arXiv subjects

M. S. Turner

Publications and source records attributed to M. S. Turner.

At least 19 recordsLinked to original sources

arXiv2026

Log-normal Superstatistics Reveals Statistical Resilience in the Panic Response of Confined Ants

We report the emergence of Log-normal Superstatistics in the collective motion of ants confined in a quasi-2D arena and exposed to a panic-inducing stimulus. A data-driven superstatistical Langevin model accurately reproduces the transition from stationary behavior to an organized escape response, characterized by non-Gaussian velocity distributions and a stochastic diffusion coefficient. Our findings show that danger information propagates via a memory-limited, cascade-like mechanism, resulting in a stable cluster formation despite individual memory constraints. These results indicate that a slowly varying diffusivity arises from the multiplicative combination of interaction-mediated processes under confinement, leading naturally to Log-normal fluctuations. The persistence of this statistical structure under panic reveals a form of collective resilience, establishing a mechanistic bridge between Superstatistics and living active matter in confined environments.

q-bio.PE↗

arXiv2019

Solvated Membrane Nanodiscoids: A Probe For The Effects Of Gaussian Curvature

Several methods now exist to solvate lipid bilayer discoids at the scale of tens of nanometres. Due to their size, such nanodiscoids have a comparatively large boundary-to-area ratio, making them unusually well-suited to probing the effects of Gaussian curvature. Arguing that fluctuations in discoid size and shape are quenched on formation, we quantify the stability, in terms of size and shape, of near-solvation discoid-like flaps that are subject to thermal fluctuations. Using cryo-Electron Microscopy images of Styrene Maleic Acid stabilised discoids, we deduce that stable, saddle-like discoids (with high Gaussian curvature) can likely be solvated from bulk lamellar ($L_α$) phase at moderate-to-high surface tensions ($>10^{-4}$ N/m). We then describe how such tension-controlled solvation can be used for both measuring, and fractionating membrane components according-to, the modulus of Gaussian rigidity $\barκ$. Opportunities for investigating the effects of Gaussian curvature on membrane-embedded proteins, which can be co-solvated during the formation process, are also discussed.

cond-mat.soft↗

arXiv2017

Recycling controls membrane domains

We study the coarsening of strongly microphase separated membrane domains in the presence of recycling of material. We study the dynamics of the domain size distribution under both scale-free and size-dependent recycling. Closed form solutions to the steady state distributions and its associated central moments are obtained in both cases. Moreover, for the size-independent case, the~time evolution of the moments is analytically calculated, which provide us with exact results for their corresponding relaxation times. Since these moments and relaxation times are measurable quantities, the biophysically significant free parameters in our model may be determined by comparison with experimental data.

q-bio.SC↗

arXiv2014

Threading Dynamics of Ring Polymers in a Gel

We perform large scale three-dimensional molecular dynamics simulations of unlinked and unknotted ring polymers diffusing through a background gel, here a three-dimensional cubic lattice. Taking advantage of this architecture, we propose a new method to unambiguously identify and quantify inter-ring threadings (penetrations) and to relate these to the dynamics of the ring polymers. We find that both the number and the persistence time of the threadings increase with the length of the chains, ultimately leading to a percolating network of inter-ring penetrations. We discuss the implications of these findings for the possible emergence of a topological jammed state of very long rings.

cond-mat.soft↗

arXiv2010

Reply to comment on Twisted Protein Aggregates and Disease by Liu and Gunton

We reply to a recent comment [arXiv:1002.2445] and describe why the chemical potential conjugate to the mass of linear aggregates is not an independent parameter in the ensemble that the total length is free to adjust. It is only in the (unphysical) ensemble of fixed total polymer length that such a chemical potential can act as an independent control parameter for the aggregate radius.

cond-mat.soft↗

arXiv2006

Stall, spiculate or runaway - the fate of fibers growing towards fluctuating membranes

We solve the dynamic equations of motion for a growing semi-flexible polymer, or fiber, approaching a fluctuating membrane at an angle. At late times we find three different regimes: fiber {\em stalling}, when fiber growth stops due to membrane resistence, {\em run-away}, in which the polymer bends away from the membrane, and another regime in which the membrane response is nonlinear and tubular membrane {\em spicules} are formed. We discuss which regions of the resulting `phase diagram' are explored by (i) single and bundled actin fibers in living cells, (ii) sickle hemoglobin fibers in red blood cells, and (iii) microtubules growing within artificial vesicles. We complement our analysis with full 3-dimensional stochastic simulations.

cond-mat.soft↗

arXiv2005

Spicules and the effect of rigid rods on enclosing membrane tubes

Membrane tubes (spicules) arise in cells, or artificial membranes, in the nonlinear deformation regime due to, e.g. the growth of microtubules, actin filaments or sickle hemoglobin fibers towards a membrane. We calculate the axial force exerted by the cylindrical membrane tube, and its average radius, by taking into account steric interactions between the fluctuating membrane and the enclosed rod. The force required to confine a fluctuating membrane near the surface of the enclosed rod diverges as the separation approaches zero. This results in a smooth crossover of the axial force between a square root and a linear dependence on the membrane tension as the tension increases and the tube radius shrinks. This crossover can occur at the most physiologically relevant membrane tensions. Our work may be important in (i) interpreting experiments in which axial force is related to the tube radius or membrane tension (ii) dynamical theories for biopolymer growth in narrow tubes where these fluctuation effects control the tube radius.

cond-mat.soft↗

arXiv2003

On the formation of caveolae and similar membrane invaginations

We study a physical model for the formation of bud-like invaginations on fluid membranes under tension, and apply this model to caveolae formation. We demonstrate that budding can be driven by membrane-bound inclusions (proteins) provided that they exert asymmetric forces on the membrane that give rise to bending moments. In particular, Caveolae formation may not necessarily require forces to be applied by the cytoskeleton. Our theoretical model is able to explain several features observed experimentally in caveolae, where proteins in the caveolin family are known to play a crucial role in the formation of caveolae buds. These include (i) the formation of caveolae buds with sizes in the 100nm range (ii) that a fairly large variation of bud shape is expected (iii) that certain N and C termini deletion mutants result in vesicles that are an order of magnitude larger. Finally, we discuss the possible origin of the morphological striations that are observed on the surfaces of the caveolae.

cond-mat.soft↗

arXiv2003

Interactions between proteins bound to biomembranes

We study a physical model for the interaction between general inclusions bound to fluid membranes that possess finite tension, as well as the usual bending rigidity. We are motivated by an interest in proteins bound to cell membranes that apply forces to these membranes, due to either entropic or direct chemical interactions. We find an exact analytic solution for the repulsive interaction between two similar circularly symmetric inclusions. This repulsion extends over length scales of order tens of nanometers, and contrasts with the membrane-mediated contact attraction for similar inclusions on tensionless membranes. For non circularly symmetric inclusions we study the small, algebraically long-ranged, attractive contribution to the force that arises. We discuss the relevance of our results to biological phenomena, such as the budding of caveolae from cell membranes and the striations that are observed on their coats.

cond-mat.soft↗

arXiv2000

Precision Cosmology and the Density of Baryons in the Universe

Big-bang Nucleosynthesis (BBN) and Cosmic Microwave Background (CMB) anisotropy measurements give independent, accurate measurements of the baryon density and can test the framework of the standard cosmology. Early CMB data are consistent with the longstanding conclusion from BBN that baryons constitute a small fraction of matter in the Universe, but may indicate a slightly higher value for the baryon density. We clarify precisely what the two methods determine, and point out that differing values for the baryon density can indicate either an inconsistency or physics beyond the standard models of cosmology and particle physics. We discuss other signatures of the new physics in CMB anisotropy.

astro-ph↗

arXiv2000

Annihilating Cold Dark Matter

Structure formation with cold dark matter (CDM) predicts halos with a central density cusp, which are observationally disfavored. If CDM particles have an annihilation cross section sigma*v ~ 10**(-29) (m/GeV) cm**2, then annihilations will soften the cusps. We discuss plausible scenarios for avoiding the early Universe annihilation catastrophe that could result from such a large cross section. The predicted scaling of core density with halo mass depends upon the velocity dependence of sigma*v, and s-wave annihilation leads to a core density nearly independent of halo mass, which seems consistent with observations.

astro-ph↗

arXiv1998

The LMC Microlensing Events: Evidence for a Warped and Flaring Milky Way Disk?

The simplest interpretation of the microlensing events towards the Large Magellanic Cloud detected by the MACHO and EROS collaborations is that about one third of the halo of our own Milky Way galaxy exists in the form of objects of around 0.5 solar mass. There are grave problems with this interpretation. A normal stellar population of 0.5 solar mass stars should be visible. The other obvious candidate for the lenses is a population of white dwarfs. But, the precursor population must have polluted the interstellar medium with metals, in conflict with current population II abundance. Here, we propose a more conventional, but at the moment more speculative, explanation. Some of the lenses are stars in the disk of the Milky Way. They lie along the line of sight to the LMC because of warping and flaring of the Galactic disk. Depending on its scalelength and ellipticity, the disk's optical depth may lie anywhere between $0.2 \times 10^{-7}$ and $0.9 \times 10^{-7}$. Together with contributions from the LMC disk and bar and perhaps even intervening stellar contaminants, the total optical depth may match the data within the uncertainties. Microlensing towards the LMC may be telling us more about the distorted structure and stellar populations of the outer Milky Way disk than the composition of the dark halo.

astro-ph↗

arXiv1998

Diffusive growth of a polymer layer by in sity polymerization

We consider the growth of a polymer layer on a flat surface in a good solvent by in-situ polymerization. This is viewed as a modified form of diffusion-limited aggregation without branching. We predict theoretically the formation of a pseudo-brush with density rhog(z) \propto z^{-2/3} and characteristic height \propto t^{3}. These results are found by combining a mean-field treatment of the diffusive growth (marginally valid in three dimensions) with a scaling theory (Flory exponent nu =3/5) of the growing polymers. We confirm their validity by Monte Carlo simulations.

cond-mat.stat-mech↗

arXiv1996

Gamma Rays and the Decay of Neutrinos from SN1987A

We calculate limits to the properties of massive, unstable neutrinos using data from gamma-ray detectors on the Pioneer Venus Orbiter Satellite; a massive neutrino emitted from SN1987A that decayed in flight and produced gamma rays would be detectable by this instruments. The lack of such a signal allows us to constrain the branching ratio to photons ($\Bg$), mass ($\mnu$), and radiative lifetime ($τ_γ= τ/\Bg$). For low mass ($m<T\sim8\MeV$) neutrinos decaying $ν\rightarrowν'γ$, $\Bg<3\times 10^{-7}$, for $\mt\lesssim 10^6 \keV\sec$, and $\Bg<6\times 10^{-14} \mt/\keV\sec$ for $\mt\gtrsim 10^6 \keV\sec$; limits for high-mass neutrinos are somewhat weaker due to Boltzmann suppression. We also calculate limits for decays that produce gamma rays through the \brem channel, $ν\rightarrowν'e^+e^-γ$. In the case that neutrino mass states are nearly degenerate, $δm^2/m^2\ll1$, our limits for the mode $ν\rightarrowν'γ$ become more stringent by a factor of $δm^2/m^2$, because more of the decay photons are shifted into the PVO detector energy window.

astro-ph↗

arXiv1994

The Case for a Hubble Constant of 30 km/s/Mpc

Although cosmologists have been trying to determine the value of the Hubble constant for nearly 65 years, they have only succeeded in limiting the range of possibilities: most of the current observational determinations place the Hubble constant between 50 km/s/Mpc and 90 km/s/Mpc. The uncertainty is unfortunate because this fundamental parameter of cosmology determines both the distance scale and the time scale, and thereby affects almost all aspects of cosmology. Here we make the case for a Hubble constant that is even smaller than the lower bound of the accepted range, arguing on the basis of the great advantages, all theoretical in nature, of a Hubble constant of around 30 km/s/Mpc. Those advantages are: (1) a comfortable expansion age that avoids the current age crisis; (2) a cold dark matter power spectrum whose shape is in good agreement with the observational data and (3) which predicts an abundance of clusters in close agreement with that of x-ray selected galaxy clusters; (4) a nonbaryonic to baryonic mass ratio that is in better agreement with recent determinations based upon cluster x-ray studies. In short, such a value for the Hubble constant cures almost all the ills of the current theoretical orthodoxy, a flat Universe comprised predominantly of cold dark matter.

astro-ph↗

arXiv1994

Massive Tau Neutrino and SN 1987a

The emission of $\MeV$-mass tau neutrinos from newly formed neutron stars is considered in a simple, but accurate, model based upon the diffusion approximation. The tau-neutrinosphere temperature is found to increase with mass so that emission of massive tau neutrinos is not suppressed by the Boltzmann factor previously used, $(\mnu /T_ν)^{1.5}\exp(-\mnu/T_ν)$, where $T_ν\sim 4\MeV -8\MeV$. If the tau neutrino decays to electron neutrinos, then for short lifetimes ($\taunu\la10^{-3}\sec$) the location of both the tau and electron neutrinospheres can be affected, and, for very short lifetimes ($τ_ν\la 10^{-6}\sec$) its temperature falls below $1\MeV$, in conflict with neutrino observations of Supernova 1987A (SN 87A). Using our results, we revise limits to the mass/lifetime of an $\MeV$-mass tau neutrino based upon SN 87A. Our constraints, together with bounds based upon primordial nucleosynthesis and the laboratory mass limit of around $30\MeV$, exclude the possibility of a tau neutrino more massive than $0.4\MeV$ if the dominant decay mode is radiative. Finally, we speculate on the possible role a $15\MeV -25\MeV$ tau neutrino might play in the supernova explosion itself.

astro-ph↗

arXiv1994

Relaxing the Big-bang Bound to the Baryon Density

In the standard picture of big-bang nucleosynthesis the yields of D, $^3$He, $^4$He, and $^7$Li only agree with their inferred primordial abundances if the fraction of critical density contributed by baryons is between $0.01h^{-2}$ and $0.02h^{-2}$ ($h$ is the present value of the Hubble constant in units of $100\kms\Mpc^{-1}$). This is the basis of the very convincing and important argument that baryons can contribute at most 10\% of critical density and thus cannot close the Universe. Nonstandard scenarios involving decaying particles,$^1$ inhomogeneities in the baryon density,$^2$ and even more exotic ideas$^3$ put forth to evade this bound have been largely unsuccessful.$^4$ We suggest a new way of relaxing the bound: If the tau neutrino has a mass of $20\MeV-30\MeV$ and lifetime of $200\sec -1000\sec$, and its decay products include electron neutrinos, the bound to the baryon mass density can be loosened by a about factor of $10$. The key is the decay-generated electron antineutrinos: around the time of nucleosynthesis they are captured by protons to produce neutrons, thereby changing the outcome of nucleosynthesis. Experiments at $e^\pm$ colliders should soon be sensitive to a tau-neutrino mass in the required range.

astro-ph↗

arXiv1993

Primordial Nucleosynthesis with a Decaying Tau Neutrino

A comprehensive study of the effect of an unstable tau neutrino on primordial nucleosynthesis is presented. The standard code for nucleosynthesis is modified to allow for a massive decaying tau neutrino whose daughter products include neutrinos, photons, $e^\pm$ pairs, and/or noninteracting (sterile) daughter products. Tau-neutrino decays influence primordial nucleosynthesis in three distinct ways: (i) the energy density of the decaying tau neutrino and its daughter products affect the expansion rate tending to increase $^4$He, D, and $^3$He production; (ii) electromagnetic (EM) decay products heat the EM plasma and dilute the baryon-to-photon ratio tending to decrease $^4$He production and increase D and $^3$He production; and (iii) electron neutrinos and antineutrinos produced by tau-neutrino decays increase the weak rates that govern the neutron-to-proton ratio, leading to decreased $^4$He production for short lifetimes ($\la 30\sec$) and masses less than about $10\MeV$ and increased $^4$He production for long lifetimes or large masses. The precise effect of a decaying tau neutrino on the yields of primordial nucleosynthesis and the mass-lifetime limits that follow depend crucially upon decay mode. We identify four generic decay modes that serve to bracket the wider range of possibilities:

astro-ph↗