Astrophysics of the Diffuse Universe

By M. Dopita, R. Sutherland. 2004

276 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/b4ebf5741dd477455df247f14df575f251a7ba9f

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Citations in the corpus

On the origin of radio emission in radio-quiet quasars (2008, background): “7.1 in Dopita & Sutherland 2003), implying an electron cooling time of t ′ff = 3 2 nkTe/Ėff = 2.6 × 1015n−1T 1/29 s (48) (note that this is somewhat shorter than tff for relativistic electrons).”
Atomic data from the Iron Project LIX. New radiative transition probabilities for Fe IV including fine structure (2004, unknown): “Key words. atomic processes – line: formation – radiation mechanisms: thermal – radiative transfer – ISM: HII regions – radio lines: galaxies”
Rest-frame ultraviolet-to-optical spectral characteristics of extremely metal-poor and metal-free galaxies (2011, methodology): “After exploring a wide range of nebular parameters (Table 1) which are appropriate to real H ii regions, we have derived average intensities of 119 emission lines relative to Hβ (Figure 1 for the 6 strongest metal lines) and temperatures of the nebular gas (Table 2) as a function of metallicity.”
THE 2013 RELEASE OF CLOUDY (2013, background): “Texts that review this field include Spitzer (1978), Dopita & Sutherland (2003), Tielens (2005), Osterbrock & Ferland (2006) (hereafter AGN3), and Draine (2011).”
Distant radio galaxies and their environments (2008, unknown): “…3 = Felten and Morrison (1966), 4 = Schwartz (2002), 5 = Osterbrock and Ferland (2006), 6 = Groves et al (2004), 7 = Groves et al (2004), 8 = Dopita and Sutherland (2003), 9 = Aller (1984), 10 = Dickson et al (1995), 11 = Morganti (2006), 12 = van Ojik et al (1997), 13 = Binette et al…”
The SAMI Galaxy Survey: shocks and outflows in a normal star-forming galaxy (2014, background): “In the case where the transverse magnetic field pressure dominates the gas pressure in the recombination zone of the shock, the density contrast becomes ne1 ne0 = √ 2 vsh vA = √ 2 σ vA , (5) where vA is the Alfvén velocity determined by the density and magnetic field (see Dopita & Sutherland 2003).”