The Physics and Chemistry of the Interstellar Medium

By A. Tielens. 2005

1,157 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/7a49fc55d06135c32f9ad777ec296ee93b64b822

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Ralf Klessen
2. S. Glover
3. Mark R. Krumholz
4. P. Hopkins
5. T. Naab
6. E. Ostriker
7. L. Hernquist
8. R. Somerville

In Atomic and Molecular Physics, and Optics

1. R. Garrod
2. E. Herbst
3. E. Dishoeck
4. A. Tielens
5. H. Cuppen
6. P. Caselli
7. B. McGuire
8. S. Ioppolo

In Spectroscopy

1. Ralf Klessen
2. P. Caselli
3. Cecilia Ceccarelli
4. S. Glover
5. R. Garrod
6. E. Herbst
7. E. Dishoeck
8. V. Wakelam

Citations in the corpus

• Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “All theoretical calculations of grain lifetimes against destruction by SN shocks agree that they are much shorter than the ∼ 2 Gyr timescale of dust injection by stars (e.g. Jones et al. 1996; Tielens et al. 2005).”
• Programmable self-assembly in a thousand-robot swarm (2014, background): “…several groups have developed self-assembling “ cellular ” robots that can reconfigure into many morphologies to complete different grasping or locomotion tasks ( 11 ), or can act as programmable matter that can rapidly assemble into user-specified tools such as a wrench or key ( 12 , 13 ).”
• Polycyclic aromatic hydrocarbon processing in a hot gas (2009, methodology): “Here, we will modify the analysis of Tielens (2005) for H-loss by UV pumped PAHs to determine the parameters for carbon loss.”
• CO Isotopologues in the Perseus Molecular Cloud Complex: the X-factor and Regional Variations (2008, background): “Curve of Growth Assuming LTE, the photon escape probability for a slab as a function of optical depth, ( ), can be written as (Tielens 2005) ( ) ¼ 1 exp ( 2:34 )½ =4:68 if < 7; 1=4 ln ffiffiffi p 1=2 if > 7; 8>< >: ð10Þ and the Doppler broadening parameter, b, is related to the atomic weight, A,…”
• On the relationship between molecular hydrogen and carbon monoxide abundances in molecular clouds (2010, background): “Given these assumptions, the relationship between NCO and τ10 becomes (Tielens 2005) τ10 = A10c 3 8πν310 g1 g0 f0 [ 1− exp (−E10 kT )] NCO ∆v , (12) where A10 is the spontaneous radiative transition rate for the J = 1 → 0 transition, ν10 is the frequency of the transition, E10 = hν10 is the…”
• On-line database of the spectral properties of polycyclic aromatic hydrocarbons (2007, background): “us and nwchem codes, as well as on the expected accuracy achieved, can be found elsewhere [32a–c]. 2.2 The sample of molecules A wide range of PAHs and related species are thought to exist in the ISM [16b]. The total of 40 molecules selected in this work, ranging in size from naphthalene and azulene”
• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution (2009, background): “This growth is limited, however, because there are many small grains – which dominate the total grain surface area – over which the ice should be distributed; if all the condensible gas freezes out, the thickness of the ice mantles is still only 175 Å (Draine 1985).”
• CO-dark gas and molecular filaments in Milky Way-type galaxies (2014, methodology): “We also assume a constant metallicity and dust-to-gas ratio, whereas the Milky Way galaxy has a slight metallicity gradient with Galactocentric radius. Luck et al. (2011) find that the iron distribution can be fit by the relationship [Fe/H] = −0.”
• The SILCC (SImulating the LifeCycle of molecular Clouds) project – I. Chemical evolution of the supernova-driven ISM (2014, methodology): “Following McKee & Ostriker (1977) and Tielens (2005), we can estimate the VFF of the hot phase that we expect for a given SN rate and mean gas density.”
• 2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules (2018, background): “…gas required to ensure that these collisions dominate the distribution over radiative processes is the critical density (ncr), given by Equation A7 (Tielens 2005) where Aul is the Einstein A coefficient (s−1) and γul is the collisional rate coefficient (cm3 s−1) for the transition from upper state…”