NUCLEAR AND PARTICLE ASTROPHYSICS

International Teaching NUCLEAR AND PARTICLE ASTROPHYSICS

0522600056
DEPARTMENT OF PHYSICS "E. R. CAIANIELLO"
EQF7
PHYSICS
2021/2022

YEAR OF COURSE 2
YEAR OF DIDACTIC SYSTEM 2017
SECONDO SEMESTRE
CFUHOURSACTIVITY
648LESSONS
Objectives
THE COURSE IS FOCUSED ON THE ROLE OF NUCLEAR AND ASTROPARTICLE PHYSICS IN ASTROPHYSICS.

KNOWLEDGE AND UNDERSTANDING:
STUDENTS WILL ACHIEVE A GOOD GENERAL KNOWLEDGE OF THE ROLE OF NUCLEAR AND PARTICLE PHYSICS PROCESSES IN ASTROPHYSICAL ENVIRONMENTS. EXPERIMENTAL METHODS USED TO GATHER INFORMATION OF THE RELEVANT MICROSCOPIC PROCESSES IN ASTROPHYSICS WILL BE DESCRIBED, AND EMPHASIS WILL BE GIVEN TO THE LINK TO OBSERVATIONAL DATA, IN PARTICULAR THOSE ARISING FROM MULTIMESSENGER ASTRONOMY.

APPLYING KNOWLEDGE AND UNDERSTANDING:
STUDENTS WILL BE TRAINED THROUGH A SIMPLIFIED CALCULATION OF THE STELLAR RATES DURING HYDROGEN AND HELIUM BURNING STAGES AND THE COMPARISON TO POBSERVATIONAL DATA (SOLAR NEUTRINO ENERGY SPECTRUM AND WHITE DWARF COMPOSITION). IN ADDITION, THE STUDY OF THE SPECIFICATIONS AND STRUCTURE OF SOME DETECTORS SELECTED FOR THEIR RELEVANCE IN THE FIELD OF MULTIMESSENGER ASTRONOMY WILL BE PROPOSED.
Prerequisites
THE COURSE REQUIRES A GOOD KNOWLEDGE OF QUANTUM MECHANICS AND BASIC EXPERIMENTAL TECHNIQUES IN NUCLEAR AND SUBNUCLEAR PHYSICS.
Contents
1. NUCLEOSYNTHESIS AND STELLAR EVOLUTION (4h)
OBSERVATIONAL DATA. INTRODUCTION TO COSMOLOGY. STAR FORMATION. PHYSICS BASIS OF STELLAR EVOLUTION: EQUATION OF STATE. ENERGY PRODUCTION AND TRANSPORT. STELLAR EVOLUTION. QUIESCENT BURNING. EXPLOSIVE SCENARIOS. STELLAR MODELS.
2. NUCLEAR REACTIONS IN ASTROPHYSICAL ENVIRONMENT (4h)
CHARACTERISTIC QUANTITIES AND PROPERTIES OF NUCLEAR REACTIONS. CHARGED PARTICLE INDUCED NUCLEAR REACTIONS. NEUTRON INDUCED NUCLEAR REACTIONS. NUCLEAR REACTIONS IN ASTROPHYSICAL PLASMAS.
3. NUCLEOSYNTHESIS (4h)
BIG BANG NUCLEOSYNTHESIS. STELLAR NUCLEOSYNTHESIS. HYDROGEN AND HELIUM BURNINGS. ADVANCED BURNINGS. R-, S-, AND P- PROCESSES. EXPLOSIVE NUCLEOSYNTHESIS. CHEMICAL EVOLUTION OF GALAXIES.
4. EXPERIMENTAL NUCLEAR ASTROPHYSICS. (4h)
DIRECT MEASUREMENTS IN NUCLEAR ASTROPHYSICS: ACCELERATORS, TARGETS, DETECTORS. RADIOACTIVE ION BEAMS. INDIRECT METHODS. DATA ANALYSIS. EXTRAPOLATIONS.
5.ASTROPARTICLE PHYSICS (4h)
BRIEF HISTORICAL INTRODUCTION. THE DISCOVERY OF COSMIC RAYS. COMPLEMENTARITY WITH PARTICLE PHYSICS. ASTRONOMY WITH THE MULTI-MESSENGER APPROACH.
6.THE COSMIC RAYS AND OUR GALAXY (4h)
FLUX AND SPECTRUM OF COSMIC RAYS. THE PHYSICAL PROPERTIES OF OUR GALAXY.
7.THE DIRECT REVELATION OF COSMIC RAYS: PROTONS, NUCLEI, ELECTRONS AND ANTI-MATTER. (4h)
METHODS OF DETECTION AND TYPES OF EXPERIMENTS
8.INDIRECT REVELATION OF COSMIC RAYS: PARTICLE SWARMS IN THE ATMOSPHERE. (4h)
METHODS OF DETECTION AND TYPES OF EXPERIMENTS
9.THE SPREAD OF COSMIC RAYS IN THE GALAXY AND ACCELERATION MECHANISMS (4h)
THE DIFFUSION EQUATIONS. THE FERMI MECHANISM. THE SHAPE OF THE SPECTRUM OF COSMIC RAYS (I.E. SPECTRAL INDICES).
10.NOTES ON THE COSMIC RAYS OF VERY HIGH ENERGY (2h)
11.THE SKY SEEN THROUGH GAMMA RAYS. (2h)
GAMMA RAY PRODUCTION MECHANISMS AND DETECTION METHODS
12.ASTRONOMY WITH HIGH-ENERGY NEUTRINOS. (2h)
PRODUCTION MECHANISMS. DETECTION METHODS: CERENKOV LIGHT, RADIO WAVES, ACOUSTIC WAVES.
13.THE DISCOVERY OF GRAVITATIONAL WAVES (2h)
14.THE MULTI-MESSENGER APPROACH: ADVANTAGES AND FIRST RESULTS (2h)
Teaching Methods
THE COURSE IS BASED ON LECTURES, TOTAL 48 HOURS. ATTENDING LECTURES IS NOT MANDATORY, BUT STRONGLY RECOMMENDED. TWO HOURS OF INDIVIDUAL STUDY FOR EACH HOUR OF LECTURE ARE ON AVERAGE NECESSARY TO FOLLOW THE COURSE WITH PROFIT.
Verification of learning
THE ASSESSMENT OF THE COMPETENCE OF STUDENTS WILL BE BASED ON AN ORAL TEST AND ON THE PRESENTATION OF THE RESULTS OF AN INDIVIDUAL STUDY. THE ORAL TEST WILL CONSIST IN AN INTERVIEW (APPROX. 60 MIN) ON THE CONTENTS OF THE COURSE PROGRAM. THE INDIVIDUAL STUDY WILL TYPICALLY BE FOCUSED ON THE ROLE OF NUCLEAR PROCESSES IN A SELECTED ASTROPHYSICAL SCENARIO AND THE IMPACT OF THE UNCERTAINTY IN THEIR EXPERIMENTAL DETERMINATION OF THE RELEVANT NUCLEAR QUANTITIES.
A BASIC KNOWLEDGE OF THE COURSE PROGRAMME IS REQUIRED TO PASS THE EXAMINATION. THE MAXIMUM RATING REQUIRES THE ABILITY OF FACING CASES NOT EXPLICITLY INCLUDED IN THE PROGRAMME, BUT FULLY APPROACHABLE WITH THE PROVIDED INFORMATION.
Texts
CAULDRONS IN THE COSMOS, C.E. ROLFS AND RODNEY
PRINCIPLES OF STELLAR EVOLUTION AND NUCLEOSYNTHESIS, D.D. CLAYTON.
PARTICLES AND ASTROPHYSICS: A MULTI-MESSENGER APPROACH, M. SPURIO
NUCLEAR PHYSICS OF STARS, C. ILIADIS (OPTIONAL)
  BETA VERSION Data source ESSE3