پديد آورنده :
باورساد، احسان
عنوان :
فرآيندهاي ذرات در ميدان مغناطيسي زمينه
محل تحصيل :
اصفهان: دانشگاه صنعتي اصفهان، دانشكده فيزيك
صفحه شمار :
[10]،133ص.: جدول،نمودار
يادداشت :
ص.ع.به فارسي و انگليسي
استاد راهنما :
منصور حقيقت
توصيفگر ها :
قطبش دايره اي تابش CMB , ستاره نوتروني , پراكندگي نوكلئون-نوكلئون , تابندگي نوترينو , رمبش گرانشي و نوترينوهاي پرانرژي
تاريخ نمايه سازي :
26/1/91
استاد مدعو :
ندا صدوقي، ياسمن فرزان
كد ايرانداك :
ID417 دكتري
چكيده فارسي :
به فارسي و انگليسي: قابل رويت در نسخه ديجيتالي
چكيده انگليسي :
Particle Processes in a Magnetic Field Background Ehsan Bavarsad ehsan@ph iut ac ir January 16 2012 Department of Physics Isfahan University of Technology Isfahan 84156 83111 IranMansour Haghighat supervisor mansour@cc iut ac irFarhang Loran advisor loran@cc iut ac irAbstractIn this thesis we have shown that corrections due to the magnetic field background can producecircular polarization in CMB photons The nucleon nucleon scattering in a large magneticbackground is considered to find its potential to change the neutrino emissivity of the neutronstars For this purpose we consider the one pion exchange approximation to find the nucleon nucleon cross section in a background field as large as 1015 1018G We show that the nucleon nucleon cross section in neutron stars with temperatures in the range 0 1 5MeV can be changedup to the 1 order of magnitude with respect to the one in the absence of the magnetic field Around B 1018G the emissivity changes about an order of magnitude with respect to itscorresponding value without magnetic field Furthermore the enhancement on the emissivity ishigher for the lower temperatures We show that corrections due to magnetic field in speed ofneutrino are much smaller than anomaly reported by OPERA experiment By obtaining themixing angle and square mass difference in large magnetic field of neutron star we show thatthis magnetic field cannot be larger than 1016G We show that the Lorentz violation parameterssuch as c and d can be generated by the magnetic background We obtain c and d of theorder of 10 27 for a neutrino we also obtain H of the order of 10 36 eV for an electron neutrinoand d around 10 17 for electron in a magnetic background about 1G Although the obtainedresults for neutrino is far from the experimental bounds the magnetic field can produce theelectron d parameter as large as the current experimental bounds on this parameter We havestudied gravitational collapse of a compact star as a complete degenerate Fermi gas of neutrons protons and electrons We find fluxes of 10MeV electron neutrinos and GeV electron and muonflavor neutrinos The ratio of total muon flavor neutrinos to the total electron flavor neutrinos iscomputed at the source and after oscillation effects at the Earth which is less than 1 We findthat number of GeV antineutrino events in an ordinary detector such as Kamiokande is graterthan 1 and total energy of neutrino flux is larger than 1052erg Key Words Magnetic field background Circular polarization of the CMB radiation Neutron star Nucleon nucleon scattering Neutrino emissivity Speed of neutrino Neutrino oscillation Gravitational collapse High energy neutrinos Department of Physics Isfahan University of Technology Isfahan 84156 83111 Iran
استاد راهنما :
منصور حقيقت
