Physical Processes In The Interstellar Medium

By Vanessa Hertzog. 2016

692 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/f0e5a3aae1a1f6d2e07b39d9461ce00c7db8d5cb

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Citations in the corpus

STARS, GAS, AND DARK MATTER IN THE SOLAR NEIGHBORHOOD (2015, methodology): “(2009) find a local density of 4.9 10 3 ́ - WD pc 3 - , which is in good agreement with the previous estimate of 5 0.7 10 3 ( )  ́ - WD pc 3 - by Holberg (2002), although it is somewhat less than the estimate of 6.0 10 3 ́ - WD pc 3 - by Reid (2005). Assuming a scale height h 325 1 = pc, Sion et a”
Physical Processes in the Interstellar Medium (2014, background): “…80° 60° 40° 20° 0° 340° 320° 300° 280° 260° 240° 220° 200° 180°170° 150° 130° 110° 90° 70° 50° 30° 10° 350° 330° 310° 290° 270° 250° 230° 210° 190° Beam classic example is line emission from the hydrogen atom itself in the Lyman, Balmer, Paschen, etc. series (e.g. Spitzer, 1978; Osterbrock, 1989).”
GIANT SPARKS AT COSMOLOGICAL DISTANCES? (2014, background): “Historically, cosmic rays were the first to be suggested as ionizing sources for the diffuse ISM (see Spitzer 1978).”
Before the first supernova: combined effects of H II regions and winds on molecular clouds (2014, unknown): “Rs is not easy to estimate in inhomogeneous gas, but we plot for comparison Spitzer evolution curves for Rs = 1.5, 2.5, 5.0 and 7.5 pc. This allows us to gauge qualitatively the effect of gas leakage and/or winds on the expansion of the HIIRs. The effect of either gas leakage or winds on the bubble ”
The Hα surface brightness–radius relation: a robust statistical distance indicator for planetary nebulae (2015, background): “(2011); RH02 – Rauch, Heber & Werner (2002); RK99 – Rauch et al. (1999); RK04 – Rauch et al. (2004); RR14 – Reindl et al.”
GRACKLE: a chemistry and cooling library for astrophysics (2016, background): “(2011); 8 – Shavitt (1959); 9 – Ripamonti (2007); 10 – Kreckel et al.”
MOMENTUM INJECTION BY SUPERNOVAE IN THE INTERSTELLAR MEDIUM (2014, background): “Similar to the case of single SNe, however, cooling of the interior implies that a constant asymptotic momentum is reached shortly after the last SN event.”
Theoretical Challenges in Galaxy Formation (2016, background): “The momentum input by direct absorption of UV photons (single scattering) seems sub-dominant (Arthur et al. 2004, Krumholz & Matzner 2009, Mathews 1969, Sales et al. 2014, Spitzer 1978).”
How to Calculate Molecular Column Density (2015, background): “…radiation is traveling is uniform at an excitation temperature Tex, defined as: Tex = hν/k ln ( nl gu nu gl ) , (20) 1 Draine (2011) points out that Spitzer (1978) uses the opposite convention, that radiation propagates in the direction of decreasing optical depth. where n is the density (cm−3)…”
The dust content of galaxies from z = 0 to z = 9 (2016, background): “The modelling of their IR spectral energy distribution (SED) has been especially improved within the past 10-20 years with the arrival of far-IR (Spitzer, Herschel) and sub-mm (Herschel, Submillimetre Common-User Bolometer Array (SCUBA), Balloonborne Large Aperture Submillimeter Telescope (BLAST), a”
Analyzing Inverse Problems with Invertible Neural Networks (2018, background): “The process is governed by the complex interplay of competing physical agents such as gravity, turbulence, magnetic fields, and radiation; with stellar feedback playing a decisive regulatory role [37].”