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Photoionisation of Supernova Driven, Turbulent, MHD Simulations of the Diffuse Ionised Gas

Photoionisation of Supernova Driven, Turbulent, MHD Simulations of the Diffuse Ionised Gas . Jo Barnes 1 , Kenny Wood 1 , Alex Hill 2. [1]University of St Andrews , [2] CSIRO Astronomy and Space Science. Outline. Observations of the ISM MHD and radiative transfer simulations

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Photoionisation of Supernova Driven, Turbulent, MHD Simulations of the Diffuse Ionised Gas

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  1. Photoionisation of Supernova Driven, Turbulent, MHD Simulations of the Diffuse Ionised Gas Jo Barnes1, Kenny Wood1, Alex Hill2 [1]University of St Andrews, [2] CSIRO Astronomy and Space Science

  2. Outline • Observations of the ISM • MHD and radiative transfer simulations • Fractal models of the ISM • Scattered Light • How far can photons travel in the DIG? • Conclusions

  3. H [N II]/H [S II]/H [S II]/[N II] Observations: WHAM Survey • All sky survey of Hα (Haffner et al. 2003,2010) • Wide area surveys of [NII] λ6584 and [SII]λ6716 (Reynolds et al 1998, Hausen et al, 2002) • Filaments, loops and HII regions • [NII]/Hα and [SII]/Hα increase with height above midplane(Haffner 1999) • Additional heating mechanism (Reynolds 1999)

  4. MHD simulations • MHD simulations of ISM from Hill et al. 2012 • Include type Ia and core collapse supernovae, set off at galactic supernova rate • 3/5 of core collapse distributed to simulate superbubbles in the gas. • Do not include photoionisation heating

  5. Monte Carlo Radiative Transfer • Monte Carlo radiation transfer code of Wood et al. 2004. • Includes ions of H, He, C, N, O, Ne, S • Outputs 3D temperature and ionisation structure • Include additional heating sources for diffuse ionised gas in the Milky Way.

  6. Simulation Setup MHD DL DL+DIG • Subsection of MHD simulations with z = ±2kpc • 24 ionising sources with scaleheight63 pc (Maiz-Apellaniz 2001) • Ionizing luminosity 0.5<Q<10 x 1049 s-1 kpc-2. • Repeating boundary conditions to simulate semi-infinite simulation box N (cm-2)

  7. Hα and HI

  8. Hα Scale height Perseus Arm, H = 500 pc Q=10 x 10 49s-1kpc-2, H = 150 pc

  9. Fractal models of the ISM • MHD simulations have a lower density above the plane than observed in the Galaxy. • Average Column densities above 1kpc: MHD = 2.4 x 1018cm-2 DL+WIM= 2.4 x 1019cm-2 Fractal= 3.0x 1019cm-2 • Q=16 x 1049 s-1 kpc-2 • Additional heating: • G = 4 x 10-26neergs cm-3s-1 + Perseus Arm + Simulation: 2<z<2kpc +simulation: 1.8<z<1.8 kpc

  10. Scattered Light • Monte Carlo scattered light code. • Look at scattering of photons from HII regions • Include effects of dust scattering and absorptions in the DIG

  11. Scattered Light Maps HII region Total Diffuse gas = +

  12. Scattered Light

  13. Distance Travelled by Ionising Photons • Ionising photons travel through low density ‘bubbles’ close to the midplane • Need very few photons to travel to the top of the simulation box. • Higher ionising luminosity = larger distance • Photons with higher energy travel further than those with low energy Total distance Reprocessed photons

  14. Conclusions • Photoionisation of MHD simulations produces general Hα and HI with different scale heights • Able to reproduce general trends that we see in the Milky Way • Fractal models produce line ratios and scale heights similar to those in the Perseus Arm • But structure not the same as observed • Along many sightlines scattered light has a very small impact on the observed light. Along other sight lines, particularly close to the midplane, scattered light may have a significant effect on the intensity of light observed. • Only a small number of photons are required to travel large distances to ionise the DIG, but enough are able to reach the top of the simulation box and ionise the gas

  15. Distance Travelled by Ionising Photons Q = 10 x1049 s-1 kpc-2 Q = 1 x1049 s-1 kpc-2 Q = 0.5 x1049 s-1 kpc-2

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