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ASTRONOMY COLLOQUIUM<br>Watching a Little Gas Cloud on its Way into the Galactic Supermassive Black Hole

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        1. <b>ASTRONOMY COLLOQUIUM</b><br>Tracing the Cosmic Shutdown of Star Formation in Massive Galaxies
        2. <b>ASTRONOMY COLLOQUIUM</b><br>The Effects of Magnetic Field Morphology on the Determination of Oxygen and Iron Abundances in the Solar Photosphere
        3. <b>ASTRONOMY COLLOQUIUM</b><br>Star Formation Across Space
        4. <b>ASTRONOMY COLLOQUIUM</b><br>Lonely Galaxies: The Baryon Content of Isolated Dwarf Galaxies
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        7. <b>ASTRONOMY COLLOQUIUM</b><br>A Galaxy-Scale Fountain of Cold Molecular Gas Pumped by a Black Hole
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        34. SPECIAL ASTRONOMY COLLOQUIUM<br>Ralph Baldwin Prize in Astrophysics and Space Sciences<br>Lonely Massive Stars</br>
        35. ASTRONOMY COLLOQUIUM<br>Live Fast Die Young: The Evolution of Massive Stars towards their Death</br>
        36. ASTRONOMY COLLOQUIUM<br>Watching a Little Gas Cloud on its Way into the Galactic Supermassive Black Hole
        37. ASTRONOMY COLLOQUIUM<br>Dwarf Galaxies as Cosmological Probes
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        42. ASTRONOMY COLLOQUIUM<br>Accretion Disk Outbursts: MHD Simulations (Finally) Confront Reality
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        44. ASTRONOMY COLLOQUIUM<br>Star Clusters and High Mass X-Ray Binaries in Nearby Spirals, Mergers, and Starburst Galaxies
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Thursday, April 3, 2014
12:00 AM
807 Dennison Building

The Galactic center is one of the most fascinating and extreme places in the Galaxy. Harboring a supermassive black hole with a mass of order 4 million solar masses, it experiences cycles of activity and star formation, separated by periods of quiescence that last of order a million years. The Milky Way's SMBH currently is inactive. However, a small, diffuse gas cloud (G2) has recently been detected (Gillessen et al. 2012, 2013) on an orbit almost straight into the Galactic SMBH. In April 2013 G2 started to pass the SMBH at a small distance of just 2000 Schwarzschild radii, corresponding to 20 light hours. Most of its emission is still strongly redshifted and prior to pericenter. However, a fraction of it is now emerging on the strongly blue-shifted side of the orbit, past pericenter. This indicates that the ionized gas of G2 is not stretched over more than 15,000 Schwarzschild radii around the pericenter. Depending on its nature G2 will now begin to break up and feed the SMBH, possibly triggering a phase of AGN activity. The next years will therefore provide a unique opportunity to investigate directly the processes that drive and regulate gas accretion onto the Galactic SMBH. In addition, G2 turns out to be a powerful probe in order to probe the structure and composition of the Galactic center.

This talk will summarize the observations of G2 and current models about its nature. Is G2 a diffuse gas clump that originates from winds of high-mass stars in the surrounding stellar disk or is it the atmosphere of an evaporating, invisible protostellar disk, surrounding a young low-mass star? Or is it something completely different? The existence of such a tiny, cold gas cloud in the hostile vicinity of the SMBH raises numerous fascinating questions related to its structure. Where did it come from and where will it go? Why is it on such a highly eccentric orbit? Which physical processes constrain its properties like size, mass, density, temperature and geometrical shape? How many clouds like G2 are currently orbiting Sgr A* and how do they affect its activity and gas accretion rate? Like comet Shoemaker-Levy's 1994 collision with Jupiter, the big challenge has started for astrophysicists to predict the outcome of G2's close encounter with the SMBH in the years 2013-2015 and beyond. Their models will be validated directly by observations within the next couple of years.

Colloquia are generally preceded by tea and cookies at 3:30 in the Owl room (Dennison 845). For more information, please contact

Astronomy Colloquia listings for Winter 2014.