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| 1 | Brain-computer interfaces for space applications 显示文摘 | Negue ruela Cristina Broschart Michael Menon | 2011 | Personal and Ubiquitous Computing2011，15，5： | 1 |
| 2 | Isolation and identi cation of antioxidative peptides from bovine a -lactalbumin显示文摘 | Le la Sadat C e line Cakir-Kiefer Marie-Andr e e N' Negue | 2011 | International Dairy Journal2011，21，： | 1 |
| 3 | Isolation and identification of anti-oxidative peptides from bovine a-lactalbumin 显示文摘 | Lella Sadat C61ine Cakir-Kiefer Marie-Andrre N' Negue | 2011 | International Dairy Journal2011，21，4： | 1 |
| 4 | Isolation and identification of antioxidative peptides from bovine α-lactalbumin显示文摘 | Sadat L Cakir-Kiefer C N'Negue M A Gaillard J L Girardet J M Miclo L | 2011 | International Dairy Journal2011，21，： | 1 |
| 5 | Biological oxidation of arsenite : batch reactor experiments in presence of kutnahorite and chabazite 显示文摘 | LIE 'VREMONT D N'NEGUE M A BEHRA P | 2003 | Chemosphere2003，51，： | 1 |
| 6 | Effects of dynamo magnetic fields on observational properties of accreting millisecond X-ray pulsars显示文摘In this paper,we have investigated accreting millisecond X-ray pulsars,which are rapidly rotating neutron stars in low-mass X-ray binaries.These systems exhibit coherent X-ray pulsations that arise when the accretion flow is magnetically channeled to the stellar surface.Here,we have developed the fundamental equations for an accretion disk around accreting millisecond X-ray pulsars in the presence of a dynamo generated magnetic field in the inner part of the disk.We have also formulated the numerical method for the structure equations in the inner region of the disk and the highest accretion rate is enough to form the inner region of the disk,which is overpowered by radiation pressure and electron scattering.Finally,we have examined our results with the effects of dynamo magnetic fields on accreting millisecond X-ray pulsars. | Dugasa Belay Zeleke Solomon Belay Tessema Seblu Humne Negu | 2021 | Research in Astronomy and Astrophysics2021，21，1： | 1 |
| 7 | Peraluminous granitoids within the Hangloa area,Adamawa-YadéDomain,Cameroon:Petrogenesis and tectonic implication显示文摘Hangloa granitoids form part of the wide range calc-alkaline Pan-African granitic suites within the Adamawa Yade Domain(AYD)in Cameroon.There are several reports on metaluminous granitoids within this domain.The peraluminous suite has been locally reported and their petrogenesis is not fully understood.Petrography and whole-rock geochemistry were used to study the petrogenesis/formation of granitic rocks within this area.The results show that the granitoids are composed of quartzo-feldspathic,made up of granites,monzonites and quartz monzonites which were intruded in the Paleoproterozoic orthogneissic basement.The major and trace element compositions show that they are high-K calc-alkaline to shoshonites,with S-type affinity.The molar ratio A/CNK is>1.1,while the ratio of CaO+Na_(2)O/Al_(2)O_(3) is generally<1 making them strongly peraluminous.The REE shows enrichment in the LREE over the HREE,with(La/Yb)N varying from 11.9 to 53.32,(Dy/Yb)N from 0.77 to 2.13 and moderately negative Eu anomaly((Eu/Eu^(*))N range from 0.42 to 0.93).Most granite samples show depletion in P,with CaO/Na_(2)O<0.3 and Rb/Sr≤1 indicative of clay-poor metapelitic source,while the others show clay-rich metagreywackes sources.The strong peraluminosity,S-type affinity,high Ba/Sr,Ba/Rb and low Rb/Sr indicate they are crustal-derived.The compositional variation might be induced by the partial melting of different source materials followed by fractional crystallization of the granitic magma.The source nature requires fragments of Paleoproterozoic metasedimentary and metaigneous rocks derived from the collision between the north-central Cameroon block and the Congo Craton during the Pan-African. | Yaya Fodoué Mero Yannah Rigobert Tchameni Wadjou Jacques Wassouo Amadou Diguim Kepnamou Joseph Penaye Abakar Mahamat Emmnuel Nomo Negue | 2022 | Acta Geochimica2022，41，6： | 0 |
| 8 | Physical Parameters of W UMa Type Contact Binaries and Their Stability of Mass Transfer显示文摘In this study,we determined the physical parameters of W UMa type contact binaries and their stability of mass transfer with different stellar mass ranges over a broad space by applying the basic dynamical evolution equations of the W UMa type contact binaries using accretor and donor masses between 0.079 and 2.79 M_(⊙).In these systems,we have studied the three subclasses of W UMa systems of A-,B-and W-type contact binaries using the initial and final mass ranges and we investigated different stellar and orbital parameters for the subclasses of W UMa systems.We examined the stability of the W UMa type contact binaries using the orbital parameters such as critical mass ratio,Roche lobe radius of the donor star and mass ratio of these systems.Thus,we computed the observed and calculated physical parameters of A-,B-and W-type W UMa systems.Moreover,we determined the combined and color temperatures to classify the three subclasses of the systems.Also,we presented the result of the internal stellar structure and evolution of W UMa type contact binaries by using the polytropic model. | Berikol Tekeste Gebreyesus Seblu Humne Negu | 2023 | Research in Astronomy and Astrophysics2023，23，4： | 0 |
| 9 | Evolution of Close Binary System Parameter Distributions显示文摘In this paper,we investigate the orbital and stellar parameters of low-and intermediate-mass close binary systems.We use models,presented in the catalog of Han et al.and calculate parameters of accretors.We also construct distributions of systems along luminosity,semimajor axis and angular momentum,and make some conclusions on their evolution with time.We compare the results with observational data and it shows a good agreement.The set of theoretical models published quite adequately describes the observational data and,consequently,can be used to determine the evolutionary path of specific close binary systems,their initial parameter values and final stages. | Dugasa Belay Zeleke Seblu Humne Negu Oleg Yu.Malkov | 2022 | Research in Astronomy and Astrophysics2022，22，10： | 0 |
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