PPT-Cepheid Variable Stars

Cepheids Very late in their lives massive stars can pass briefly through a stage in which they are unstable During this stage their outer parts oscillate pulsate in a nd out. Wrocław 20.08.2013. Mid 1960ties.. . Variability. of . Cepheids. and RR . L. y. r. ae. stars explained. . Radial. . pulsation. . hypothesis. (Ritter 1879. ) . confirmed. (. Shapley. 1914, . Soprano I Hence  stars,  you  daz- zle but the sight,   you teach to Soprano II Hence  stars, \r \r \r Alto Hence  stars, hence   stars too  dim of light,  you  daz-  zle  b Pulsating Variable Stars. Overview. History of discovery. What are pulsating variable stars?. Why are they important?. Any recent works?. Pulsating Variable Stars. History. 1595 – David Fabricius. o Ceti,. Introduction. Trigonometric Parallax . Spectroscopic Parallax . Cepheid Variables . Type Ia Supernovae. Tully-Fisher Relationship. Hubble’s ‘Law’ . Trigonometric Parallax. While fundamental, this method is very limited in terms of how far away one can use it. For large numbers of star, ground-based measurements of parallax do not get beyond about 20 pc, although on individual objects this can be extended to about 100 pc (with much effort). . Mid-Infrared Light Curve Structure of LMC Cepheids. Acknowledgements. National Science Foundation's Office of International Science and Engineering award number 1065093, NCU, the Department of Physics and Astronomy at NCU, Dr. Shashi Kanbur, the International Office at NCU. Program. A mid-infrared recalibration of the extragalactic distance scale. Carnegie Hubble . Program. Wendy Freedman (PI). Eric . Persson. , Mark Seibert. Vicky Scowcroft, Andy Monson. Laura . Sturch. LMC Cepheid Variables PL Relation in IR. J. Bennett, D. Citro, J. . Chartrand. , S. . Kanbur. , C. . Ngcow. , L. . Macri. , S. . Mahzooni. , F. Ripple. Physics Department, SUNY Oswego, National Central University Taiwan, and Texas . Overlapping rungs:. Earth. Earth-Mars. Earth’s orbit. Parallax. Spectral “Parallax”. RR Lyrae variables. Cepheid variables. Type I Supernovae. Type II Supernovae. Galaxy brightness. Measuring Earth - Geometry. 25 years of Astronomy. Etteyeb Nejmeddine. 21 years old. The Astronomical Society of Tunisia (SAT) . The Charlie Bates Solar Astronomy Project (CBSAP). Computer Science . What Are Variable Stars?. Detecting variability. and Parallax from Spatial Scanning. Part 2. Adam Riess and Stefano . Casertano. Distortion at the . milli. -. pixel level. Spatial Scanning Provides measurement 1D. *. precision of < 1 . millipix. Chapter . 13, . Sections . 1. -5,7 (12 . pages). Homework for Next Time: . www.galaxyzoo.org. Question. Which of these is a picture of the Milky Way?. A. B. D. C. The Milky Way. Angular Size. Andromeda: MW’s Sister Galaxy. 23. Jeff Wilkerson. Luther College. RAC. July 13, 2010. We image 3 clusters per year: M23 and two others. Image durations: 2 to 12 seconds, unfiltered. Campaign durations: 5 to 7 months. Return to a cluster at least once. Gordon Myers. AAVSO Speakers Bureau. ALCON 2009. Historical Perspective – Mira. David . Fabricius. discovered “omicron . ceti. ” in 1596. Brightened from 3. rd. Jeremiah Horrocks Institute. University of Central Lancashire. 11/26/10. IAC WS 2010 – Lecture 3. 11/26/10. IAC WS 2010 – Lecture 3. Pieter de Groote . PhD thesis. 11/26/10. Shorter time scale photometrically variable stars.