the Taurus star-forming region appears to be deficient in
brown dwarfs when compared with the Orion Trapezium cluster. The new
calculation also produces wide binaries (separations >20 AU), one of which is a
wide binary brown dwarf system. Based on the hydrodynamical calculations, we
develop a simple accretion/ejection model for the origin of the IMF. In the
model, all stars and brown dwarfs begin with the same mass (set by the opacity
limit for fragmentation) and grow in mass until their accretion is terminated
stochastically by their ejection from the cloud through dynamically
interactions. The model predicts that the main variation of the IMF in
different star-forming environments should be in the location of the peak (due
to variations in the mean thermal Jeans mass of the cloud) and in the
substellar regime. However, the slope of the IMF at high-masses may depend on
the dispersion in the accretion rates of protostars.Comment: 22 pages, 14 figures, accepted for publication in MNRAS. Paper with
high-resolution figures and animations available from
http://www.astro.ex.ac.uk/people/mbate/ Replacement removes inconsistent
definitions of base 10 logarithm
Glycosylphosphatidylinositols: More than just an anchor?
There is increasing interest in the role of glycosylphosphatidylinositol (GPI) anchors that attach some proteins to cell membranes. Far from being biologically inert, GPIs influence the targeting, intracellular trafficking and function of the attached protein. Our recent paper demonstrated the role of sialic acid on the GPI of the cellular prion protein (PrPC). The “prion diseases” arise following the conversion of PrPC to a disease-associated isoform called PrPSc or “prion”. Our paper showed that desialylated PrPC inhibited PrPSc formation. Aggregated PrPSc creates a signaling platform in the cell membrane incorporating and activating cytoplasmic phospholipase A2 (cPLA2), an enzyme that regulates PrPC trafficking and hence PrPSc formation. The presence of desialylated PrPC caused the dissociation of cPLA2 from PrP-containing platforms, reduced the activation of cPLA2 and inhibited PrPSc production. We concluded that sialic acid contained within the GPI attached to PrPC modifies local membrane microenvironments that are important in PrP-mediated cell signaling and PrPSc formation
The effect of magnetic fields on star cluster formation
We examine the effect of magnetic fields on star cluster formation by
performing simulations following the self-gravitating collapse of a turbulent
molecular cloud to form stars in ideal MHD. The collapse of the cloud is
computed for global mass-to-flux ratios of infinity, 20, 10, 5 and 3, that is
using both weak and strong magnetic fields. Whilst even at very low strengths
the magnetic field is able to significantly influence the star formation
process, for magnetic fields with plasma beta < 1 the results are substantially
different to the hydrodynamic case. In these cases we find large-scale
magnetically-supported voids imprinted in the cloud structure; anisotropic
turbulent motions and column density structure aligned with the magnetic field
lines, both of which have recently been observed in the Taurus molecular cloud.
We also find strongly suppressed accretion in the magnetised runs, leading to
up to a 75% reduction in the amount of mass converted into stars over the
course of the calculations and a more quiescent mode of star formation. There
is also some indication that the relative formation efficiency of brown dwarfs
is lower in the strongly magnetised runs due to the reduction in the importance
of protostellar ejections.Comment: 16 pages, 9 figures, 8 very pretty movies, MNRAS, accepted. Version
with high-res figures + movies available from
http://www.astro.ex.ac.uk/people/dprice/pubs/mcluster/index.htm
The Formation Mechanism of Brown Dwarfs
We present results from the first hydrodynamical star formation calculation
to demonstrate that brown dwarfs are a natural and frequent product of the
collapse and fragmentation of a turbulent molecular cloud. The brown dwarfs
form via the fragmentation of dense molecular gas in unstable multiple systems
and are ejected from the dense gas before they have been able to accrete to
stellar masses. Thus, they can be viewed as `failed stars'. Approximately three
quarters of the brown dwarfs form in gravitationally-unstable circumstellar
discs while the remainder form in collapsing filaments of molecular gas. These
formation mechanisms are very efficient, producing roughly the same number of
brown dwarfs as stars, in agreement with recent observations. However, because
close dynamical interactions are involved in their formation, we find a very
low frequency of binary brown dwarf systems (\lsim 5%) and that those binary
brown dwarf systems that do exist must be close \lsim 10 AU. Similarly, we
find that young brown dwarfs with large circumstellar discs (radii \gsim 10
AU) are rare (%).Comment: 5 pages, 2 GIF figures, postscript with figures available at
http://www.astro.ex.ac.uk/people/mbat
The Formation of Close Binary Systems by Dynamical Interactions and Orbital Decay
We present results from the first hydrodynamical star formation calculation
to demonstrate that close binary stellar systems (separations \lsim 10 AU)
need not be formed directly by fragmentation. Instead, a high frequency of
close binaries can be produced through a combination of dynamical interactions
in unstable multiple systems and the orbital decay of initially wider binaries.
Orbital decay may occur due to gas accretion and/or the interaction of a binary
with its circumbinary disc. These three mechanisms avoid the problems
associated with the fragmentation of optically-thick gas to form close systems
directly. They also result in a preference for close binaries to have roughly
equal-mass components because dynamical exchange interactions and the accretion
of gas with high specific angular momentum drive mass ratios towards unity.
Furthermore, due to the importance of dynamical interactions, we find that
stars with greater masses ought to have a higher frequency of close companions,
and that many close binaries ought to have wide companions. These properties
are in good agreement with the results of observational surveys.Comment: Published in MNRAS, 10 pages, 6 figures (5 degraded). Paper with
high-resolution figures and animations available from
http://www.astro.ex.ac.uk/people/mbat
Modelling circumstellar discs with 3D radiation hydrodynamics
We present results from combining a grid-based radiative transfer code with a
Smoothed Particle Hydrodynamics code to produce a flexible system for modelling
radiation hydrodynamics. We use a benchmark model of a circumstellar disc to
determine a robust method for constructing a gridded density distribution from
SPH particles. The benchmark disc is then used to determine the accuracy of the
radiative transfer results. We find that the SED and the temperature
distribution within the disc are sensitive to the representation of the disc
inner edge, which depends critically on both the grid and SPH resolution. The
code is then used to model a circumstellar disc around a T-Tauri star. As the
disc adjusts towards equilibrium vertical motions in the disc are induced
resulting in scale height enhancements which intercept radiation from the
central star. Vertical transport of radiation enables these perturbations to
influence the mid-plane temperature of the disc. The vertical motions decay
over time and the disc ultimately reaches a state of simultaneous hydrostatic
and radiative equilibrium.Comment: MNRAS accepted; 15 pages; 17 figures, 4 in colou
The hierarchical formation of a stellar cluster
Recent surveys of star forming regions have shown that most stars, and
probably all massive stars, are born in dense stellar clusters. The mechanism
by which a molecular cloud fragments to form several hundred to thousands of
individual stars has remained elusive. Here, we use a numerical simulation to
follow the fragmentation of a turbulent molecular cloud and the subsequent
formation and early evolution of a stellar cluster containing more than 400
stars. We show that the stellar cluster forms through the hierarchical
fragmentation of a turbulent molecular cloud. This leads to the formation of
many small subclusters which interact and merge to form the final stellar
cluster. The hierarchical nature of the cluster formation has serious
implications in terms of the properties of the new-born stars. The higher
number-density of stars in subclusters, compared to a more uniform distribution
arising from a monolithic formation, results in closer and more frequent
dynamical interactions. Such close interactions can truncate circumstellar
discs, harden existing binaries, and potentially liberate a population of
planets. We estimate that at least one-third of all stars, and most massive
stars, suffer such disruptive interactions.Comment: 6 pages, 4 figures, accepted for publication in MNRAS. Version
including hi-res colour postscript figure available at
http://star-www.st-and.ac.uk/~sgv/ps/clufhier.ps.g
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