Roland DiehlIAU Beijing Aug 2012 The ISM throughout the Galaxy 26 Al Radioactivity Positron Annihilation Roland Diehl MPE Garching, Germany.

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Presentation transcript:

Roland DiehlIAU Beijing Aug 2012 The ISM throughout the Galaxy 26 Al Radioactivity Positron Annihilation Roland Diehl MPE Garching, Germany

Roland DiehlIAU Beijing Aug 2012 Radioactivity in Astrophysics – an Example rod/26alnucl p n  Al Mg

Roland DiehlIAU Beijing Aug 2012 ISM Working Meeting, MPE, 25 Jul 2012 Roland Diehl 3

Roland DiehlIAU Beijing Aug 2012 Inner Galaxy Cygnus Orion Vela Sco-Cen Massive-Star Nucleosynthesis in the Current Galaxy: Exploiting the Message from 26 Al  -rays

Roland DiehlIAU Beijing Aug 2012 Hot-Gas Kinematics throughout the Galaxy:  Account for Instrumental Line Width (~3 keV)  Extract Additional (astrophysical) Broadening  Doppler velocity  ~1.4 ±0.35 ±0.3 keV Consistent with Expectation from Galactic Rotation (~1.35 keV) 175 ± 45 km s -1

Roland DiehlIAU Beijing Aug 2012  Clear Doppler Shifts  velocity resolution <100 km/s Instrumental line 26 Al line

Roland DiehlIAU Beijing Aug 2012 Hot gas streaming away from star-forming clouds  Enhanced star formation in inner  spiral arms  Stars vs. gas/parental-cloud  motion incurs one-sided  outflow  forward in GalRotation

Roland DiehlIAU Beijing Aug 2012  Annihilation  -rays are dominated by a Bright Inner-Galaxy Component  The 26 Al e+ Produced in the Disk (82%) are a Minor Contribution  Annihilation  -ray Emission Presents a Puzzle:  e+ Sources ?  Propagation !!  Annihilation Knödlseder Weidenspointner Bouchet+ 2010

Roland DiehlIAU Beijing Aug 2012  Nucleosynthesis  Accreting Binaries  Pulsars  SMBH?  Dark Matter?  Only Gamma Rays Can Tell  Locations?? Prantzos et al., RMP 83 (2011)

Roland DiehlIAU Beijing Aug 2012 Could e+ be transported from disk to central region of Galaxy?  Large-scale transport in halo magnetic field Irregular Toroidal Poloidal Han 2001 Sources of Positrons and Annihilation Sites -> Nikos Prantzos 2005 SPI/INTEGRAL 511 keV (Knödlseder et al. 2005)

Roland DiehlIAU Beijing Aug 2012  Radioactivity  -rays provide a different view  Emissivity Independent of complexity from environment (density, temperature)  Trace diluted ejecta at late phases = hot ISM  ISM around massive-star regions:  26 Al kinematics  Superbubble blow-out in forward directions  e + transport through chimneys & halo? Irregular Toroidal Poloidal Han 2001

Roland DiehlIAU Beijing Aug 2012 The Orion Region as Test Case (Laboratory)  Mixing of SN Ejecta into Multi-Phase ISM? Simulations:  Trace Evolution of Massive-Star Activity in Parental Cloud Fierlinger, Burkert, Diehl, et al. Diehl et al HI