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[Fe II] 1.64 μm features of Jets and Outflows from Young Stellar Objects in the Carina Nebula
Jong-Ho Shinn,Tae-Soo Pyo,Jae-Joon Lee,Ho-Gyu Lee,Hyun-Jeong Kim,Bon-Chul Koo,Hwankyung Sung,Moo-Young Chun,A.-Ran Lyo,Dae-Sik Moon,Jaemann Kyeong,Byeong-Gon Park,Hyeonoh Hur,Dae-Sik Moon 한국천문학회 2014 天文學會報 Vol.39 No.1
Shinn, Jong-Ho,Lee, Ho-Gyu,Moon, Dae-Sik IOP Publishing 2012 The Astrophysical journal Vol.759 No.1
<P>We present near-infrared (2.5-5.0 mu m) spectral studies of shocked H-2 gas in two supernova remnants, IC 443 and HB 21, which are well known for their interactions with nearby molecular clouds. The observations were performed with the Infrared Camera aboard the AKARI satellite. At the energy range 7000 K less than or similar to E(upsilon, J) less than or similar to 20,000 K, the shocked H-2 gas in IC 443 shows an ortho-to-para ratio (OPR) of 2.4(-0.2)(+0.3), which is significantly lower than the equilibrium value 3, suggesting the existence of non-equilibrium OPR. The shocked gas in HB 21 also indicates a potential non-equilibrium OPR in the range of 1.8-2.0. The level populations are well described by the power-law thermal admixture model with a single OPR, where the temperature integration range is 1000-4000 K. We conclude that the obtained non-equilibrium OPR probably originates from the reformed H-2 gas of dissociative J-shocks, considering several factors such as the shock combination requirement, the line ratios, and the possibility that H-2 gas can form on grains with a non-equilibrium OPR. We also investigate C-shocks and partially dissociative J-shocks as the origin of the non-equilibrium OPR. However, we find that they are incompatible with the observed ionic emission lines for which dissociative J-shocks are required to explain. The difference in the collision energy of H atoms on grain surfaces would give rise to the observed difference between the OPRs of IC 443 and HB 21, if dissociative J-shocks are responsible for the H-2 emission. Our study suggests that dissociative J-shocks can produce shocked H-2 gas with a non-equilibrium OPR.</P>