ISSN:
1572-946X
Keywords:
star formation
;
molecular lines
;
radiation transfer
;
Orion KL
Source:
Springer Online Journal Archives 1860-2000
Topics:
Physics
Notes:
Abstract The data of the line series CH3CN 8(K) − 7(K) K = 0 − 7 and line CS J = 3 − 2 were taken simultaneously. At beam size of 16″ the emissions of CH3CN and CS have a common center position located near IRc2 with deviations Δα ∼ -8″ and Δδ ∼ 5″. The observed data show that in Orion KL core the integrated intensities of the two species have double peaks separated by a space of 14″. The 2-dimension Gaussian fitting plots (FWHM) are ellipses ofD maj = 26″ andD min = 22″ for CH3CN 8(K) − 7(K) K = 3 − 6 andD′maj = 39″ D′min = 31″ for CS J = 3 − 2 at a distance about 450 pc. Towards the multiple line emission region of CH3CN 8(K) − 7(K) K = 3 − 6, using a simplified very large velocity gradient model to solve the statistical equilibrium and radiative transfer equations, we find to fit the observed results, the optimum physical parameters and kinetic temperatureT k∼ 120 K, densityn(H a) ∼ 1.2 × 105 cm−3, velocity gradientV gr∼ 92 km s−1 pc−1 and the local abundance of CH3CNF ab∼ 3 × 10−8. However towards the region of single line emission of CS J = 3 − 2 we have to use LTE and the optical thin approximation on the assumption ofT k= 120 K to obtain the lower limits of column density and then, an averaged abundance of CS of 6 × 10−8.
Type of Medium:
Electronic Resource
URL:
http://dx.doi.org/10.1007/BF00626871
Permalink
