PHYS30591
Astrophysical Processes
10
Semester 1
Undergraduate
Level 3
Rebecca Bowler
Unit coordinator
Rene Breton
Unit coordinator
Department of Physics & Astronomy
1
FHEQ level (Framework for Higher Education Qualifications) ' Last part of a Bachelors '
European Credit Transfer & Accumulation System Rating : 5.0
<p>Foundations in radiative transfer</p><p>Flux, intensity, radiative transfer equation, optical depth, mean free path, equivalent width of emission lines, emission/absorption line profiles.</p><p> </p><p>The interstellar medium</p><p>Composition of the ISM, properties of gas within galaxies, photo-ionization regions, heating/cooling mechanisms, dust grain properties, absorption and emission by dust.</p><p> </p><p>Radiative processes in astrophysics</p><p>a. Bound-bound transitions: Spectral line formation, emission lines as diagnostics of ISM conditions, Einstein coefficients, collisional excitation</p><p>b. Bound-free: continuum processes in the ISM, nebular continuum, formation of spectral breaks</p><p>c. Free-free: thermal Bremsstrahlung</p><p>d. Relativistic emission: synchrotron radiation and Compton scattering</p><p> </p><p>Physics of shocks</p><p>Introduction of fluid mechanics, ram pressure, jump conditions, shock frames of reference</p><p> </p><p>High-energy astrophysics</p><p>a. Supernova remnants: Free expansion, Sedov-Taylor phase, snowplough phase, merger with the ISM.</p><p>b. Accretion physics: Eddington limit, Bondi-Hoyle accretion, steady thin accretion</p><p>c. First and second order Fermi acceleration (diffuse shocks)</p><p> </p><p>Multi-messenger astrophysics</p><p>Gravitational waves, basic physics from binary mergers, and cosmic rays.</p>
<p>Foundations in radiative transfer</p><p>Flux, intensity, radiative transfer equation, optical depth, mean free path, equivalent width of emission lines, emission/absorption line profiles.</p><p> </p><p>The interstellar medium</p><p>Composition of the ISM, properties of gas within galaxies, photo-ionization regions, heating/cooling mechanisms, dust grain properties, absorption and emission by dust.</p><p> </p><p>Radiative processes in astrophysics</p><p>a. Bound-bound transitions: Spectral line formation, emission lines as diagnostics of ISM conditions, Einstein coefficients, collisional excitation</p><p>b. Bound-free: continuum processes in the ISM, nebular continuum, formation of spectral breaks</p><p>c. Free-free: thermal Bremsstrahlung</p><p>d. Relativistic emission: synchrotron radiation and Compton scattering</p><p> </p><p>Physics of shocks</p><p>Introduction of fluid mechanics, ram pressure, jump conditions, shock frames of reference</p><p> </p><p>High-energy astrophysics</p><p>a. Supernova remnants: Free expansion, Sedov-Taylor phase, snowplough phase, merger with the ISM.</p><p>b. Accretion physics: Eddington limit, Bondi-Hoyle accretion, steady thin accretion</p><p>c. First and second order Fermi acceleration (diffuse shocks)</p><p> </p><p>Multi-messenger astrophysics</p><p>Gravitational waves, basic physics from binary mergers, and cosmic rays.</p>
<p class="MsoNormal" style="line-height:150%;text-align:justify;"><span style="background-color:rgb(255,255,255);color:rgba(0,0,0,0.87);"><span style="-webkit-text-stroke-width:0px;display:inline !important;float:none;font-family:"Segoe UI", Lato, "Helvetica Neue", Arial, Helvetica, sans-serif;font-size:14px;font-style:normal;font-variant-caps:normal;font-variant-ligatures:normal;font-weight:400;letter-spacing:normal;orphans:2;text-align:start;text-decoration-color:initial;text-decoration-style:initial;text-decoration-thickness:initial;text-indent:0px;text-transform:none;white-space:normal;widows:2;word-spacing:0px;">To introduce a wide range of fundamental astrophysical processes and their role in modern astrophysics. These processes range from those which control the structure of the interstellar medium to those associated with supermassive black holes in the centre of galaxies. The observational signatures of these processes are identified, which cover the entire electromagnetic spectrum from radio to gamma-ray and include non-photonic tracers such as cosmic rays.</span></span></p>
<p><i>On the successful completion of the course, students will be able to: </i></p><p>ILO 1</p><p>Describe the sky as seen across the electromagnetic spectrum and non-photonic messengers and the involved radiation mechanisms</p><p>ILO 2</p><p>Explain fundamental physical processes in astrophysics such as</p><p>a. radiative transfer</p><p>b. shock waves</p><p>c. accretion</p><p>ILO 3</p><p>Apply physical principles to predict the emission and absorption properties for atoms, molecules and grains in astrophysics contexts.</p>
<p>Two one hour, live in-person lectures per week where the core material with examples will be delivered. The recordings of these lectures will be on the course online page. A weekly problem sheet will be provided, with solutions and feedback on common problems released the following week. A Piazza discussion forum is also provided where students can ask questions with answers provided by other students and the unit lead. </p>
1
Written exam
100%
<p>Feedback will be offered to the cohort on the common difficulties on the weekly questions sheets, model answers will be issued.<p></p></p>
PHYS10101
Dynamics
Pre-Requisite
Compulsory
PHYS10191
Introduction to Astrophysics and Cosmology
Pre-Requisite
Compulsory
PHYS20141
Electromagnetism
Pre-Requisite
Compulsory
MMath & Phys(Hons) Maths & Phy
MMath & Phys(Hons) Maths & Phy
Third Year
Optional
Y
<p>Recommended texts </p><p>Dyson, J.E. & Williams, D.A. The Physics of the Interstellar Medium (2nd ed.) (IOP Publishing)</p><p>Rosswog, S. & Bruggen, M. Introduction to High-Energy Astrophysics (CUP)</p><p> </p><p>Supplementary reading</p><p>Draine, B.T., Physics of the Interstellar and Intergalactic Medium, (Princeton)</p><p>Longair, M. S. High Energy Astrophysics, 3rd edition, (CUP) </p><p>Rybicki, G.B. & Lightman, A.P. Radiative Processes in Astrophysics </p>
Assessment written exam
2
Lectures
22
0
76