Slide 1Stellar Evolution II Slide 2 The Upper End of the Main Sequence: How massive can a star get? Larger clouds of gas (GMCs) tend to fragment into smaller ones before…

Slide 1 the s-process Fe Co Ni Rb Ga Ge Zn Cu Se Br As Zr Y Sr Kr (n,  ) ()() ()() r-process p-process 63 Ni, t 1/2 =100 a 64 Cu, t 1/2 =12 h,…

Slide 1 Improving our understanding of Stellar Evolution with PLATO 2.0 Santi Cassisi INAF - Astronomical Observatory of Teramo, Italy Slide 2 PLATO2.0 Stellar Evolution…

Slide 1 Activity #32, pages 111-112 (pages 109-110 were done last Friday) Slide 2 12.3 Life as a High-Mass Star Our Goals for Learning What are the life stages of a high…

Slide 1 Memory restriction, limits and heterogeneous grids. A case study. Txema Heredia Or an example of how to adapt your policies to your needs Slide 2 DISCLAIMER What…

Astronomy 1020 Stellar Astronomy Spring_2015 Day-33 Course Announcements 1 Dark night observing session left: Thurs. Apr. 16 Alternative exercise is posted. Reports are due…

Presentation for perspective graduate students 2006 Astronomy 1 – Fall 2014 Lecture 12; November 18, 2014 1 Algol (beta Persei) provided the first clear evidence of mass…

Stellar Evolution â the Life and Death of a Star⦠Hereâs the story weâll tell⦠Lowest mass stars and their evolution Low mass star evolution High mass star evolution…

The solar system Our sun does not have a solid surface. Most of the energy comes from the core and is radiated out to the surface like convection in boiling water. In the…

Stars The Sun The largest object in our solar system You can line-up about 109 Earths across the Sun Made mostly of Hydrogen (70.4%) and Helium (28%) Remaining 1.6% is made…