Erciyes University - Info Package

Course unit title	Level of course unit	Course unit code	Type of course unit	Semester of course unit	Local credit	ECTS credit	Syllabus
CHEMICAL EVOLUTION AND FORMATION OF THE GALAXY	Third cycle	AUB605		1	7.50	7.50	Print

Description of course unit

Prerequisites and course requisities	None
Language of instruction	Turkish
Coordinator	Asst.Prof.Dr. İnci AKKAYA ORALHAN
Lecturer(s)	Asst.Prof.Dr. İnci AKKAYA ORALHAN
Teaching assitant(s)	---
Mode of delivery	face to face
Course objective	In recent years a great deal of high resolution spectroscopic data, relating to chemical abundances in the stars of the Milky Way and its satellites, has appeared. Through the analysis of chemical abundances we can reconstruct the star formation histories of galaxies in terms of an astro-archaeological approach.
Course description	How to interpret abundances and abundance ratios in galaxies by means of detailed galactic chemical evolutionary models. After comparing model results and observational data we can put constraints on the star formation history, stellar nucleosynthesis and time-scales for the formation of galaxies.

Course contents

1	How to Model Galactic Chemical Evolution: The Initial Conditions, Stellar Yields
2	Basic Equations for Chemical Evolution: Yields per Stellar Generation, Analytical Models
3	Detailed Numerical Models
4	The Milky Way: The Formation of the Milky Way
5	The Two-Infall Model
6	The Chemical Enrichment History of the Solar Vicinity
7	The G-dwarf Metallicity Distribution and Constraints on the Thin Disk Formation
8	Mid-Term Exam
9	The G-dwarf Metallicity Distribution and Constraints on the Thin Disk Formation
10	Carbon and Nitrogen Evolution of Our Galaxy
11	S- and R- Process Elements
12	The Galactic Disk: Abundance Gradients,
13	The Galactic Bulge: Bulge Formation, The History of Bulge Chemical Evolution, Interpretation of Bulge Data and Other Galaxies, Recent Developments in the Galactic Bulge
14	The Time-Delay Model and the Hubble Sequence: The Typical Timescale for SN Ia Enrichment
15	Dwarf Spheroidals of the Local Group: How do dSphs Form?, Dark Matter in dSphs, Ultra-Faint Dwarfs in the Local Group
16	Final Exam
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Learning outcomes of the course unit

1	Extracting some important conclusions on the formation and evolution of the Milky Way, derived from chemical abundances.
2	By comparing the [α/Fe] ratios in the Milky Way and in dSphs of the Local Group we can conclude that these systems had different histories of SF.
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*Contribution level of the course unit to the key learning outcomes

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Number of stars refer to level of contribution from 1 (the least) to 5 (the most)

Planned learning activities, teaching methods and ECTS work load

	Quantity	Time (hour)	Quantity*Time (hour)
Lectures (face to face teaching)	16	3	48
Study hours out of classroom (study before and after the class)	16	3	48
Homework	2	10	20
Presentation / seminar	2	10	20
Quiz	0	0	0
Preparation for midterm exams	1	10	10
Midterm exams	1	2	2
Project (term paper)	0	0	0
Laboratuar	0	0	0
Field study	0	0	0
Preparation for final exam	1	10	10
Final exam	1	2	2
Research	3	10	30
Total work load			190
ECTS			7.50

Assessment methods and criteria

Evaluation during semester	Quantity	Percentage
Midterm exam	1	20
Quiz	0	0
Homework	1	20
Semester total		40
Contribution ratio of evaluation during semester to success		40
Contribution ratio of final exam to success		60
General total		100

Recommended and required reading

Textbook
Additional references

Files related to the course unit