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

Non-ideal magnetohydrodynamics versus turbulence – I. Which is the dominant process in protostellar disc formation?

Funding: European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013 grant agreement no. 339248); University of St Andrews (JW). National Aeronautics and Space Administration (NASA) through grant NN17AK90G and from the National Science Foundation (NSF) through grants no 1517488 and PHY-1748958 (BTL).Non-ideal magnetohydrodynamics (MHD) is the dominant process. We investigate the effect of magnetic fields (ideal and non-ideal) and turbulence (sub- and transsonic) on the formation of circumstellar discs that form nearly simultaneously with the formation of the protostar. This is done by modelling the gravitational collapse of a 1 M☉ gas cloud that is threaded with a magnetic field and imposed with both rotational and turbulent velocities. We investigate magnetic fields that are parallel/antiparallel and perpendicular to the rotation axis, two rotation rates, and four Mach numbers. Disc formation occurs preferentially in the models that include non-ideal MHD where the magnetic field is antiparallel or perpendicular to the rotation axis. This is independent of the initial rotation rate and level of turbulence, suggesting that subsonic turbulence plays a minimal role in influencing the formation of discs. Aside from first core outflows that are influenced by the initial level of turbulence, non-ideal MHD processes are more important than turbulent processes during the formation of discs around low-mass stars.Publisher PDFPeer reviewe

Non-ideal magnetohydrodynamics versus turbulence II : which is the dominant process in stellar core formation?

Funding: JW acknowledges support from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007- 2013 grant agreement no. 339248), and from the University of St Andrews. BTL acknowledges the support of the National Aeronautics and Space Administration (NASA) through grant NN17AK90G and from the National Science Foundation (NSF) through grants no. 1517488 and PHY-1748958.Non-ideal magnetohydrodynamics (MHD) is the dominant process. We investigate the effect of magnetic fields (ideal and non-ideal) and turbulence (sub- and transsonic) on the formation of protostars by following the gravitational collapse of 1 M☉ gas clouds through the first hydrostatic core to stellar densities. The clouds are imposed with both rotational and turbulent velocities, and are threaded with a magnetic field that is parallel/antiparallel or perpendicular to the rotation axis; we investigate two rotation rates and four Mach numbers. The initial radius and mass of the stellar core are only weakly dependent on the initial parameters. In the models that include ideal MHD, the magnetic field strength implanted in the protostar at birth is much higher than observed, independent of the initial level of turbulence; only non-ideal MHD can reduce this strength to near or below the observed levels. This suggests that not only is ideal MHD an incomplete picture of star formation, but that the magnetic fields in low mass stars are implanted later in life by a dynamo process. Non-ideal MHD suppresses magnetically launched stellar core outflows, but turbulence permits thermally launched outflows to form a few years after stellar core formation.Publisher PDFPeer reviewe

Smoothed particle magnetohydrodynamic simulations of protostellar outflows with misaligned magnetic field and rotation axes (dataset)

The compressed tarballs in this repository contain the binary output data from the SPMHD (smoothed particle magnetohydrodynamics) simulation presented in the paper. The data is a Fortran binary file in big-endian format. The DAT???? files are dumps of the simulation spaced every 1/100 of a free-fall time and can be read in Splash (Written by Daniel Price, see http://users.monash.edu.au/~dprice/splash/). The Atest_? and Ptest_? files contain information on accreted particles and sink particles respectively (again in big-endian format). The two Fortran programs in utils.tar.xz can read these files and output ASCII data. The tarballs themselves are named according to the following scheme: theta_*.tar.xz are the 1.5 million particle simulations presented as the main result of the paper, where theta_0.tar.xz is a fully aligned model and theta_90.tar.xz is fully misaligned (i.e. theta = 90) &c.; lowres_*.tar.xz are the two low-resolution collapse simulations earlier in the paper and disc_*.tar.xz are the two test models. For both the low-resolution and test models, `clean' denotes the result of using and unmodified code and `hav' denotes the new formalism presented in the paper. All the plots in the paper, except for Figs. 13 and 14, can be produced using Splash and the `DAT' files directly. Figs. 13 and 14 use the data extracted from the `A' and `P' files.The journal article associated with this datast was published in Monthly Notices of the Royal Astronomical Society Vol. 451 (1), pp 288-299. doi: 10.1093/mnras/stv957 and is in ORE at http://hdl.handle.net/10871/19588The article associated with this dataset is available in ORE at http://hdl.handle.net/10871/19588.This is the dataset that was used to produce the paper published in MNRAS. Included are the binary dump files from each of the simulations in the paper and two utilities that can be used to produce an ASCII file detailing accreted particles.Science and Technology Facilities CouncilEuropean Research CouncilAustralian Research Council Discovery Project GrantUniversity of Exeter Supercomputer: jointly funded by Science and Technology Facilities Council (STFC), Large Facilities Capital Fund of BIS, and the University of Exeter DiRac Complexity computer: jointly funded by Science and Technology Facilities Council (STFC) and the Large Facilities Capital Fund of BI

Active Referral Intervention following Fragility Fractures Leads to Enhanced Osteoporosis Follow-Up Care

At one major urban academic medical center, patients aged 50 years and older with fragility fractures were identified and scheduled or assisted in referral into osteoporosis medical management appointments. We evaluated the efficacy of an active intervention program at overcoming the logistical barriers and improving proper osteoporosis follow-up for persons who have sustained a fragility fracture. Of 681 patients treated for defined fractures, 168 were eligible and consented for the study of fragility fractures. Of those enrolled, 91 (54.2%) had appropriate osteoporosis follow-up on initial interview, and overall 120 (71.4%) had successful osteoporosis follow-up following our active intervention. Seventy patients (41.7%) were deemed to have no osteoporosis follow-up, and, of these, 48 were successfully referred to a scheduling coordinator. The scheduling coordinator was able to contact 37 (77%) patients to schedule proper follow-up, and, of these, 29 (78.4%) confirmed receiving an appropriate follow-up appointment. Active intervention and assisted scheduling for patients with recent fragility fractures improved the self-reported rate of osteoporosis follow-up from 54.2% to 71.4%

Terrestrial snail communities of the lower rio grande valley are affected by human disturbance and correlate with vegetation community composition

The lower Rio Grande Valley of Texas (LRGV) contains a unique, subtropical, semiarid floodplain with most of the few remaining Tamaulipan thorn forests in the United States. Less than 2% of Tamaulipan thorn forest remains, with urban and agricultural conversion potentially threatening diverse plant and animal communities native to the habitat. We performed vegetative community surveys and conducted a comprehensive survey of terrestrial snail communities in intact (refugia sites, minimally altered in recent times) and altered (previously cleared and regrown or restored) Tamaulipan thorn forest habitats of the LRGV. In a comparison of intact and altered sites that have comparable vegetation (paired sites), we found that intact sites had a less species-rich snail community than their altered counterparts, but this difference was not statistically significant. This counterintuitive result, in part reflects the fact that the most species-rich, intact snail communities (i.e., Sabal Palm Forest) have no altered (restored or regrown) counterparts and so were not included in the paired comparisons. A nestedness analysis supports this, finding that these unique intact sites, which have the highest species richness and no comparable restored sites, contain the largest pool of species in South Texas. Species richness of snails significantly correlated with a precipitation gradient. A general linear model incorporating mean canopy cover, mean plant height, plant abundance, and plant species richness shows a significant correlation with snail communities. This study is the only comprehensive survey of the snail communities of the lower Rio Grande Valley. - La cuenca baja del río Grande en Texas (LRGV) contiene una llanura de inundación única, subtropical y semiárida con la mayor´ıa de los remanentes de los bosques espinosos tamaulipecos en los Estados Unidos. Queda menos del 2% del bosque espinoso tamaulipeco, con la conversión a áreas urbanas y agrıcolas potencialmente amenazando las comunidades diversas de plantas y animales nativos del hábitat. Hicimos muestreos de comunidades vegetales y un muestreo comprensivo de comunidades de caracoles terrestres en hábitats de bosques espinosos tamaulipecos intactos (sitios refugio, con poca alteración en tiempos recientes) y perturbados (previamente cortados y recuperados o restaurados) en el LRGV. En una comparaci ´on de los sitios intactos con los perturbados con la vegetación comparable (sitios emparejados), sitios intactos tuvieron comunidades con menos riqueza de especies de caracoles que sus contrapartes alteradas, aunque la diferencia no fue estad´ısticamente significativa. Este resultado contra intuitivo, en parte refleja el hecho de que las comunidades intactas de caracoles mas ricas en especies (o sea, Sabal Palm Forest) no tienen contrapartes alteradas (restauradas o regeneradas) y por eso no fueron incluidas en las comparaciones emparejadas. Un análisis de anidamiento respalda esto, encontrando que estos ´unicos sitios intactos, que tienen la mayor riqueza de especies y ningun sitio comparable restaurado, contienen el grupo más grande de especies en el sur de Texas. La riqueza de especies de caracoles se correlacion significativamente con un gradiente de precipitación. Un modelo lineal general incorporando el promedio de cobertura del dosel, el promedio de altura vegetal, la abundancia de plantas, y la riqueza de especies de plantas muestra una correlación significativa con comunidades de caracoles. Este es el único muestreo comprensivo de las comunidades de caracoles de la cuenca baja del río Grande