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**Stellar Atmosphere & Spectra Analysis**

**Course Code**: 031M4004H

**Course Name**: Stellar Atmosphere & Spectra Analysis

**Credits**: 3.0

**Level**: Graduate

**Pre-requisite**: The Basic Astronomy, The Radiation Processes in Astrophysics

**Lecture Time**: 20 weeks, 3 hours/week, 60 hours in total

**Instructors**: Prof. Feilu WANG

**Course Description**

This course is designed to give a fundamental understanding to the physics in stars for the graduate student whose mayor is astrophysics or similar. The stellar physics is a wide-ranged topic, and this course will focus on the stellar atmosphere and spectra analysis. The topics include: the fundamental theories of the stellar atmosphere, the basic concepts of the stellar spectra, and the analyzing methods. By completing this course, the students will have a basic understanding to the stellar atmospheres, stellar spectra, and the analyzing methods, which are of great importance to their future academic careers.

**Topics and Schedule**

**Part I. ****The chemical evolution of the Milky Way (15 hours)**

*Lecture 1**: The origin of elements, nucleosynthesis, and metal-poor stars (3 hours) *

*Lecture** 2: The evolution of the stars (3 hours) *

*Lecture 3:** The isochrones and the ages of stars (3 hours) *

*Lecture 4:** The stellar populations and structures of the Milky (3 hours) *

*Lecture 5**: The galactic chemical evolution (GCE) models. (3 hours) *

**Part II. ****The stellar atmospheric models and their computations (21 hours)**

*Lecture 1:** An introduction to the stellar radiation field (3 hours) *

*Lecture 2**: The local thermodynamic equilibrium (LTE) and opacity (3 hours) *

*Lecture 3**: The radiation transfer equation (3 hours)*

**Highlights**: The deviation of the radiation transfer equation under the parallel-plane assumption; the definition of source function; the interpretation of the limb darkening of the Sun; the solution and boundary of the transfer equation; the moment of the radiation transfer equation; the commonly used operators in the radiation transfer theory.

**Difficulties**: Understand the nature of absorption line and emission line; the Schwarzschild-Milne equations.

*Lecture 4**: The radiative and hydrostatic equilibrium equations, the convection, and the grey atmosphere assumption (3 hours) *

*Lecture 5**: The continuum opacity (3 hours) *

*Lecture 6**: The non-local thermodynamic equilibrium (NLTE), the movement of the atmosphere and the stellar wind (3 hours) *

*Lecture 7**: Model atmosphere (3 hours) *

**Part III. ****Modern Spectrograph and Spectrum Reduction (6 hours)**

*Lecture 1**: The spectrograph and optical fibers (2 hours) *

*Lecture 2**: The spectrum observation (2 hours) *

*Lecture 3**: The spectrum reduction (2 hours) *

**Part IV. ****The Quantificational Spectrum Analysis (18 hours)**

*Lecture 1**: The line profiles and the broadening mechanisms (3 hours) *

*Lecture 2**: The equivalent width and line profiles (6 hours) *

*Lecture 3**: NLTE line synthesize (6 hours) *

*Lecture 4**: The Quantificational Analysis to Stellar Spectra (3 hours) *

**Textbook & References**

1. Runqian Huang, Stellar Physics, Science Press, 1998 (Only in Chinese)

2. Erika Böhm-Vitense, Introduction to stellar astrophysics, Cambridge University Press, New York, 1989.

3、Eva Novotny, Introduction to stellar atmospheres and interiors, Oxford university Press, New York, 1973.

4、David F. Gray, The observation and analysis of stellar photospheres, John Wiley & Sons company, New York, 1976; 1992.

5、Allen’s Astrophysical Quantities, Arthur N. Cox, Editor, AIP Press, Springer, 2000.

6、John T. Jefferies, Spectral line formation, Blaisdell publishing company, London, 1986.

**Introduction to the Instructors:** None.