PPT-Star Formation in Extremely Faint Gas

Rich Dwarf Galaxies Sambit Roychowdhury NCRA Jayaram N Chengalur NCRA Igor D Karachentsev SAO Margarita Sharina SAO Ayesha Begum . Extra-solar planetary systems. Lecture . 16. Other theory. Tidal Hypothesis. Early attempt to explain the dichotomy of planets.. Problem?. tidal force strong enough to “draw out” a filament from stars will effectively disperse it before it could condense into planets!. What force makes stars? . Gravity!. Out of what? Interstellar gas and dust. But this stuff is VERY low density… a dense area may have ~100 atoms / cm. 3. . Compare that the air you’re breathing… ~10. Smolcic. . ea. ). Compilation based on different star formation estimators (UV, IR, radio, Hα..). Large scatter: Dust obscuration is major problem. Hopkins & . Beacom. (2006) compilation. redshift. 1. The ". Q". word and its meaning. Is quenching a good word to describe the end of star-formation in galaxies ? . What are the timescale(s) for quenching? . Pablo , Jarle. Is quenching due to starvation or gas expulsion? . Christopher W. Ashcraft M.S., M.Ed.. Big Bang vs. Creation. Origin of Stars. Solar System: Evidence of Design. Age of the Cosmos. Are we being told all the evidence or just selected information to support a particular idea?. Sections 39.1-39.5. Reminders. Don. ’. t forget about weekly reflections. …. Should I drop the 2 lowest weekly reflections?. Should I drop the 3 lowest reading quizzes?. Final . exam. . Thursday. D. Calzetti (Univ. of Massachusetts). a. nd the LEGUS . Team. https://. legus.stsci.edu. /. HUBBLE2020: Hubble’s 25. th. Anniversary Symposium. STScI. , Baltimore, April 20-24, 2015. NGC3344. NGC1566. ’ Stars . . Supremely Important. In order to make the most important astrophysical determinations, including. True (intrinsic) brightness. , . mass, . size, . e. tc. …. we . have to . know the distances.. Oleg . Gnedin. (University of Michigan. ). g. raduate student . Hui. Li. Star clusters are dominant components of active star formation:. they connect small-scale SF (local) and global processes in galaxies. with Marco Lombardi, . Joao Alves, . Jan Forbrich, . Gus Munch. Kevin Covey. & Carlos Roman . z = 1 - 10. Bouwens et al. 2010. z = 0.000. S. Guisard ESO. Pipe Nebula. Guidepost. In this chapter, you will consider how the interstellar medium condenses into stars and what the conditions inside stars must be like. How do stars form?. What is the evidence that stars are forming now?. Zooming in on Star Formation. , Nafplio, June 14. , 2019. Galactic Scale Star Formation. What we know for sure now:. Feedback, and vertical pressure (. im. -)balance is crucial. The role of radial and vertical net mass transport is poorly understood. Jeff Mangum. NRAO. 2. Extragalactic Star Formation. 3. Multi-transition analysis of molecular excitation within high spatial. . density (n(H2) > 10^5 cm^-3) and high kinetic temperature (. Tk. > 100 K) environments. How Galaxies form Stars – August 24 2016 . Robbert. Verbeke. 1. Bert . Vandenbroucke. Sven De . Rijcke. Ghent University. 1. Robbert.verbeke@ugent.be. @. Rbhfd. Λ. CDM. Standard model for cosmology.