Stellar formation and circum-estelar medium
### Teaching language
English
_Obs.: As aulas serão em português caso todos dominem esta língua._
### Objectives
The processes associated with the formation and the early evolution of stars are introduced. The period in analysis includes the molecular clouds formation, the formation of the proto-star and the pre-main-sequence evolution before the star reaches the main sequence. Complementing the theoretical part, we present observational examples of the different stages of evolution of a young star.
### Learning outcomes and competences
At the end the student will have a global view of the theories of star formation and pre-main sequence stellar evolution. The student will also have a global view over the observational component that is used for the study of molecular clouds, protostars and circumstellar medium.
### Working method
Presencial
### Program
I - Star Formation in our Galaxy
1\. Overview
1. Stellar Nurseries
2. Stars and their evolution
3. The Galactic context
2\. Interstellar Medium (ISM)
1. Galactic Gas
2. Phases of the ISM
3. Insterstellar Dust - Extinsion/Emission - Properties of the grains
3\. Molecular Clouds
1. Giant Molecular Clouds
2. Virial Theorem Analysis
3. Dense Cores
4\. Young Stellar Systems
1. Embebed Clusters
2. The Initial Mass Function
II - Physical Processes in Molecular Clouds
1\. Introduction to Radiative Transfer
2\. Molecular Transitions
1. Interstellar Molecules
2. Hydrogen (H2)
3. Carbon-Monoxide (CO)
4. Applications of CO
3\. Heating and Cooling
1. Cosmic Rays
2. Interstellar Radiation
3. Cooling by Atoms, Molecules and Dust
4\. Cloud Thermal Structure
1. The Buildup of Molecules
2. The Molecular Interior
III - From Clouds to Stars
1\. Cloud Equilibrium and Stability
1. Isothermal Spheres and the Jeans Mass
2. Magnetostatic Configurations
2\. The Collapse of Dense Cores
1. Ambipolar Diffusion
2. Inside-Out Collapse
3\. Protostars
1. First Core and Main Accretion Phase
4\. Multiple Star Formation
1. Dynamical Fragmentation of Massive Clouds
IV - Pre-Main Sequence Stars
1 - T-Tauri Stars
1. Line and Continuum Emission
2. Outflow and Infall
3. Circunstellar Disks
4. Post-T Tauri Stas and Beyond
2 - Herbig Ae/Be Stars
1. Basic Properties
2. Gaseous and Debris Disks
V - Accretion discs
1\. Theory of standard accretion discs
1. Equations of conservation and the difusion equation
2. Stationary discs
3. Boundary conditions
2\. Observations vs Theory
1. Spectral Energy distribution
2. Spectral emission from an optically thick steady disc
3. Sources of excess emission
3\. Introduction to accretion shock models
### Mandatory literature
Stahler Steven W.; [The formation of stars](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000263483 "The formation of stars (Opens in a new window)"). ISBN: 3-527-40559-3
Frank J.; [Accretion power in astrophysics](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000244780 "Accretion power in astrophysics (Opens in a new window)")
### Complementary Bibliography
Lee Hartmann; Accretion Processes in Star Formation, Cambridge University Press, 2009. ISBN: 978-0-521-53199-3
Donald E. Osterbrock; [Astrophysics of gaseous nebulae and active galactic nuclei](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000226259 "Astrophysics of gaseous nebulae and active galactic nuclei (Opens in a new window)"). ISBN: 0-935702-22-9
Gray David F.; [The observation and analysis of stellar photospheres](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000268080 "The observation and analysis of stellar photospheres (Opens in a new window)"). ISBN: 0-521-85186-6
Philip J. Armitage; Astrophysics of Planet Formation, Cambridge University Press, 2010. ISBN: 978-0-521-88745-8
### Teaching methods and learning activities
Multimedia presentations and Tutorial guidance.
The support material of the course will be available via the Moodle UP, including a copy of the slides used. There is a main reference book that is the main bibliography, but for some components of the course complementary bibliography and/or scientific articles may be used.
### Software
Python
Latex
### keywords
Physical sciences
Physical sciences > Astronomy
Physical sciences > Astronomy > Astrophysics
### Evaluation Type
Distributed evaluation with final exam
### Assessment Components
Exam: 70,00%
Practical assignment or project: 30,00%
**Total:**: 100,00%
### Amount of time allocated to each course unit
Presentation/discussion of a scientific work:10,00 hours
Autonomous study: 70,00 hours
Frequency of lectures: 42,00 hours
Written assignment: 40,00 hours
**Total:**: 162,00 hours
### Eligibility for exams
The student has frequency to the course if he/she misses no more than 1/3 of the planned classes.
### Calculation formula of final grade
The final grade is obtained through three components:
1) 70% - a final written exam
2) 20% - computational work developped during the semester with a final written report
3) 10% - presentation and discussion of the computational work.
### Examinations or Special Assignments
Pratical work task with written report and presentation. This task will be done throughout the semester.
### Classification improvement
The student may improve the classification in the written exam (weight of 70% in the final classification). It will not be possible to improve the classification in the pratical work task
More information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498808
Presential
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Stellar formation and circum-estelar medium
Funded by the European Union. Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or HaDEA. Neither the European Union nor the granting authority can be held responsible for them. The statements made herein do not necessarily have the consent or agreement of the ASTRAIOS Consortium. These represent the opinion and findings of the author(s).
