UV Ceti Stars Jessica Windschitl Atmospheres Spring 2007.
Poster 67. A PHOTOMETRIC TRANSIT SEARCH FOR PLANETS AROUND COOL STARS FROM THE ITALIAN ALPS: RESULTS FROM A FEASIBILITY STUDY A. Bernagozzi (1), E. Bertolini.
Chapter 13 Cont’d – Pressure Effects More curves of growth How does the COG depend on excitation potential, ionization potential, atmospheric parameters.
1 Stars Stars are very far away. The nearest star is over 270,000 AU away! ( Pluto is 39 AU from the Sun ) That is equal to 25 trillion miles! At this.
Diagnostics of Inhomogeneity in the Outer Atmospheres/Winds of M Supergiants Alexander Brown Center for Astrophysics and Space Astronomy University of.
Origin of the Elements Cosmochemistry I Lecture 39.
Using Semantic Web Technology to Integrate Scientific Data Alasdair J G Gray University of Manchester.
X-ray Emission from Massive Stars: Using Emission Line Profiles to Constrain Wind Kinematics, Geometry, and Opacity David Cohen Dept. of Physics and Astronomy.
Extraterrestrial Expeditions: 2010 Poseidon Expedition to Neptune By: Abbie, Brian, Emily, and Karina.
Winds and Chromospheres of Cool (Super-) Giants Wind Acceleration, Structure and Energy Balance What we know, don’t know, and what we can do about it Graham.
Wind Signatures in the X-ray Emission Line Profiles of the O Supergiant Orionis Kevin Grizzard 1, David Cohen 2, Maurice Leutenegger 3, Casey Reed 2,
First Hour Test –Wednesday 16 February –Bring two No. 2 pencils –An eraser (“Do you feel lucky?”) –A photo ID –Something to write on Review Session –Tuesday.