Protective effect of perioperative recombinant human growth hormone application on intestinal mucosal barrier function in patients with intestinal obstruction and the assessment of immune inflammatory response

Objective:To study the protective effect of perioperative recombinant human growth hormone (r-hGH) application on intestinal mucosal barrier function in patients with intestinal obstruction and the influence on the immune inflammatory response.Methods:60 patients with intestinal obstruction who underwent surgical treatment in our hospital between February 2013 and July 2016 were selected as the research subjects and divided into the control group (n=34) who received conventional surgical treatment and the observation group (n=26) who received surgery combined with perioperative r-hGH treatment. The serum levels of intestinal mucosal barrier indexes, immunoglobulin and inflammatory response indicators were compared between two groups of patients before and after treatment.Results: Before treatment, differences in serum levels of intestinal mucosal barrier indexes, immunoglobulin and inflammatory response indicators were not statistically significant between the two groups of patients. After treatment, serum intestinal mucosal barrier indexes Endotoxin, D-Lactate and DAO levels in observation group were lower than those in control group, immunoglobulin IgA, IgM and IgG levels were higher than those in control group, and inflammatory response indicators IL-1, IL-6, PCT and TNF-α levels were lower than those in control group patients. Conclusion:Perioperative r-hGH application in patients with intestinal obstruction can protect the intestinal mucosal barrier, also optimize the humoral immunity and suppress the systemic inflammatory response.

The effect of hydrodynamics alone on the subhalo population in aΛCDM rich cluster sized dark matter halo

We perform a set of non-radiative hydro-dynamical(NHD)simulations of a rich cluster sized dark matter halo from the Phoenix Project with three different numerical resolutions,to investigate the effect of hydrodynamics alone on the subhalo population in the halo.Compared to dark matter only(DMO)simulations of the same halo,subhaloes are less abundant for relatively massive subhaloes(Msub>2.5×109h 1M⊙,or Vmax>70 km s 1)but more abundant for less massive subhaloes in the NHD simulations.This results in different shapes in the subhalo mass/Vmax function in two different sets of simulations.At given subhalo mass,the subhaloes less massive than 1010h 1M⊙have larger Vmax in the NHD than DMO simulations,while Vmax is similar for the subhaloes more massive than the mass value.This is mainly because the progenitors of present day low mass subhaloes have larger concentration parameters in the NHD than DMO simulations.The survival number fraction of the accreted low mass progenitors of the main halo at redshift 2 is about 50 percent higher in the NHD than DMO simulations.

The temperature of IGM at high redshifts:shock heating and high mach problem

The thermal history of cosmic gas in the dark ages remains largely unknown.It is important to quantify the impact of relevant physics on the IGM temperature between z=10 and z^30,in order to interpret recent and oncoming observations,including results reported by EDGES.We revisit the gas heating due to structure formation shocks in this era,using a set of fixed grid cosmological hydrodynamical simulations performed by three different codes.In all our simulations,the cosmic gas is predicted to be in multiphase state since z>30.The gas surrounding high density peaks gradually develops a relation more sharp than T∝ρ2/3,approximately T∝ρ2,from z=30 to z=11,might be due to shock heating.Meanwhile,the gas in void region tends to have a large local Mach number,and their thermal state varies significantly from code to code.In the redshift range 11-20,the mass fraction of gas shock heated above the CMB temperature in our simulations is larger than previous semi-analytical results by a factor of 2 to 8.At z=15,the fraction varies from^19%to 52%among different codes.Between z=11 and z=20,the gas temperature<1/TK>M-1 is predicted to be^10-20 K by two codes,much higher than the adiabatic cooling model and some previous works.However,in our simulations performed by RAMSES,<1/TK>M-1is predicted to be even below the temperature required to explain result of the EDGES.Given the fact that different codes give different predictions,currently,it seems a challenge to make solid prediction on the temperature of gas at z^17 in simulations.