Simple and accurate modelling of the gravitational potential produced by thick and thin exponential discs

We present accurate models of the gravitational potential produced by a radially exponential disc mass distribution. The models are produced by combining three separate Miyamoto–Nagai discs. Such models have been used previously to model the disc of the Milky Way, but here we extend this framework to allow its application to discs of any mass, scalelength, and a wide range of thickness from infinitely thin to near spherical (ellipticities from 0 to 0.9). The models have the advantage of simplicity of implementation, and we expect faster run speeds over a double exponential disc treatment. The potentials are fully analytical, and differentiable at all points. The mass distribution of our models deviates from the radial mass distribution of a pure exponential disc by <0.4 per cent out to 4 disc scalelengths, and <1.9 per cent out to 10 disc scalelengths. We tabulate fitting parameters which facilitate construction of exponential discs for any scalelength, and a wide range of disc thickness (a user-friendly, web-based interface is also available). Our recipe is well suited for numerical modelling of the tidal effects of a giant disc galaxy on star clusters or dwarf galaxies. We consider three worked examples; the Milky Way thin and thick disc, and a discy dwarf galaxy

Congruent families and invariant tensors

Classical results of Chentsov and Campbell state that -- up to constant multiples -- the only $2$-tensor field of a statistical model which is invariant under congruent Markov morphisms is the Fisher metric and the only invariant $3$-tensor field is the Amari-Chentsov tensor. We generalize this result for arbitrary degree $n$, showing that any family of $n$-tensors which is invariant under congruent Markov morphisms is algebraically generated by the canonical tensor fields defined in an earlier paper

s-Process Nucleosynthesis in Advanced Burning Phases of Massive Stars

We present a detailed study of s-process nucleosynthesis in massive stars of solar-like initial composition and masses 15, 20,25, and 30 Msun. We update our previous results of s-process nucleosynthesis during the core He-burning of these stars and then focus on an analysis of the s-process under the physical conditions encountered during the shell-carbon burning. We show that the recent compilation of the Ne22(alpha,n)Mg25 rate leads to a remarkable reduction of the efficiency of the s-process during core He-burning. In particular, this rate leads to the lowest overproduction factor of Kr80 found to date during core He-burning in massive stars. The s-process yields resulting from shell carbon burning turn out to be very sensitive to the structural evolution of the carbon shell. This structure is influenced by the mass fraction of C12 attained at the end of core helium burning, which in turn is mainly determined by the C12(alpha,gamma)O16 reaction. The still present uncertainty in the rate for this reaction implies that the s-process in massive stars is also subject to this uncertainty. We identify some isotopes like Zn70 and Rb87 as the signatures of the s-process during shell carbon burning in massive stars. In determining the relative contribution of our s-only stellar yields to the solar abundances, we find it is important to take into account the neutron exposure of shell carbon burning. When we analyze our yields with a Salpeter Initial Mass Function, we find that massive stars contribute at least 40% to s-only nuclei with mass A 90, massive stars contribute on average ~7%, except for Gd152, Os187, and Hg198 which are ~14%, \~13%, and ~11%, respectively.Comment: 52 pages, 16 figures, accepted for publication in Ap

Making a Place for the Next Generation of Geoscientists

Early-career scientists from the AGU Mentoring Network discuss how the global pandemic has exacerbated long-standing issues with the availability of positions in and the diversity of the geosciences.</jats:p

The New Pretender: A Large UK Case Series of Retinal Injuries in Children Secondary to Handheld Lasers

Purpose: To characterize a large single-center series of retinal injuries in children secondary to handheld laser devices, with emphasis on potential prognostic factors. / Design: Retrospective case series. / Methods: Sixteen children (24 eyes) with retinal injuries secondary to handheld lasers were identified from our electronic patient record system. Case notes, digital fundus photography, and spectral-domain optical coherence tomography images were reviewed. / Results: The mean age of affected children was 12.7 years (range 9–16 years), with 12 male and 4 female subjects. Mean follow up was 5.4 months (range 1–23 months). Five children (31%) were referred as suspected retinal dystrophies. The mean logMAR visual acuity at presentation was 0.30 (20/40) (range −0.20 [20/12.5] to 1.6 [20/800]). Eleven children (69%; 15 eyes) had “mild” injuries with focal retinal disruption confined to the photoreceptor and ellipsoid layers; such injuries were associated with a better prognosis, the mean visual acuity at presentation being 0.10 (20/25). “Moderate” injuries were seen in 3 eyes of 2 children, with retinal disruption confined to the outer retinal layer but diffuse rather than focal in nature. Three patients (4 eyes) had “severe” injuries, with subfoveal outer retinal architecture loss and overlying hyperreflective material in inner retinal layers. / Conclusion: Retinal injuries secondary to handheld laser devices may be difficult to diagnose and are likely underreported. It is important that such data are in the public domain, so regulatory authorities recognize the importance of laser retinopathy as an avoidable cause of childhood visual impairment and take steps to minimize the incidence and impact of laser injuries

Direct measurement of molecular stiffness and damping in confined water layers

We present {\em direct} and {\em linear} measurements of the normal stiffness and damping of a confined, few molecule thick water layer. The measurements were obtained by use of a small amplitude (0.36 $\textrm{\AA}$), off-resonance Atomic Force Microscopy (AFM) technique. We measured stiffness and damping oscillations revealing up to 7 layers separated by 2.56 $\pm$ 0.20 $\textrm{\AA}$. Relaxation times could also be calculated and were found to indicate a significant slow-down of the dynamics of the system as the confining separation was reduced. We found that the dynamics of the system is determined not only by the interfacial pressure, but more significantly by solvation effects which depend on the exact separation of tip and surface. Thus ` solidification\rq seems to not be merely a result of pressure and confinement, but depends strongly on how commensurate the confining cavity is with the molecule size. We were able to model the results by starting from the simple assumption that the relaxation time depends linearly on the film stiffness.Comment: 7 pages, 6 figures, will be submitted to PR