Saturday, June 24, 2017

Online courses

1. Papers of Dr. Young Chol Minh

Paper 1: Download link (andrews_ppdisk.pdf) - ASSIGNED TO GROUP 2 (Nguyễn Thị Phương & Widyanita Eka Putri)

Key points: protoplanetary disks, planet–disk interactions, dust continuum emission modelling, radio interferometric observations

Paper 2Download link (cesarsky_uib.pdf)

Key pointsreflection nebular, spectrophotometry, dust, infrared lines and bands 

Paper 3: Download link (heyer_cloud.pdf) - ASSIGNED TO GROUP 4 (Phạm Tuấn Anh & Phan Hoàng Minh)

Key points: molecular cloud, globule, kinematics and dynamics, interstellar molecules, star formation

Paper 4: Download link (minh_h2cs.pdf) - ASSIGNED TO GROUP 6 (Đinh Thị Mỹ Hảo & Bùi Thị Hoa)

Key points: molecular cloud, star formation, interstellar molecules, astrochemistry, dust mantle

Paper 5Download link (ngoc_bd.pdf)

Key points: low-mass star formation, brown dwarf, radio interferometric observations, interstellar molecules

Paper 6: Download link (onaka_miub.pdf)

Key points: diffuse dust emission, space mid-IR observation, dust properties

Paper 7Download link (snell_h2o.pdf)

Key points: molecular cloud, interstellar water molecule, space sub-millimeter observations, water abundances

Paper 8Download link (takahashi_omc.pdf)

Key points: molecular cloud, star forming dense cores, interstellar molecules, large-scale radio observations


 

2. Papers of Dr. Jorick Vink

Paper 1: Download link - ASSIGNED TO GROUP 7 (Mary Rose Balmeo & Phạm Văn Pháp)

Key points:
- Global stellar wind parameters (Sect 2.1)
- Resulting mass-loss rates and wind momenta (Sect 3.2)
- Metallicity effect (Sect 3.3)

Paper 2: Download link - ASSIGNED TO GROUP 4 (Phạm Tuấn Anh & Phan Hoàng Minh)

Key points:
- The theory of dM/dt determination (Sect 2.1)
- The calculation of the radiative acceleration g(r) (Sect 3.3)
- the predicted bi-stability jump (Sect 5)

Paper 3: Download link - ASSIGNED TO GROUP 1 (Đặng Đức Cường & Nguyễn Thị Vy Phương)

Key points:
- The calculation of the radiative acceleration (Sect 4.1)
- The self-consistent modelling of Wolf-Rayet winds (Sect 5)


3. Papers of Dr. Eva Villaver

Paper 1: Download link - ASSIGNED TO GROUP 3 (Đinh Thị Lan Anh & Ngô Thanh Liêm)

Key points: The focus is on how hard it is to determine observationally one of the most important quantities in Astrophysics: the initial to final mass relation and the implications that knowing the ending of stars have in all branches of astronomy.

Paper 2: Download link - ASSIGNED TO GROUP 8 (Nguyễn Thành Đạt & Nguyễn Thành Luân)

Key points: The focus is on how uncertain is our knowledge of mass-loss in massive (and not so massive) mass stars. The implications that mass-loss has on all branches of astrophysics.

Paper 3: Download link - ASSIGNED TO GROUP 2 (Nguyễn Thị Phương & Widyanita Eka Putri)

Key points: The focus is how is the evolution of the chemical elements in a galaxy. How the computations are performed and what are the constrains that can be extracted from the observations.  The discussion should be on the origin of Fe. 

 

 

4. Papers of Prof. Hiromoto Shibahashi

Paper 1: Download link - ASSIGNED TO GROUP 1 (Đặng Đức Cường & Nguyễn Thị Vy Phương)

Key pointsHow is the light time effect useful to find invisible binary companions among pulsating stars and to determine the orbital elements.

Lecutre 1Download link 

Paper 2: Download link - ASSIGNED TO GROUP 3 (Đinh Thị Lan Anh & Ngô Thanh Liêm)

Key pointsFor a given stellar mass, if the star is chemically homogeneous, the size of the star is determined so that the star can be in hydrostatic equilibrium and in thermal equilibrium. In most of text books, the presence of carbon, oxygen and other heavy elements is assumed, and as a consequence, hydrogen burning by the CNO cycle is supposed to occur at the main-sequence stage. If we consider stars born as the first generation in the universe, before heavy elements are created, how is the situation different?

Lecture 2Download link

Paper 3: Download link - ASSIGNED TO GROUP 5 (Huỳnh Loan Thảo & Nguyễn Trần Hoàng)

Key pointsHow different is the Fourier transform of discrete data from that of the corresponding continuous function? And what is a consequence of sampling with a periodically modulated time interval?

Lecture 3Download link

 

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