bluuebunny/crossref_metadata_2025_split huggingface dataset:
Star Formation in the Early Universe
Authors: Omukai Kazuyuki 
Published: September 2012

AbstractIn low-metallicity environments, massive stars are more easily formed than in the solar neighborhood. In this article, we see the following examples of low-mass star formation. We first describe the first star formation in the universe and argue that they are typically ordinary-sized massive stars, rather than very massive (> 100M⊙) ones. Next, we see how the metal-enrichment changes the thermal evolution of gas, thereby causing the shift of characteristic stellar mass towards lower mass. Finally, we discuss the possibility of forming supermassive stars in some special conditions in young galaxies.
Pair-Instability Explosions: observational evidence
Authors: Gal-Yam Avishay 
Published: September 2012

AbstractIt has been theoretically predicted many decades ago that extremely massive stars that develop large oxygen cores will become dynamically unstable, due to electron-positron pair production. The collapse of such oxygen cores leads to powerful thermonuclear explosions that unbind the star and can produce, in some cases, many solar masses of radioactive 56Ni. For many years, no examples of this process were observed in nature. Here, I briefly review recent observations of luminous supernovae that likely result from pair-instability explosions, in the nearby and distant Universe.
Asymmetry in Supernovae
Authors: Maeda Keiichi 
Published: September 2012

AbstractAsymmetry in the innermost part of the supernova (SN) ejecta is a key to understanding their explosion mechanisms. Late-time spectroscopy is a powerful tool to investigate the issue. We show what kind of geometry is inferred for different types of SNe – core-collapse SNe Ib/c, those associated with Gamma-Ray Bursts (GRBs), and thermonuclear SNe Ia –, and discuss implications for the explosion mechanisms, observational diversities, and cosmological applications. For SNe Ib/c, the data show the clear deviation from spherical symmetry, and they are most consistent with the bipolar-type explosion as the characteristic geometry. Detailed modeling of optical emissions from SN 1998bw associated with GRB980425 indicates that this SN was in the extreme end of the bipolar explosion, suggesting that the explosion mechanisms of canonical SNe Ib/c and GRB-SNe are different. The situation is different for SNe Ia. Late-time spectra indicate the deviation from spherical symmetry, but for SNe Ia the explosion is asymmetric between two hemispheres, i.e., one-sided explosions. The diversities arising from different viewing directions can nicely explain (a part of) observational diversities of SNe Ia, and correcting this effect may improve the standard-candle calibration of SNe Ia for cosmology.
Formation and evolution of black hole and accretion disk in collapse of massive stellar cores
Authors: Sekiguchi Yuichiro 
Published: September 2012

AbstractWe describe the results of our numerical simulations of the collapse of a massive stellar core to a BH, performed in the framework of full general relativity incorporating finite-temperature equation of state and neutrino cooling. We adopt a 100 M⊙ presupernova model calculated by Umeda & Nomoto (2008), which has a massive core with a high value of entropy per baryon. Changing the degree of rotation for the initial condition, we clarify the dependence of the outcome on this. When the rotation is rapid enough, the shock wave formed at the core bounce is deformed to be a torus-like shape. Then, the infalling matter is accumulated in the central region due to the oblique shock at the torus surface, hitting the hypermassive neutron star (HMNS) and dissipating the kinetic energy there. As a result, outflows can be launched. The HMNS eventually collapses to a BH and an accretion torus is formed around it. We also found that the evolution of the BH and torus depends strongly on the rotation initially given.
Temporal Evolution of GRB Spectra: Leptonic and Hadronic
Authors: Asano Katsuaki , Mészáros Peter 
Published: September 2012

AbstractAs the Fermi observatory has revealed, the GRB light curves show variant behaviours in different energy bands. Especially, the onset of GeV emission tend to lag that at lower energy. Various models to explain the GeV-delay, including early afterglow models or hadronic models, have been proposed. We have developed a time-dependent code for emission processes with one-zone approximation. The temporal evolution of GRB spectra is discussed based on leptonic inverse Compton and hadronic cascade models. This offers important predictions for future observations such as CTA.
Mass and metallicity constraints on supernova progenitors derived from integral field spectroscopy of the environment
Authors: Kuncarayakti Hanindyo , Doi Mamoru , Aldering Greg , Arimoto Nobuo , Maeda Keiichi , Morokuma Tomoki , Pereira Rui , Usuda Tomonori , Hashiba Yasuhito 
Published: September 2012

AbstractWe have obtained optical integral field spectroscopy of the explosion sites of more than 25 nearby type-IIP/IIL/Ib/Ic supernovae using UH88/SNIFS, and additionally Gemini/GMOS IFU. This technique enables us to obtain both spatial and spectral information of the immediate environment of the supernovae. Using strong line method we measured the metallicity of the star cluster present at the explosion site, presumably the coeval parent stellar population of the supernova progenitor, and comparison with simple stellar population models gives age estimate of the cluster. With this method we were able to put constraints on the metallicity and age of the progenitor star. The age, i.e. lifetime, of the progenitor corresponds to the initial mass of the star. By far this is the most direct measurement of supernova progenitor metallicity and, if the cluster-progenitor association is confirmed, provides reliable determination of the initial mass of supernova progenitor stars.
Trigger Simulations for GRB Detection with the Swift Burst Alert Telescope
Authors: Lien Amy , Sakamoto Takanori , Gehrels Neil , Palmer David , Graziani Carlo 
Published: September 2012

AbstractUnderstanding the intrinsic cosmic long gamma-ray burst (GRB) rate is essential in many aspects of astrophysics and cosmology, such as revealing the connection between GRBs, supernovae (SNe), and stellar evolution. Swift, a multi-wavelength space telescope, is quickly expanding the GRB category by observing hundreds of GRBs and their redshifts. However, it remains difficult to determine the intrinsic GRB rate due to the complex trigger algorithm adopted by Swift. Current studies of the GRB rate usually approximate the Swift trigger algorithm by a single detection threshold. Nevertheless, unlike the previously flown GRB instruments, Swift has over 500 trigger criteria based on count rates and additional thresholds for localization. To investigate possible systematic biases and further explore the intrinsic GRB rate as a function of redshift and the GRB luminosity function, we adopt a Monte Carlo approach by simulating all trigger criteria used by Swift. A precise estimation of the intrinsic GRB rate is important to reveal the GRB origins and their relation to the black-hole forming SNe. Additionally, the GRB rate at high redshifts provides a strong probe of the star formation history in the early universe, which is hard to measure directly through other methods.
GRB host galaxies: theoretical investigation
Authors: Mao Jirong 
Published: September 2012

AbstractLong gamma-ray bursts (GRBs) can be linked to the massive stars and their host galaxies are assumed to be the star-forming galaxies within small dark matter halos. We apply a galaxy evolution model, in which the star formation process inside the virialized dark matter halo at a given redshift is achieved. The star formation rates (SFRs) in the GRB host galaxies at different redshifts can be derived from our model. The related stellar masses, luminosities, and metalicities of these GRB host galaxies are estimated. We also calculate the X-ray and optical absorption of GRB afterglow emission. At higher redshift, the SFR of host galaxy is stronger, and the absorption in the X-ray and optical bands of GRB afterglow is stronger, when the dust and metal components are locally released, surrounding the GRB environment. These model predictions are compared with some observational data as well.
Carnegie Supernova Project: Spectroscopic Observations of Core Collapse Supernovae
Authors: Morrell Nidia I. 
Published: September 2012

AbstractThe Carnegie Supernova Project (CSP) has performed, during the period 2004-2009, the optical and NIR follow up of 253 supernovae (SNe) of all types. Among those, 124 were core collapse events, comprising 93 SNe of type II and 31 of types Ib/Ic/IIb. Our follow up consisted of photometric observations suitable to build detailed light curves and a considerable amount of optical spectroscopy.The bulk of our observations is carried out at Las Campanas Observatory, while access to other facilities is also provided thanks to our strong collaboration with the Millennium Center for Supernova Studies (MCSS).Our spectroscopic observations were primarily aimed at typing possible new SNe, and follow-up the evolution of CSP targets. One of the goals of the follow-up of type II SNe is the application of independent distance indicators such as the Standard Candle (SCM) and the Expanding Photosphere (EPM) methods. Moreover, through the study of the spectroscopic evolution of these objects, from as early as possible after explosion to the nebular phases, we hope to contribute to their further understanding. Specific analysis of particular objects is underway by members of the CSP and an extended collaboration.
Numerical code of the neutrino-transfer in three dimensions for core-collapse supernovae
Authors: Sumiyoshi Kohsuke , Yamada Shoichi 
Published: September 2012

AbstractWe develop a new numerical code of the multi-energy and multi-angle neutrino-radiation transfer in three dimensions (3D) for core-collapse supernovae. Our 3D code to solve the Boltzmann equations is based on the discretized-ordinate (SN) method with a fully implicit differencing for time advance. A basic set of neutrino reactions is implemented in the collision terms together with a realistic equation of state. By following the time evolution of neutrino distributions in six dimensions (3 spatial and 3 momentum-space) by the 3D Boltzmann solver, we study the 3D feature of neutrino transfer for given background models of supernova cores in order to understand the explosion mechanism through neutrino heating in multi dimensions.
Magnetic Energy Release in Relativistic Plasma
Authors: Takahashi Hiroyuki R. , Ohsuga Ken 
Published: September 2012

AbstractThe efficiency of the energy conversion rate in the relativistic magnetic reconnection is investigated by means of Relativistic Resistive Magnetohydrodynamic (R2MHD) simulations. We confirmed that the simple Sweet-Parker type magnetic reconnection is a slow process for the energy conversion as theoretically predicted by Lyubarsky (2005). After the Sweet-Parker regime, we found a growth of the secondary tearing instability in the elongated current sheet. Then the energy conversion rate and the outflow velocity of reconnection jet increase rapidly. Such a rapid energy conversion would explain the time variations observed in many astrophysical flaring events.To construct a more realistic model of relativistic reconnection, we extend our R2MHD code to R3MHD code by including the radiation effects (Relativistic Resistive Radiation Magnetohydrodynamics R3MHD). The radiation field is described by the 0th and 1st moments of the radiation intensity (Farris et al. 2008, Shibata et al. 2011). The code has already passed some one-dimensional and multi-dimensional numerical problems. We demonstrate the first results of magnetic reconnection in the radiation dominated current sheet.
Shock Breakout of Type II Plateau Supernova
Authors: Tominaga Nozomu , Morokuma Tomoki , Blinnikov Sergei I. 
Published: September 2012

AbstractType II-plateau supernovae (SNe II-P) are fainter than Type Ia SNe and thus have so far been observed only at z < 1. We introduce shock breakout and propose a distant SN II-P survey at z > 1 with shock breakout. The first observation of shock breakout from the rising phase is reported in 2008. We first construct a theoretical model reproducing the UV-optical light curves (LCs) of the first example and demonstrate that the peak apparent g-band magnitude of the shock breakout would be mg ~ 26.4 mag if an identical SN occurs at a redshift z = 1, which can be reached by 8m-class telescopes. Furthermore, we present LCs of shock breakout of SN explosions with various main-sequence masses, metallicities, and explosion energies and derive the observable SN rate and reachable redshift as functions of filter and limiting magnitude by taking into account an initial mass function, cosmic star formation history, intergalactic absorption, and host galaxy extinction. The g-band observable SN rate with limiting magnitude 27.5 mag is 3.3 SNe deg−2 day−1 and half of them are located at z > 1.2.
Fate of most massive stars
Authors: Yusof Norhasliza , Hirschi Raphael , Kassim Hasan Abu 
Published: September 2012

AbstractThe first generations of stars are thought to have been more massive than Pop I stars and therefore some of these are thought to have produced pair creation supernovae (PCSNe) at the end of their life. However, the chemical signature of PCSNe is not observed in extremely metal poor stars (e.g. Umeda and Nomoto 2002) and it raises the following questions: Were stars born less (or more massive) than the mass range expected to lead to the PCSNe? Or was mass loss too strong during the evolution of these stars and prevented them from retaining enough mass to produce PCSNe? The discovery of very massive stars (VMS, M > 100 M⊙) in the Milky Way and LMC (Crowther et al. 2010) shows that VMS can form and exist. The observations of PCSN candidates (2006gy & 2007bi) also seems to indicate that such SNe may occur. Mass loss plays a crucial role in the life of VMS since the star will only die as a PCSN if the star retains a high mass throughout its life. In this paper, we shall describe the dependence of VMS evolution on metallicity and present stellar evolution models at various metallicities, including the effects of mass loss and rotation. Based on our models, we will give our predictions concerning the fate of these VMS, either a PCSN or SNIc (possibly GRBs in some cases) as a function of metallicity.
East Pacific ocean eddies and their relationship to subseasonal variability in Central American wind jets
Authors: Chang Chueh‐Hsin , Xie Shang‐Ping , Schneider Niklas , Qiu Bo , Small Justin , Zhuang Wei , Taguchi Bunmei , Sasaki Hideharu , Lin Xiaopei 
Published: September 2012

Subseasonal variability in sea surface height (SSH) over the East Pacific warm pool off Central America is investigated using satellite observations and an eddy‐resolving ocean general circulation model. SSH variability is organized into two southwest‐tilted bands on the northwest flank of the Tehuantepec and Papagayo wind jets and collocated with the thermocline troughs. Eddy‐like features of wavelength ∼600 km propagate southwestward along the high‐variance bands at a speed of 9–13 cm/s. Wind fluctuations are important for eddy formation in the Gulf of Tehuantepec, with a recurring interval of 40–90 days. When forced by satellite wind observations, the model reproduces the two high‐variance bands and the phase propagation of the Tehuantepec eddies. Our observational analysis and model simulation suggest the following evolution of the Tehuantepec eddies. On the subseasonal timescale, in response to the gap wind intensification, a coastal anticyclonic eddy forms on the northwest flank of the wind jet and strengthens as it propagates offshore in the following two to three weeks. An energetics analysis based on the model simulation indicates that besides wind work, barotropic and baroclinic instabilities of the mean flow are important for the eddy growth. Both observational and model results suggest a re‐intensification of the anticyclonic eddy in response to the subsequent wind jet event. Off Papagayo, ocean eddy formation is not well correlated with local wind jet variability. In both the Gulfs of Tehuantepec and Papagayo, subseasonal SSH variability is preferentially excited on the northwest flank of the wind jet. Factors for this asymmetry about the wind jet axis as well as the origins of wind jet variability are discussed.
Regulation of the V-type ATPase by redox modulation
Authors: Seidel Thorsten , Scholl Stefan , Krebs Melanie , Rienmüller Florian , Marten Irene , Hedrich Rainer , Hanitzsch Miriam , Janetzki Patricia , Dietz Karl-Josef , Schumacher Karin 
Published: September 2012

ATP-hydrolysis and proton pumping by the V-ATPase (vacuolar proton-translocating ATPase) are subject to redox regulation in mammals, yeast and plants. Oxidative inhibition of the V-ATPase is ascribed to disulfide-bond formation between conserved cysteine residues at the catalytic site of subunit A. Subunits containing amino acid substitutions of one of three conserved cysteine residues of VHA-A were expressed in a vha-A null mutant background in Arabidopsis. In vitro activity measurements revealed a complete absence of oxidative inhibition in the transgenic line expressing VHA-A C256S, confirming that Cys256 is necessary for redox regulation. In contrast, oxidative inhibition was unaffected in plants expressing VHA-A C279S and VHA-A C535S, indicating that disulfide bridges involving these cysteine residues are not essential for oxidative inhibition. In vivo data suggest that oxidative inhibition might not represent a general regulatory mechanism in plants.
Nitric oxide and glucocorticoids synergize in inducing apoptosis of CD4+8+ thymocytes: implications for ‘Death by Neglect’ and T-cell function
Authors: Cohen Orly , Ish-Shalom Eliran , Kfir-Erenfeld Shlomit , Herr Ingrid , Yefenof Eitan 
Published: September 2012

Abstract
Thymic epithelial cells (TECs) play a central role in T-cell development by presenting self-antigens on MHC proteins. Double-positive (DP) thymocytes that fail to interact with TEC via their TCR die by ‘Death by Neglect’. We demonstrated a role for TEC-derived glucocorticoids (GCs) in this process. In a previous study, we used an in vitro system recapitulating Death by Neglect, to demonstrate the involvement of nitric oxide (NO) and inducible NO synthase (iNOS) in this process. In this study, we show that NO synergizes with GCs to induce apoptosis of DP thymocytes in a fetal thymic organ culture. Also, DP thymocytes from iNOS−/− mice are less sensitive to GC-induced apoptosis. Furthermore, the number of DP thymocytes in iNOS−/− mice is higher than in wild-type mice, suggesting a role for NO in Death by Neglect. This phenomenon effects T-cell function profoundly: iNOS−/− T cells do not respond to TCR-mediated activation signals, measured by up-regulation of CD69, IL-2R and IFNγ secretion. This failure to activate is a result of TCR incompetence because iNOS−/− T cells respond to TCR-independent stimuli (phorbol myristate acetate and calcium ionophore). This study suggests that NO and GCs synergize to execute TEC-induced death of DP thymocytes.
Differences in Alcohol‐Soluble Protein from Genetically Altered Wheat Using Capillary Zone Electrophoresis, One‐ and Two‐Dimensional Electrophoresis, and a Novel Gluten Matrix Association Factor Analysis
Authors: Robertson George H. , Hurkman William , Anderson Olin D. , Tanaka Charlene K. , Cao Trung K. , Orts William J. 
Published: September 2012

ABSTRACTWheat protein composition and organization play interrelated roles in determining physical properties for technological purposes. In prior research, a number of isogenic wheat lines of Bobwhite that have high levels of expression of the native Dx5 and/or Dy10 high‐molecular‐weight glutenin subunits (HMW‐GS) were examined vis‐à‐vis physical properties related to separation. In particular, these altered lines were characterized by poor mixing properties, the formation of mixtures in water that could not be separated by conventional mechanical methods, reduced water absorption, unique milling properties, and severely limited development of microscopic fibrils. These attributes suggested inherent organizational differences at submicroscopic and molecular levels among the various lines. Therefore, proteins were fractionated from whole meals using 70% ethanol to elucidate solubility characteristics and compositions and to infer structural properties. Capillary zone electrophoresis and one‐ and two‐dimensional SDS‐PAGE (2DE) revealed striking differences in the protein composition and solubility among these new lines and the Bobwhite from which they were derived. Generally, Bobwhite yielded soluble protein that included not only what would be considered as classical gliadins but also some of each of the HMW‐GS as monomers or polymers with low degrees of polymerization, whereas the genetically altered lines produced far less total soluble protein and very limited amounts of HMW‐GS. In the extreme, high levels of expression of Dx5 subunit not only led to reduced solubility of the HMW‐GS but also limited the solubility of the many other proteins that are normally soluble. In addition, a matrix association factor similar to the classical separation factor of analytical chemistry and chemical engineering was introduced and applied to 2DE data for insoluble and soluble protein to summarize and index relative involvement of specifically enhanced proteins in the insoluble gluten matrix after equilibration with ethanol. The highest relative association was determined for the HMW‐GS lines enriched in Dx5 or Dy10 protein and the lowest for Bobwhite. Greater association was indicated for Dx5 than for Dy10 protein in these lines. The value of the association factor was likely influenced by differences in glutamine‐to‐cysteine ratios and differences in altered glutenin chain configurations stemming from high levels of expression of a single or limited number of HMW‐GS.
Oral bioavailability of dabigatran etexilate (Pradaxa®) after co‐medication with verapamil in healthy subjects
Authors: Härtter Sebastian , Sennewald Regina , Nehmiz Gerhard , Reilly Paul 
Published: September 2012

AimTo investigate the effect of the P‐glycoprotein inhibitor verapamil on the pharmacokinetics and pharmacodynamics of dabigatran etexilate (DE).MethodIn this two part multiple crossover trial in 40 healthy subjects, DE 150 mg was given alone or with verapamil at different doses, duration of treatment (single vs. multiple dosing), formulations, and timings (before, concurrently or after DE). Primary pharmacokinetic endpoints were determined from concentrations of total dabigatran (unconjugated plus conjugated). Pharmacodynamic endpoints were determined from clotting time.ResultsThe greatest effect was observed with single dose verapamil 120 mg immediate release given 1 h before single dose DE. Geometric mean area under the plasma concentration curve [AUC(0,∞)] and maximum analyte concentration in the plasma (Cmax) were increased by 143% [90% confidence interval (CI) 91, 208] and 179% (90% CI 115, 262), respectively. The effect was reduced to a 71% and 91% increase in AUC and Cmax, respectively, when DE was administered with verapamil 240 mg extended release. After multiple verapamil dosing, DE AUC(0,∞) and Cmax increases were 54% and 63%, respectively. However, DE given 2 h before verapamil increased DE AUC(0,∞) and Cmax by <20%. With regard to clotting prolongation, the dabigatran plasma concentration–effect relationship was generally not affected by the co‐administration of verapamil. Concomitant administration of DE and verapamil did not reveal any unexpected safety findings.ConclusionVerapamil increased DE bioavailability, likely due to inhibition of P‐glycoprotein. Our results suggest that an interaction between verapamil and DE can be minimized if DE is administered 2 h prior to verapamil.