پديد آورنده :
محمدي، روح ا...
عنوان :
بررسي برهمكنش ذرات بنيادي در حضور ميدان هاي زمينه
محل تحصيل :
اصفهان: دانشگاه صنعتي اصفهان، دانشكده فيزيك
صفحه شمار :
ده،193ص.: مصور،جدول،نمودار
يادداشت :
ص.ع.به فارسي و انگليسي
استاد راهنما :
منصور حقيقت
توصيفگر ها :
فضاي ناجابجايي , تابع تبا , ميدان مغناطيسي , ستاره نوتروني , فاكتورژيرومغناطيسي , نرخ گسيل نوترينوها تابش زمينه كيهاني GMB
تاريخ نمايه سازي :
29/8/90
استاد مدعو :
محمد زبرجد، نداصدوقي
كد ايرانداك :
ID401 دكتري
چكيده فارسي :
به فارسي و انگليسي: قابل رويت در نسخه ديجيتالي
چكيده انگليسي :
The Interaction of Elementary Particles in Presence of Background Fields Rohoollah Mohammadi E mail r mohammadi@ph iut ac ir Date of Submission September 18 2011 Department of Physics Isfahan University of Technology Isfahan 84156 83111 IranSupervisor Mansour Haghighat mansor@cc iut ac irAdvisor Farhang Loran IsfahaniDepartment Graduate Program Coordinator Farhad ShahbaziAbstractIn this thesis we will investigate the effects of non commutative and magnetic field as back groundfield on the some most important interactions of elementary particles In non commutative case wewill show that by considering QCD and QED interactions together Beta function of NCQED canobtain zero negative and plus values In case of back ground magnetic field we will study andcalculate the effects of weak ordinary and strong magnetic field on some physical systems Forstrong magnetic field we calculate the probably effects of this magnetic field on distributions ofnucleons and electrons as constituent particles of neutron star and show the ratio number neutrons tonumber protons reduce in presence of magnetic field Also we will obtain the electric potential andelectric fields by using Thomas Fermi equation modified Poisson equation for complete degeneracysystem of electrons and nucleons and then we will show the electric field in presence of magneticfield increases at surface of neutron star Farther more we will see the maximum electron Fermienergy to keep all of electron in side of neutron star in magnetic field have the same value with thecase without magnetic field Finally we will investigate the effects of strong magnetic field forcooling step of neutron star spatially we will calculate neutrino emissivity in during NN NN process and we will see this quantity increases in presence of strong magneticfield this process is one of most important for cooling step for example when the magnetic field is NN about 1016 Gauss the rate lost energy by NN grows up to one order magnitude Forweak magnetic field we will try to consider the effects of very weak magnetic about micro gauss present in back ground cosmic on the polarization of cosmic microwave background CMB and forthis case we will show magnetic field due to produce circular polarization for CMB photons whereasin order to produce circular polarization doesn t need primary linear polarization for CMB photonsand the end we will obtain a value about for Faraday conversion phase shift in presence of magneticfield Finally for ordinary magnetic field we will consider the effects of magnetic field present inexperience to measure electron and muon g factor on electron and muon magnetic moment and wewill obtain a correction about 10 12 for electron g factor and a correction about 10 9 for muong factor from transformed momentum due to background magnetic field Keywords Background Fields Non commutative Space Time Magnetic Field Beta Function Neutron Star Thomas Fermi Equation Cooling Step CMB Photons Circular Polarization Electron and Muon g Factors
استاد راهنما :
منصور حقيقت
