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Transcript
Black Hole Chaos The Environments of the most supermassive black holes in the Universe Belinda Wilkes, Chandra X-ray Center, CfA Francesca Civano, CfA Black Hole • Nothing beats gravity → collapses forever • Light cannot escape from inside the event horizon Matter spiraling inwards → accretion disk Stellar Mass Black Hole • Big, old star blows up • Can be seen when in binary star systems • BH pulls matter from companion star • Bright, variable/bursting sources Star Jet BH and accretion disk Black Hole: Mass and Spin • Properties determine their effects on their surroundings • Spinning BH has a smaller “size” (event horizon is closer in) No spin With spin Super-massive Black Hole (SMBH) Galaxy-sized! • Formed in centers of galaxies in early Universe • 1 million – 1 billion times Sun’s mass • SMBH size ~ our solar system (15 lt mins) • SMBH grows as material falls in Central Regions: Accretion Disk spinning around SMBH • Matter spirals in to galactic center and forms an accretion disk (~few lt.yrs.) • Becomes very hot and outshines the 10 billion stars in the host galaxy → Quasar • Hottest near center • X-rays good clear view, even when edge-on • BH grows as matter falls in • Other matter is pushed outwards: jets, winds Artist’s Impressions! But this one is real: Cen A Model of Polar Jets Accretion with latitude-dependent angular momentum and radial magnetic field can launch and sustain a jet Proga et al. 2003 Radio Jets • Electrons spiral around magnetic field at velocities close to light • Emit radio-X-rays “nonthermal” emission radio Chandra X-ray Observatory NASA’s X-ray Eye on the Universe Launched in 1999 Actual Chandra First Light • Point source to focus telescope • PKS0637-75, quasar at large distance (z=0.5, 3 Gpc) • Shadow on side! • Known to have radio jet • X-ray Jet visible: 5” long, 200,000 lyrs X-ray/Radio Jets in Quasars: M87 Galaxy M87 jet in X-ray, radio and optical MS0735.6 Radio/X-ray 3C273 X-ray More jets! Cygnus A radio Accretion Disk Winds • Wind blown off surface of accretion disk • Accelerated by radiation pressure • High velocity gas observed X-ray source Proga et al. 2000 AD surface How do SMBHs form and grow? • • • • Secular: accreting from within the galaxy Group: accretes from within the group of galaxies Cosmological: accretes from cold dark matter filaments Major Mergers: Hopkins et al (2008)
