Hyperons in neutron-star cores and two-solar-mass pulsar

Recent measurement of mass of PSR J1614-2230 rules out most of existing models of equation of state (EOS) of dense matter with high-density softening due to hyperonization or a phase transition to quark matter or a boson condensate. We look for a solution of an apparent contradiction between the consequences stemming from up-to-date hypernuclear data, indicating appearance of hyperons at 3 nuclear densities and existence of a two-solar-mass neutron star. We consider a non-linear relativistic mean field (RMF) model involving baryon octet coupled to meson fields. An effective lagrangian includes quartic terms in the meson fields. The values of the parameters of the model are obtained by fitting semi-empirical parameters of nuclear matter at the saturation point, as well as potential wells for hyperons in nuclear matter and the strength of the Lambda-Lambda attraction in double-Lambda hypernuclei. We propose a non-linear RMF model which is consistent with up-to-date semiempirical nuclear and hypernuclear data and allows for neutron stars with hyperon cores and M larger than 2 solar masses. The model involves hidden-strangenes scalar and vector mesons, coupled to hyperons only, and quartic terms involving vector meson fields. Our EOS involving hyperons is stiffer than the corresponding nucleonic EOS (with hyperons artificially suppressed) above five nuclear densities. Required stiffening is generated by the quartic terms involving hidden-strangeness vector meson.Comment: 7 pages, 5 figures. Main results of this paper were already presented at the MODE-SNR-PWN Workshop in Bordeaux, France, November 15-17, 2010, and in a poster at the CompStar 2011 Workshop in Catania, Italy, May 9-12, 2011. The paper is being submitted to Astronomy & Astrophysic

Solving relativistic hydrodynamic equation in presence of magnetic field for phase transition in a neutron star

Hadronic to quark matter phase transition may occur inside neutron stars (NS) having central densities of the order of 3-10 times normal nuclear matter saturation density ($n_0$). The transition is expected to be a two-step process; transition from hadronic to 2-flavour matter and two-flavour to $\beta$ equilibrated charge neutral three-flavour matter. In this paper we concentrate on the first step process and solve the relativistic hydrodynamic equations for the conversion front in presence of high magnetic field. Lorentz force due to magnetic field is included in the energy momentum tensor by averaging over the polar angles. We find that for an initial dipole configuration of the magnetic field with a sufficiently high value at the surface, velocity of the front increases considerably.Comment: 16 pages, 4 figures, same as published version of JPG, J. Phys. G: Nucl. Part. Phys. 39 (2012) 09520

Core collapse supernovae in the QCD phase diagram

We compare two classes of hybrid equations of state with a hadron-to-quark matter phase transition in their application to core collapse supernova simulations. The first one uses the quark bag model and describes the transition to three-flavor quark matter at low critical densities. The second one employs a Polyakov-loop extended Nambu-Jona-Lasinio (PNJL) model with parameters describing a phase transition to two-flavor quark matter at higher critical densities. These models possess a distinctly different temperature dependence of their transition densities which turns out to be crucial for the possible appearance of quark matter in supernova cores. During the early post bounce accretion phase quark matter is found only if the phase transition takes place at sufficiently low densities as in the study based on the bag model. The increase critical density with increasing temperature, as obtained for our PNJL parametrization, prevents the formation of quark matter. The further evolution of the core collapse supernova as obtained applying the quark bag model leads to a structural reconfiguration of the central proto-neutron star where, in addition to a massive pure quark matter core, a strong hydrodynamic shock wave forms and a second neutrino burst is released during the shock propagation across the neutrinospheres. We discuss the severe constraints in the freedom of choice of quark matter models and their parametrization due to the recently observed 2 solar mass pulsar and their implications for further studies of core collapse supernovae in the QCD phase diagram.Comment: 19 pages, 4 figures, CPOD2010 conference proceedin

German National Consensus Recommendations on Nutrition and Lifestyle in Pregnancy by the ‘Healthy Start - Young Family Network’

Diet and physical activity before and during pregnancy affect short- andlong-term health of mother and child. The energy needs at the end ofpregnancy increase only by about 10% compared to nonpregnant women. Anexcessive energy intake is undesirable since maternal overweight andexcessive weight gain can increase the risks for a high birth weight andlater child overweight and diabetes. Maternal weight at the beginning ofpregnancy is especially important for pregnancy outcome and childhealth. Women should strive to achieve normal weight already beforepregnancy. Regular physical activity can contribute to a healthy weightand to the health of pregnant women. The need for certain nutrientsincreases more than energy requirements. Before and during pregnancy,foods with a high content of essential nutrients should bepreferentially selected. Supplements should include folic acid andiodine, iron (in case of suboptimal iron stores), the omega-3 fatty aciddocosahexaenoic acid (in case of infrequent consumption of ocean fish)and vitamin D (in case of decreased sun exposure and decreasedendogenous vitamin D synthesis). Pregnant women should not smoke and notstay in rooms where others smoke or have smoked before (passivesmoking). Alcohol consumption should be avoided, since alcohol can harmunborn children

German National Consensus Recommendations on Nutrition and Lifestyle in Pregnancy by the ‘Healthy Start - Young Family Network’

Diet and physical activity before and during pregnancy affect short- andlong-term health of mother and child. The energy needs at the end ofpregnancy increase only by about 10% compared to nonpregnant women. Anexcessive energy intake is undesirable since maternal overweight andexcessive weight gain can increase the risks for a high birth weight andlater child overweight and diabetes. Maternal weight at the beginning ofpregnancy is especially important for pregnancy outcome and childhealth. Women should strive to achieve normal weight already beforepregnancy. Regular physical activity can contribute to a healthy weightand to the health of pregnant women. The need for certain nutrientsincreases more than energy requirements. Before and during pregnancy,foods with a high content of essential nutrients should bepreferentially selected. Supplements should include folic acid andiodine, iron (in case of suboptimal iron stores), the omega-3 fatty aciddocosahexaenoic acid (in case of infrequent consumption of ocean fish)and vitamin D (in case of decreased sun exposure and decreasedendogenous vitamin D synthesis). Pregnant women should not smoke and notstay in rooms where others smoke or have smoked before (passivesmoking). Alcohol consumption should be avoided, since alcohol can harmunborn children

Human 13N-ammonia PET studies: the importance of measuring 13N-ammonia metabolites in blood

Dynamic 13N-ammonia PET is used to assess ammonia metabolism in brain, liver and muscle based on kinetic modeling of metabolic pathways, using arterial blood 13N-ammonia as input function. Rosenspire et al. (1990) introduced a solid phase extraction procedure for fractionation of 13N-content in blood into 13N-ammonia, 13N-urea, 13N-glutamine and 13N-glutamate. Due to a radioactive half-life for 13N of 10 min, the procedure is not suitable for blood samples taken beyond 5–7 min after tracer injection. By modifying Rosenspire’s method, we established a method enabling analysis of up to 10 blood samples in the course of 30 min. The modified procedure was validated by HPLC and by 30-min reproducibility studies in humans examined by duplicate 13N-ammonia injections with a 60-min interval. Blood data from a 13N-ammonia brain PET study (from Keiding et al. 2006) showed: (1) time courses of 13N-ammonia fractions could be described adequately by double exponential functions; (2) metabolic conversion of 13N-ammonia to 13N-metabolites were in the order: healthy subjects > cirrhotic patients without HE > cirrhotic patients with HE; (3) kinetics of initial tracer distribution in tissue can be assessed by using total 13N-concentration in blood as input function, whereas assessment of metabolic processes requires 13N-ammonia measurements

Solvation free energy profile of the SCN- ion across the water-1,2-dichloroethane liquid/liquid interface. A computer simulation study

The solvation free energy profile of a single SCN- ion is calculated across the water-1,2-dichloroethane liquid/liquid interface at 298 K by the constraint force method. The obtained results show that the free energy cost of transferring the ion from the aqueous to the organic phase is about 70 kJ/mol, The free energy profile shows a small but clear well at the aqueous side of the interface, in the subsurface region of the water phase, indicating the ability of the SCN- ion to be adsorbed in the close vicinity of the interface. Upon entrance of the SCN- ion to the organic phase a coextraction of the water molecules of its first hydration shell occurs. Accordingly, when it is located at the boundary of the two phases the SCN- ion prefers orientations in which its bulky S atom is located at the aqueous side, and the small N atom, together with its first hydration shell, at the organic side of the interface