|Delivery Type||Delivery length / details|
|Seminars / Tutorials||2 x 1-hour seminars|
|Workload Breakdown||Every 10 credits carries a nominal student workload of 100 hours: 18 hours Lectures, 2 hours Seminars, 20 hours oral presentation including preparation time, 60 hours independent study|
|Assessment Type||Assessment length / details||Proportion|
|Semester Exam||1.5 Hours||60%|
|Semester Assessment||2 assignment sheets (2 x 20%)||40%|
|Supplementary Exam||2 Hours||100%|
On successful completion of this module students should be able to:
1. Recognise the problem posed by coronal heating and critically discuss heating models;
2. Explain the variation in coronal and solar wind structure in terms of changes in the solar magnetic field;
3. List models that can accelerate relativistic charged particles;
4. Discuss how coronal parameters can be measured;
5. Derive Parker's simple theory of the solar wind and critically discuss its limitations in the light of solar wind measurements;
6. Explain the origin of co-rotating structure in the solar wind;
7. Estimate the location of the solar wind termination shock and critically discuss limitations of the simple model used to calculate this position;
8. Recognise the important factors in Sun-planetary coupling over short and long time-scales;
9. Discuss the main features of Sun-comet coupling, discuss the strengths and weaknesses of the methods available to measure solar wind parameters and show how different methods can be combined to answer specific scientific questions.
The course provides an in-depth treatment of the Physics of the solar atmosphere and heliosphere, including coupling between the solar wind and non-magnetised objects.
Solar wind and heliosphere: Parker's theory. Solar breeze and solar wind. Effect of conductivity and viscosity. Spiral structure of Interplanetary magnetic field. Acceleration of solar wind near sun. Non-uniform flow and shock fronts. Terminator Shock. Measurements of the solar wind: White-light drift measurements, interplanetary scintillation and in-situ measurements. Resolving the 3D structure of the solar wind.
Sun-Earth connections: Interaction with planetary magnetic fields. Terrestrial effects of solar variability. Long period variations in activity. Solar wind and cosmic ray shielding. 'Space climate'.
|Skills Type||Skills details|
|Application of Number||All questions set in tests, example sheets and formal examinations will include numerical problems|
|Communication||Written communication is developed via lecture assignments. Visual and spoken communication is developed via the oral presentation.|
|Improving own Learning and Performance||Formative assignments are used in order that students might reflect on their progress during the module. The oral presentations will provide an opportunity to compare their work with those of other groups and form an idea of 'best practice'|
|Information Technology||Students will be required to research topics within the module via the internet. Power Point Presentation (or equivalent) skills will be required for the oral presentation|
|Personal Development and Career planning||The module will highlight the latest developments in this field and hence will assist with career development. The poster project, requiring students to work as a team, is of importance in fostering career development.|
|Problem solving||Problem solving is a key skill in physics and will be tested via lecture problem sheets, in the oral presentation and in formal examination at the end of the module|
|Research skills||An oral presentation, for which students are required to independently research one of a range of topics covered by the course forms 15% of the module assessment. Research skills will also be developed|
|Subject Specific Skills|
|Team work||The oral presentation project is a group assignment, so team work will be developed as students co-operate to research the various areas covered and develop the presentation|
This module is at CQFW Level 6