1,994 research outputs found
Magnetic fields and radiative feedback in the star formation process
Star formation is a complex process involving the interplay of many physical
effects, including gravity, turbulent gas dynamics, magnetic fields and
radiation. Our understanding of the process has improved substantially in
recent years, primarily as a result of our increased ability to incorporate the
relevant physics in numerical calculations of the star formation process. In
this contribution we present an overview of our recent studies of star cluster
formation in turbulent, magnetised clouds using self-gravitating
radiation-magnetohydrodynamics calculations (Price and Bate 2008, 2009). Our
incorporation of magnetic fields and radiative transfer into the Smoothed
Particle Hydrodynamics method are discussed. We highlight how magnetic fields
and radiative heating of the gas around newborn stars can solve several of the
key puzzles in star formation, including an explanation for why star formation
is such a slow and inefficient process. However, the presence of magnetic
fields at observed strengths in collapsing protostellar cores also leads to
problems on smaller scales, including a difficulty in forming protostellar
discs and binary stars (Price and Bate 2007, Hennebelle and Teyssier 2008),
which suggests that our understanding of the role of magnetic fields in star
formation is not yet complete.Comment: 14 pages aip conf. format, 5 figures, submitted to AIP conf proc. of
"Plasmas in the Laboratory and in the Universe: Interactions, Patterns and
Turbulence", Como, Italy 1st-4th Dec 2009, eds. Bertin et al. Relevant movies
at http://users.monash.edu.au/~dprice/mclusterRT/index.html#movie
Smoothed particle magnetohydrodynamic simulations of protostellar outflows with misaligned magnetic field and rotation axes
We have developed a modified form of the equations of smoothed particle
magnetohydrodynamics which are stable in the presence of very steep density
gradients. Using this formalism, we have performed simulations of the collapse
of magnetised molecular cloud cores to form protostars and drive outflows. Our
stable formalism allows for smaller sink particles (< 5 AU) than used
previously and the investigation of the effect of varying the angle, {\theta},
between the initial field axis and the rotation axis. The nature of the
outflows depends strongly on this angle: jet-like outflows are not produced at
all when {\theta} > 30{\deg}, and a collimated outflow is not sustained when
{\theta} > 10{\deg}. No substantial outflows of any kind are produced when
{\theta} > 60{\deg}. This may place constraints on the geometry of the magnetic
field in molecular clouds where bipolar outflows are seen.Comment: Accepted for publication in MNRAS, 13 pages, 14 figures. Animations
can be found at
http://www.astro.ex.ac.uk/people/blewis/research/outflows_misaligned_fields.htm
Constrained hyperbolic divergence cleaning in smoothed particle magnetohydrodynamics with variable cleaning speeds
We present an updated constrained hyperbolic/parabolic divergence cleaning
algorithm for smoothed particle magnetohydrodynamics (SPMHD) that remains
conservative with wave cleaning speeds which vary in space and time. This is
accomplished by evolving the quantity instead of . Doing so
allows each particle to carry an individual wave cleaning speed, , that
can evolve in time without needing an explicit prescription for how it should
evolve, preventing circumstances which we demonstrate could lead to runaway
energy growth related to variable wave cleaning speeds. This modification
requires only a minor adjustment to the cleaning equations and is trivial to
adopt in existing codes. Finally, we demonstrate that our constrained
hyperbolic/parabolic divergence cleaning algorithm, run for a large number of
iterations, can reduce the divergence of the field to an arbitrarily small
value, achieving to machine precision.Comment: 23 pages, 16 figures, accepted for publication in Journal of
Computational Physic
Extending the Latent Multinomial Model with Complex Error Processes and Dynamic Markov Bases
The latent multinomial model (LMM) model of Link et al. (2010) provided a
general framework for modelling mark-recapture data with potential errors in
identification. Key to this approach was a Markov chain Monte Carlo (MCMC)
scheme for sampling possible configurations of the counts true capture
histories that could have generated the observed data. This MCMC algorithm used
vectors from a basis for the kernel of the linear map between the true and
observed counts to move between the possible configurations of the true data.
Schofield and Bonner (2015) showed that a strict basis was sufficient for some
models of the errors, including the model presented by Link et al. (2010), but
a larger set called a Markov basis may be required for more complex models. We
address two further challenges with this approach: 1) that models with more
complex error mechanisms do not fit easily within the LMM and 2) that the
Markov basis can be difficult or impossible to compute for even moderate sized
studies. We address these issues by extending the LMM to separately model the
capture/demographic process and the error process and by developing a new MCMC
sampling scheme using dynamic Markov bases. Our work is motivated by a study of
Queen snakes (Regina septemvittata) in Kentucky, USA, and we use simulation to
compare the use of PIT tags, with perfect identification, and brands, which are
prone to error, when estimating survival rates
Investigating prescriptions for artificial resistivity in smoothed particle magnetohydrodynamics
In numerical simulations, artificial terms are applied to the evolution
equations for stability. To prove their validity, these terms are thoroughly
tested in test problems where the results are well known. However, they are
seldom tested in production-quality simulations at high resolution where they
interact with a plethora of physical and numerical algorithms. We test three
artificial resistivities in both the Orszag-Tang vortex and in a star formation
simulation. From the Orszag-Tang vortex, the Price et. al. (2017) artificial
resistivity is the least dissipative thus captures the density and magnetic
features; in the star formation algorithm, each artificial resistivity
algorithm interacts differently with the sink particle to produce various
results, including gas bubbles, dense discs, and migrating sink particles. The
star formation simulations suggest that it is important to rely upon physical
resistivity rather than artificial resistivity for convergence.Comment: 8 pages, 7 figures. Proceedings of the "12th international SPHERIC
workshop", Ourense, Spain, 13-15 June 201
The impact of magnetic fields on single and binary star formation
We have performed magnetohydrodynamic (MHD) simulations of the collapse and
fragmentation of molecular cloud cores using a new algorithm for MHD within the
smoothed particle hydrodynamics (SPH) method, that enforces the zero magnetic
divergence constraint. We find that the support provided by magnetic fields
over thermal pressure alone has several important effects on fragmentation and
the formation of binary and multiple systems, and on the properties of massive
circumstellar discs. The extra support suppresses the tendency of molecular
cloud cores to fragment due to either initial density perturbations or disc
fragmentation. Furthermore, unlike most previous studies, we find that magnetic
pressure plays the dominant role in inhibiting fragmentation rather than
magnetic tension or magnetic braking. In particular, we find that if the
magnetic field is aligned with the rotation axis of the molecular cloud core,
the effects of the magnetic field on fragmentation and disc structure are
almost entirely due to magnetic pressure, while if the rotation axis is
initially perpendicular to the magnetic field, magnetic tension plays a greater
role and can actually aid fragmentation. Despite these effects, and contrary to
several past studies, we find that strongly-perturbed molecular cloud cores are
able to fragment to form wide binary systems even in the presence of quite
strong magnetic fields. For massive circumstellar discs, we find that slowing
of the collapse caused by the magnetic support decreases the mass infall rate
on to the disc and, thus, weakens gravitational instabilities in young massive
circumstellar discs. This not only reduces the likelihood that they will
fragment, but also decreases the importance of spiral density waves in
providing angular momentum transport and in promoting planet formation.Comment: 15 pages, 12 figures, accepted for publication in MNRAS. Images
degraded to fit size requirements. High res version and pretty movies for
this paper can be found at
http://www.astro.ex.ac.uk/people/dprice/pubs/magsf/index1.htm
Can non-ideal magnetohydrodynamics solve the magnetic braking catastrophe? (dataset)
This is all the data created for Wurster, Price & Bate (2016). This dataset was created using the SPHMD code Phantom and included a precursor to the NICIL library (Wurster 2016) to calculate the non-ideal MHD coefficients. The data and important files have been uploaded; the data files can be read with either Phantom, or with the graphics programme Splash. The filenames represent the original path and the simulation, and have the prefix WPB2016_pdata_. The second component to the filename is 1e6 (models with 1e6 particles in the sphere) or 3e5 (models with 1e6 particles in the sphere) and the third component is the simulation name. Typically, the model name has the form ABC, where A=ii,ni,nim for ideal, non-ideal with Bz, non-ideal with -Bz, respectively; B=o,h,a,oha for ohmic,hall,ambipolar,ohmic+hall+ambipolar, respectively; C=B,Q,C,D,P mu0=10,7.5,5,5,hydro, respectively. Ideal runs do not have a B part to the name.We investigate whether or not the low ionization fractions in molecular cloud cores can solve the ‘magnetic braking catastrophe’, where magnetic fields prevent the formation of circumstellar discs around young stars. We perform three-dimensional smoothed particle non- ideal magnetohydrodynamics (MHD) simulations of the gravitational collapse of one solar mass molecular cloud cores, incorporating the effects of ambipolar diffusion, Ohmic resistivity and the Hall effect alongside a self-consistent calculation of the ionization chemistry assuming 0.1 μm grains. When including only ambipolar diffusion or Ohmic resistivity, discs do not form in the presence of strong magnetic fields, similar to the cases using ideal MHD. With the Hall effect included, disc formation depends on the direction of the magnetic field with respect to the rotation vector of the gas cloud. When the vectors are aligned, strong magnetic braking occurs and no disc is formed. When the vectors are anti-aligned, a disc with radius of 13 au can form even in strong magnetic when all three non-ideal terms are present, and a disc of 38 au can form when only the Hall effect is present; in both cases, a counter-rotating envelope forms around the first hydrostatic core. For weaker, anti-aligned fields, the Hall effect produces massive discs comparable to those produced in the absence of magnetic fields, suggesting that planet formation via gravitational instability may depend on the sign of the magnetic field in the precursor molecular cloud core
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