EXPLOSIVE STELLAR PHENOMENA - 2017/8

Module code: PHYM052

Module provider

Physics

Module Leader

LOTAY GJ Dr (Physics)

Number of Credits

15

ECT Credits

7.5

Framework

FHEQ Level 7

JACs code

F370

Module cap (Maximum number of students)

N/A

Module Availability

Semester 2

Overall student workload

Lecture Hours: 11

Tutorial Hours: 11

Assessment pattern

Assessment type Unit of assessment Weighting
Examination CLOSED BOOK FORMAL 1.5 HOUR EXAMINATION 70
Coursework COMPUTATIONAL PROJECT 30

Alternative Assessment

N/A

Prerequisites / Co-requisites

Module overview

This module aims to provide an advanced level understanding of explosive nuclear astrophysics and the physics of stars. In particular, the course will provide an analytical underpinning of resonant reaction rates, together with the experimental techniques involved in their determination, as well as a theoretical treatment of nuclear reactions and celestial objects.

Module aims

Provide an understanding of the underlying physics behind the formation of stars and stellar evolution.

Provide an understanding of explosive stellar phenomena, such as novae, supernovae and x-ray bursts, including the underlying nuclear physics processes involved that result in observational data

Provide an analytical treatment of resonant stellar reaction rates for both narrow and broad resonance contributions, together with a detailed understanding of the modern experimental and theoretical techniques used in obtaining the key nuclear physics information required.

Provide an understanding of astroparticle physics, such as neutrino oscillations, dark energy and direct dark matter detection

Learning outcomes

Attributes Developed
The student will be knowledgeable about current stellar models and will be able to describe how stars of different masses are born and evolve in time. The student will understand the Hertzsprung-Russell diagram. The student will identify the different density and temperature regimes occurring inside stars and will be aware of how dense quantum fluids and extremely hot relativistic gases impact stellar properties.
The student will be able to describe in detail different explosive stellar phenomena, including the various observational data and the underlying nuclear reaction networks involved.
The student will be able to perform resonant stellar reaction rate calculations at given temperatures for a variety of reactions. In particular, the student will have a detailed understanding of the importance of the specific microscopic nuclear physics input needed as well as the experimental and theoretical techniques involved in determining these properties.
The student will obtain an understanding of dark energy, direct dark matter detection research and will be able to reproduce the formalism for 2-flavour neutrino oscillation probabilities

Attributes Developed

C - Cognitive/analytical

K - Subject knowledge

T - Transferable skills

P - Professional/Practical skills

Module content

Indicative content includes:


Introduction to EPAP, overview of nuclear landscape and the importance of stars in the formation of the chemical elements


 

The Physics of Stars


Basic observations and stellar parameters – Hertzsprung-Russell diagram, Mass-Luminosity relationship and colour
Gravitational contraction and hydrostatic equilibrium
Main Sequence stellar structure
Late stellar evolution and compact astronomical objects


 

Explosive Stellar Phenomena


Classical Novae – Observations (UV/IR spectra and presolar grains), explosive hydrogen burning and novae nuclear reaction networks
Core-Collapse supernovae and the formation of neutron stars and black holes – Principles of the explosion and the possibility of neutrino driven winds. Heavy element formation and the role of the νp-process.
Cosmic γ-ray emission
Concept of isomers and nucleosynthetic complications involved in high temperature environments – example of 26mAl
X-ray bursts – Observations (XMM-Newton and Chandra satellite missions), “Breakout” from hot CNO cycles and nucleosynthetic path of the rp-process; role of waiting points


 

Experimental determination of Resonant Stellar Reaction Rates


Basic overview of nuclear reactions in exploding stars – Energetics: Q-values, reaction cross sections and concept of particle-emission thresholds (Sn, Salpha and Sp)
Experimental determination of Q-values – Mass measurements with Ion Penning Traps and Heavy-ion Storage Rings
Resonant reactions with neutrons and charged particles – concept of broad and narrow resonances
Analytical formalism for narrow and broad resonance contributions to stellar reaction rates – key nuclear physics properties of resonance energy, spin and particle partial widths
Experimental techniques for the determination of resonant stellar reaction rates –  



Direct methods using recoil mass spectrometers and need for radioactive ion beams. Direct methods using neutrons and time-of-flight facilities: (n,gamma) as well as (n,p) for vp-process.
Indirect methods: (i) Charge exchange reactions, such as (3He,t), and angular distributions  (ii) γ-ray spectroscopy; role of angular distributions, lifetimes and mirror symmetry, (iii) β-delayed particle decay spectroscopy; selection rules and logft values, (iv) Measurements of alpha-particle decay branches using transfer reactions and (iv) Spectroscopic factors from (d,p) and (3He,d) transfer reactions and principles of scattering theory.
Broad resonance studies and R-Matrix theory: example of 18F(p,alpha) and its role in the destruction of the potential cosmic gamma-ray emitter 18F in novae.


 

Astroparticle Physics


Nuclear reactions leading to solar neutrinos. Concept of neutrino oscillations and analytical formalism of 2-flavour oscillation probabilities.
Concept of Dark Matter – current experimental studies for direct dark matter detection (LUX-Zepplin and XENON 1T).
Basic principles of Dark Energy


 

Methods of Teaching / Learning

The learning and teaching methods include:

Formal lecture based module:

• 33 hours of lectures/tutorials split approximately in 22h of lectures and 11h of tutorials.

Assessment Strategy

The proposed assessment strategy for this module will involve:



30% for a report describing a computational project involving explosive nucleosynthesis yields and/or hydrodynamical stellar simulations. Open-source numerical codes will be provided.. Coursework set in week 6, to be submitted in week 9.


70% for a final, 1.5 hour closed book examination where students will answer 2 questions from a set of 3.

 



Formative feedback will be given in class tutorial sessions and from assessment of coursework.

 

Reading list

Reading list for EXPLOSIVE STELLAR PHENOMENA : http://aspire.surrey.ac.uk/modules/phym052

Programmes this module appears in

Programme Semester Classification Qualifying conditions
Physics MPhys 2 Optional A weighted aggregate mark of 50% is required to pass the module
Physics with Quantum Technologies MPhys 2 Optional A weighted aggregate mark of 50% is required to pass the module
Physics with Nuclear Astrophysics MPhys 2 Compulsory A weighted aggregate mark of 50% is required to pass the module
Physics MSc 2 Optional A weighted aggregate mark of 50% is required to pass the module
Physics with Astronomy MPhys 2 Optional A weighted aggregate mark of 50% is required to pass the module
Mathematics and Physics MMath/MPhys 2 Optional A weighted aggregate mark of 50% is required to pass the module

Please note that the information detailed within this record is accurate at the time of publishing and may be subject to change. This record contains information for the most up to date version of the programme / module for the 2017/8 academic year.