This course deals with the physics of gas and dust evolution in protoplanetary disks. Protoplanetary disks are gas disks surrounding young stars, and the solids in the disks are the building blocks of planets and other solid bodies. We will learn how micron-sized dust particles form kilometer-sized solid bodies called planetesimals.
1) Understand the physical processes governing the evolution of gas and dust in protoplanetary disks, including the solar nebula
2) Become familiar with order-of-magnitude estimates --- how to understand physics underlying complex phenomena
planet formation, protoplanetary disks, planetesimals, dust
|✔ Specialist skills||Intercultural skills||✔ Communication skills||✔ Critical thinking skills||✔ Practical and/or problem-solving skills|
Lectures will be given in the first half of the course. In the second half, some studies on thermal evolution of dust particles in the solar nebula are shown as examples of real researches in this field. The second half will be given by NAKAMOTO.
|Course schedule||Required learning|
|Class 1||Introduction||Understand the basic concepts of protoplanetary disks and planetesimals|
|Class 2||Protoplanetary disks #1: Structure||Understand the structure of disks around young stars|
|Class 3||Protoplanetary disks #2: Dynamics||Understand how protoplanetary disks evolves|
|Class 4||Particle motion in protoplanetary disks||Understand how dust particles move in gas disks|
|Class 5||Dust aggregates||Understand how small grains stick together and form macroscopic bodies|
|Class 6||Planetesimal formation||Understand how micron-sized dust grains form (and do not form) kilometer-sized solid bodies|
|Class 7||Snow lines||Understand the concept of snow lines and how they affect planet formation|
|Class 8||Case Study 1: Chondrule #1 --- Observed Properties||Understand the observed properties of chondrules.|
|Class 9||Case Study 1: Chondrule #2 --- Shock Wave Heating Model||Evaluate the shock wave heating model as a chondrule formation theory.|
|Class 10||Case Study 1: Chondrule #3 --- Asteroid Collision Model||Evaluate the asteroid collision model as a chondrule formation theory.|
|Class 11||Case Study 1: Chondrule #4 --- Lightning Model||Evaluate the lightning model as a chondrule formation theory.|
|Class 12||Case Study 1: Chondrule #5 --- X-Wind Model||Evaluate the X-wind model as a chondrule formation theory.|
|Class 13||Case Study 2: Crystalline Silicate --- Observations and Theories||Understand the study of crystalline sillicate and evaluate models.|
|Class 14||Case Study 3: CAI --- Observations and Theories||Understand the study of CAI and evaluate models.|
To enhance effective learning, students are encouraged to spend approximately 100 minutes preparing for class and another 100 minutes reviewing class content afterwards (including assignments) for each class.
They should do so by referring to textbooks and other course material.
Handouts will be provided
Grades will be based on in-class discussion and reports.
Basic knowledge of physics, astronomy, and the solar system