J/MNRAS/406/1745 H2O in interstellar shock waves (Flower+, 2010) ================================================================================ Excitation and emission of H_2_, CO and H_2_ O molecules in interstellar shock waves. Flower D.R., Pineau des Forets G. =2010MNRAS.406.1745F ================================================================================ ADC_Keywords: Atomic physics ; Interstellar medium Keywords: molecular processes - shock waves - ISM: jets and outflows - infrared: ISM - submillimetre: ISM Abstract: The dissipation of kinetic energy that occurs in interstellar shock waves is accompanied by the emission of radiation. In the case of shocks that are propagating into mainly molecular gas, the emission occurs principally in lines of the species H_2_, H, O, CO and H_2_O. The relative intensities of these emission lines are indicative of the type and speed of the shock wave and of the physical conditions in the ambient gas. We present the results of computations of the intensities of these lines, for small grids of models of C- and J-type shock waves, and compare with the results of previous calculations. Our results should serve to aid the interpretation of observations made with the Herschel and other satellites. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablea3.dat 105 158 C-shocks : ortho-H_2_O line intensities tablea4.dat 106 157 C-shocks : para-H_2_O line intensities tablea5.dat 98 158 J-shocks : ortho-H_2_O line intensities tablea6.dat 98 157 J-shocks : para-H_2_O line intensities -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablea?.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Upper Upper level (1) 9- 15 A7 --- Lower Lower level (1) 17- 22 F6.1 K Eup Excitation energy of the upper level of the transition, relative to the 0 0 0 ground level 24- 32 F9.3 GHz nu Frequency of transition 34- 42 F9.3 um lambda Wavelength of transition 44- 50 E7.3 K.km/s v10n2e4 Line intensity, TdV, for shock speed vs=10km/s and n_H_=2x10^4^cm^-3^ (2) 52- 58 E7.3 K.km/s v20n2e4 Line intensity, TdV, for shock speed vs=20km/s and n_H_=2x10^4^cm^-3^ (2) 60- 66 E7.3 K.km/s v30n2e4 Line intensity, TdV, for shock speed vs=30km/s and n_H_=2x10^4^cm^-3^ (2) 68- 74 E7.3 K.km/s v40n2e4 ? Line intensity, TdV, for shock speed vs=40km/s and n_H_=2x10^4^cm^-3^ (2) 76- 82 E7.3 K.km/s v10n2e5 Line intensity, TdV, for shock speed vs=10km/s and n_H_=2x10^5^cm^-3^ (2) 84- 90 E7.3 K.km/s v20n2e5 Line intensity, TdV, for shock speed vs=20km/s and n_H_=2x10^5^cm^-3^ (2) 92- 98 E7.3 K.km/s v30n2e5 Line intensity, TdV, for shock speed vs=30km/s and n_H_=2x10^5^cm^-3^ (2) 100-106 E7.3 K.km/s v40n2e5 ? Line intensity, TdV, for shock speed vs=40km/s and n_H_=2x10^5^cm^-3^ (2) -------------------------------------------------------------------------------- Note (1): The levels are identified by J_K+_K-, where J is the rotational quantum number and K is its projection on the symmetry axis of the molecule; the '+' and '-' subscripts refer to the oblate and prolate symmetric top limits, respectively. Note (2): Where vs is the shock speed and n_H_ the pre-shock density. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Patricia Vannier [CDS] 01-Feb-2011