Interaksi Neutrino dengan Elektron di Atmosfir Supernova = Neutrino Interaction with Electron in Supernova Atmosphere
| Main Authors: | Listiana Satiawati, author, Add author: Anto Sulaksono, supervisor, Add author: Mart, Terry, examiner, Add author: Agus Salam, examiner, Add author: Imam Fachruddin, examiner |
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| Format: | Masters Bachelors |
| Terbitan: |
, 2011
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| Subjects: | |
| Online Access: |
https://lib.ui.ac.id/detail?id=20341264 |
Daftar Isi:
- [<b>ABSTRAK</b><br> Telah dihitung polarisasi, penampang lintang diferensial dan jalan bebas rata-rata pada interaksi neutrino-gas elektron dengan mempertimbangkan faktor bentuk elektromagnetik neutrino, untuk temperatur berhingga. Faktor- faktor yang dipertimbangkan pada perhitungan adalah retardasi, detail ba- lans dan Pauli bloking serta anti partikel. Efek banyak benda masuk dalam perhitungan polarisasi melalui pendekatan korelasi fase random ( random phase approximation ) dan massa foton efektif. Hasil yang didapat digunakan untuk mempelajari interaksi neutrino dengan materi pada atmosfir supernova. Hasil penelitian ini menunjukkan seberapa besar pengaruh faktor-faktor temperatur, kerapatan elektron, momen dipol neutrino, jari-jari muatan neu- trino, korelasi random phase approximation, massa foton efektif dan korek- si relativitas umum pada jalan bebas rata-rata neutrino pada atmosfir su- pernova. <hr> <b>ABSTRACT</b><br> The polarizations, differential cross section and mean free path of neutrino- electron gas interaction have been calculated by taking into account the neu- trino electromagnetic form factor, for finite temperature. The retarded, de- tailed balance, Pauli blocking and anti-particle factors have been also taken into account in the calculations. Many-body effects enter into polarizations calculations through random phase approximation correlation and photon effective mass. The results are used to study the interaction of neutrino with matter in supernova atmosphere. It has also shown how large the influence of temperature, electron density, neutrino moment dipole, neutrino charge radius, random phase approxi- mation correlation, photon effective mass and general relativity correction in mean free path at supernova atmosphere.;The polarizations, differential cross section and mean free path of neutrino- electron gas interaction have been calculated by taking into account the neu- trino electromagnetic form factor, for finite temperature. The retarded, de- tailed balance, Pauli blocking and anti-particle factors have been also taken into account in the calculations. Many-body effects enter into polarizations calculations through random phase approximation correlation and photon effective mass. The results are used to study the interaction of neutrino with matter in supernova atmosphere. It has also shown how large the influence of temperature, electron density, neutrino moment dipole, neutrino charge radius, random phase approxi- mation correlation, photon effective mass and general relativity correction in mean free path at supernova atmosphere., The polarizations, differential cross section and mean free path of neutrino- electron gas interaction have been calculated by taking into account the neu- trino electromagnetic form factor, for finite temperature. The retarded, de- tailed balance, Pauli blocking and anti-particle factors have been also taken into account in the calculations. Many-body effects enter into polarizations calculations through random phase approximation correlation and photon effective mass. The results are used to study the interaction of neutrino with matter in supernova atmosphere. It has also shown how large the influence of temperature, electron density, neutrino moment dipole, neutrino charge radius, random phase approxi- mation correlation, photon effective mass and general relativity correction in mean free path at supernova atmosphere.]