Prispevek prinaša pregled in analizo obstoječe prakse izobraževanja kot dela priprave na porod na primeru šole za bodoče starše v Sloveniji. Raziskava ugotavlja potrebe po spremembah v ...organizacijskem in vsebinskem smislu. Avtorici najprej predstavita interdisciplinarne vsebine babištva, porodništva in družinske andragogike ter dejavnike, ki vplivajo na učinkovi- tost izobraževanja za bodoče starše glede na značilnosti različnih modelov izobraževanja. Avtorici ugotavljata, da je v slovenskem prostoru vzpostavljena tradicija izobraževalnih programov za pripravo na porod in da se programi le počasi prilagajajo spremembam, ki jih lahko zasledimo v tujini, kjer se vse bolj uveljavljajo modeli, ki poudarjajo individualiziran pristop ter kontinuiteto v obravnavi od priprave na starševstvo, med nosečnostjo, porodom in v poporodnem obdobju. V letu 2010 je bila v Sloveniji prvič izvedena pilotna študija Zdrave ženske – zdrave družine prihodnosti, projekt, v katerem je bilo izobraževanje za bodoče starše izvedeno na interdisciplinaren način s strokovnjaki različnih strok ter usmerjeno v potrebe žensk in njihovih partnerjev na prehodu v starševstvo. Gre za prvi poskus novega načina izobraževanja in obravnave za bodoče starše v slovenskem prostoru, ki pa ga obstoječi zdravstveni sistem (še) ne podpira. Udeleženci so najvišje ocenili organizacijo in izvedbo programa s poudarkom na načinu podajanja snovi oziroma izbiri metode in oblike izobraževanja. Rezultati kažejo, da si udeleženci projekta pri izobraževanju za bodoče starše želijo več poudarka na vsebinah poporodne obravnave, partnerskega odnosa in nasvetov glede dojenja. Posebej izpostavljeni so bili svetovalno delo ter kontinuiteta in individualna obravnava vsakega para.
ABSTRACT We present the discovery that UScoCTIO 5, a known spectroscopic binary in the Upper Scorpius star-forming region (P = 34 days, ), is an eclipsing system with both primary and secondary ...eclipses apparent in K2 light curves obtained during Campaign 2. We have simultaneously fit the eclipse profiles from the K2 light curves and the existing RV data to demonstrate that UScoCTIO 5 consists of a pair of nearly identical M4.5 stars with , , , and . The radii are broadly consistent with pre-main-sequence ages predicted by stellar evolutionary models, but none agree to within the uncertainties. All models predict systematically incorrect masses at the 25%-50% level for the HR diagram position of these mid-M dwarfs, suggesting significant modifications to mass-dependent outcomes of star and planet formation. The form of the discrepancy for most model sets is not that they predict luminosities that are too low, but rather that they predict temperatures that are too high, suggesting that the models do not fully encompass the physics of energy transport (via convection and/or missing opacities) and/or a miscalibration of the SpT- scale. The simplest modification to the models (changing to match observations) would yield an older age for this system, in line with the recently proposed older age of Upper Scorpius (τ ∼ 11 Myr).
High-field magnetic white dwarfs have been long suspected to be the result of stellar mergers. However, the nature of the coalescing stars and the precise mechanism that produces the magnetic field ...are still unknown. Here, we show that the hot, convective, differentially rotating corona present in the outer layers of the remnant of the merger of two degenerate cores can produce magnetic fields of the required strength that do not decay for long timescales. Using a state-of-the-art Monte Carlo simulator, we also show that the expected number of high-field magnetic white dwarfs produced in this way is consistent with that found in the solar neighborhood.
ABSTRACT We substantially update the capabilities of the open-source software instrument Modules for Experiments in Stellar Astrophysics (MESA). MESA can now simultaneously evolve an interacting pair ...of differentially rotating stars undergoing transfer and loss of mass and angular momentum, greatly enhancing the prior ability to model binary evolution. New MESA capabilities in fully coupled calculation of nuclear networks with hundreds of isotopes now allow MESA to accurately simulate the advanced burning stages needed to construct supernova progenitor models. Implicit hydrodynamics with shocks can now be treated with MESA, enabling modeling of the entire massive star lifecycle, from pre-main-sequence evolution to the onset of core collapse and nucleosynthesis from the resulting explosion. Coupling of the GYRE non-adiabatic pulsation instrument with MESA allows for new explorations of the instability strips for massive stars while also accelerating the astrophysical use of asteroseismology data. We improve the treatment of mass accretion, giving more accurate and robust near-surface profiles. A new MESA capability to calculate weak reaction rates "on-the-fly" from input nuclear data allows better simulation of accretion induced collapse of massive white dwarfs and the fate of some massive stars. We discuss the ongoing challenge of chemical diffusion in the strongly coupled plasma regime, and exhibit improvements in MESA that now allow for the simulation of radiative levitation of heavy elements in hot stars. We close by noting that the MESA software infrastructure provides bit-for-bit consistency for all results across all the supported platforms, a profound enabling capability for accelerating MESA's development.
We present the chemical abundance analysis of 33 red giant stars belonging to the complex stellar system Terzan 5. We confirm the discovery of two stellar populations with distinct iron abundances: a ...relatively metal-poor component with Fe/H = --0.25 ? 0.07 rms and another component with Fe/H = +0.27 ? 0.04 rms, exceeding in metallicity any known Galactic globular cluster (GC). The two populations also show different Delta *a/Fe abundance ratios. The metal-poor component has an average Delta *a/Fe =+0.34 ? 0.06 rms, consistent with the canonical scenario for rapid enrichment by core collapse supernovae (SNe). The metal-rich component has Delta *a/Fe =+0.03 ? 0.04 rms, suggesting that the gas from which it formed was polluted by both type II and type Ia SNe on a longer timescale. Neither of the two populations shows evidence of the Al/Fe over O/Fe anti-correlation that is typically observed in Galactic GCs. Because these chemical abundance patterns are unique, we propose that Terzan 5 is not a true GC, but a stellar system with a much more complex history of star formation and chemical enrichment.
ABSTRACT We explore the ramification of associating the energetics of extreme magnetic reconnection events with transient mass-loss in a stellar analogy with solar eruptive events. We establish ...energy partitions relative to the total bolometric radiated flare energy for different observed components of stellar flares and show that there is rough agreement for these values with solar flares. We apply an equipartition between the bolometric radiated flare energy and kinetic energy in an accompanying mass ejection, seen in solar eruptive events and expected from reconnection. This allows an integrated flare rate in a particular waveband to be used to estimate the amount of associated transient mass-loss. This approach is supported by a good correspondence between observational flare signatures on high flaring rate stars and the Sun, which suggests a common physical origin. If the frequent and extreme flares that young solar-like stars and low-mass stars experience are accompanied by transient mass-loss in the form of coronal mass ejections, then the cumulative effect of this mass-loss could be large. We find that for young solar-like stars and active M dwarfs, the total mass lost due to transient magnetic eruptions could have significant impacts on disk evolution, and thus planet formation, and also exoplanet habitability.
ABSTRACT Gamma Cassiopeiae is an enigmatic Be star with unusually strong hard X-ray emission. The Suzaku observatory detected six rapid X-ray spectral hardening events called "softness dips" in a ...∼100 ks observation in 2011. All the softness dip events show symmetric softness-ratio variations, and some of them have flat bottoms apparently due to saturation. The softness dip spectra are best described by either ∼40% or ∼70% partial covering absorption to kT ∼ 12 keV plasma emission by matter with a neutral hydrogen column density of ∼(2−8) × 1021 cm−2, while the spectrum outside these dips is almost free of absorption. This result suggests the presence of two distinct X-ray-emitting spots in the γ Cas system, perhaps on a white dwarf (WD) companion with dipole mass accretion. The partial covering absorbers may be blobs in the Be stellar wind, the Be disk, or rotating around the WD companion. Weak correlations of the softness ratios to the hard X-ray flux suggest the presence of stable plasmas at kT ∼ 0.9 and 5 keV, which may originate from the Be or WD winds. The formation of a Be star and WD binary system requires mass transfer between two stars; γ Cas may have experienced such activity in the past.
ABSTRACT We reanalyze data on the surface densities and vertical distribution of baryonic matter in the solar neighborhood and tabulate the results. We find a local total surface density of M dwarfs ...of , whcih is significantly higher than previous values. Our result for the total local surface density of visible stars (main-sequence stars and giants), , is close to previous estimates due to a cancellation of opposing effects: more mass in M dwarfs, less mass in the others. The total local surface density in white dwarfs is ; in brown dwarfs, it is , but with considerable uncertainty. We find that the total local surface density of stars and stellar remnants is , which is somewhat less than previous estimates but within the errors of many of them. We analyze data on 21 cm emission and absorption and obtain good agreement with recent results on the local amount of neutral atomic hydrogen obtained with the Planck satellite. The local surface density of gas is . The total baryonic mass surface density that we derive for the solar neighborhood is ( within 1.1 kpc of the midplane). Combining these results with others' measurements of the total surface density of matter within 1-1.1 kpc of the plane, we find that the local density of dark matter is GeV cm . The local density of all matter is . We discuss limitations on the properties of a possible thin disk of dark matter.
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