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Pulsar V=5-50 AU/yr

How do we observe AU-scale structure? Pulsars, and optical depth imaging against extended radio continuum sources…. Pulsar V=5-50 AU/yr. CNM. *. Epoch 2. Epoch 1. Equivalent width variations.  EW = 0 within 2  for: 0823, 1133,1737, 2016 EW0 for 1929

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Pulsar V=5-50 AU/yr

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  1. How do we observe AU-scale structure? Pulsars, and optical depth imaging against extended radio continuum sources…. Pulsar V=5-50 AU/yr CNM * Epoch 2 Epoch 1

  2. Equivalent width variations • EW = 0 within 2 for: • 0823, 1133,1737, 2016 • EW0 for 1929 • TSAS: L=5-50AU, n~104 cm-4, • P~106 cm-3 K • Stanimirovic, Weisberg et al. (2010)

  3. Distance=350 pc, closest in the sample • ½ of LOS inside the Local Bubble. • HD178125 and HD180555 show NaI absorption as similar velocity  TSAS is within the LB! • LOS to B1929+10 pierces the LB wall for 50-60 pc. • Many diffuse clouds in this direction (Aquila Rift) condensing out of the LB wall or ablated nearby molecular gas • TSAS Tspin = 150-200 K • CNM/WNM ratio = only 7% •  TSAS properties/production influenced by the history/evolution of the Local Bubble What’s going on with B1929+10 ? PSR at ~330pc * Welsh et al. (2010)

  4. High optical depth Does the power spectrum extend down to AU-scales? • With different sources, essentially continuous coverage. • No observed power-law turbulent spectrum on scales: 1 to ~1000 AU. Kendall’s tau test for censored data: P(no correlation) ~60% • Inhomogeneity in Galactic distribution of TSAS + v.f.f.<~1% • TSAS is not pervasive. • If TSAS is tracing the end-scales of turbulence then turbulence may dissipate in bursts or active pockets, or it dissipates very fast. Low optical depth * : interferometric other: pulsars

  5. Does the power spectrum extend down to AU-scales? • With different sources, essentially continuous coverage. • No observed power-law turbulent spectrum on scales: 1 to ~1000 AU. Kendall’s tau test for censored data: P(no correlation) ~60% • Inhomogeneity in Galactic distribution of TSAS + v.f.f.<~1% • TSAS is not pervasive. • If TSAS is tracing the end-scales of turbulence then turbulence may dissipate in bursts or active pockets, or it dissipates very fast. * : interferometric other: pulsars

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