PPT-Towards Realistic Modeling of Massive Star Clusters

Oleg Gnedin University of Michigan g raduate student Hui Li Star clusters are dominant components of active star formation they connect smallscale SF local and global processes in galaxies. Unfortunately current geometric acoustic modeling systems do not accurately simulate reverberant sound Instead they model only direct transmission and specular re64258ection while diffraction is either ignored or modeled through statistical approx i Penn State University. ONC/Paradigm for Star Formation . STScI. Oct 2013 . The ONC and the . MYStIX. Survey. Massive . Young Star-Forming Complex Study . in . Infrared and . X-ray. Outline. Introduction: Orion as a template for . and self enrichment of globular clusters. Norbert Langer (. Bonn). Onno Pols (. Utrecht). Rob Izzard (. Brussels). Selma de Mink. Utrecht . . Bonn . . . STScI. (. N. ov 2010). A&A 507, 1 (2009). With a wide-field multi-IFU spectrograph. Cluster studies. Clusters provide large samples of galaxies in a moderate field. Unique perspective on the interaction of galaxies with their environment. As they operate much as a closed box, they are useful as tracers of galaxy evolution and of cosmology. . CDM Cosmology. Oleg . Gnedin. (University of Michigan. ). What we knew before HST: globular clusters are old, dense, compact – a distinct type of stellar spheroids. Kormendy. (1985). Over 20 years the Hubble Space Telescope has revealed young massive star clusters in interacting and gas-rich galaxies.. Drs. Carol Christian, Antonella Nota, and Brad Whitmore. May 7, 2015. Stars /Star Clusters. Carol Christian. Stars form from gas and dust clouds. The clouds collapse due to gravity. Also the clouds can collide / compress. in the Milky Way. Christian Johnson. Smithsonian Astrophysical Observatory. “Typical” Globular Clusters. Main Sequence. Main Sequence Turn-off. Subgiant Branch. Red Giant Branch. Horizontal Branch. Generally speaking, . there are two main life cycles for stars. . . The factor which determines the life cycle of the star is its mass. . . 1 solar mass = size of our Sun. Any star less than about three solar masses will spend almost all of its existence in what is called the “Main Sequence”. . Wen-Ping . Chen . National . Central . University . Census of Galactic open clusters. . Dynamical evolution of a star cluster. . Star clusters as targets and as tools. Outstanding issues. 2017 April 28 PMO . Evolution off the Main Sequence. Main Sequence Lifetimes. Most massive (O and B stars): millions of years. Stars like the Sun (G stars): billions of years. Low mass stars (K and M stars): a trillion years! . Ann Marie Cody. NPP fellow at NASA Ames. November 2, 2015. Acknowledgments. Ames collaborators. : Steve Howell, Tom Barclay, Fergal . Mullally. , Susan Thompson, . Geert. . Barentsen. , Jason Rowe, student interns: Bryan Mann, . David Cohen. Swarthmore College. If we understand . the physical connection between magnetic fields in massive stars and X-rays, we could use X-ray observations to identify magnetic massive stars.. e.g. Which of the stars in this Chandra X-ray image of the Orion Nebula Cluster are massive magnetic stars? . 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. Laura . Magrini. INAF- . Osservatorio. . Astrofisico. di . Arcetri. In Our Galaxy. Open clusters (disc population): . Many (~2200 known clusters). . even more new candidates in the inner disc from infrared surveys .