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    Understanding the role of carbon in ultraviolet extinction along galactic sight lines
    (2011-11-22) Parvathi, V. S.; Sofia, U. J.; Murthy, J.; et al.
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    Hydrodynamic simulation coupled to chemical evolution in the star forming regions
    (2011-11-22) Majumdar, Liton; Das, Ankan; Chakrabarti, Sandip K.; et al.
    Chemical composition of a molecular cloud is highly sensitive upon the physical properties around that region. In order to have the more realistic knowledge around the star forming region, a two dimensional hydrodynamical flow is considered during the collapsing phase of a proto-star. Total variation diminishing scheme (TVD) is used to solve the set of hydrodynamical equations. Arm with this sophisticated hydrodynamical model, we couple our reasonably large chemical network including gas phase as well as grain phase chemical network, to study the chemical evolution during collapse of a protostar. Chemical evolution are studied by assuming constant temperature throughout the simulation as well as considering the temperature variation from the hydrodynamical model. It is noticed that Simulation results are highly sensitive upon the dynamic behavior of the collapsing Cloud.
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    Transfer of radiation in H₂CS molecule in interstellar space
    (2011-11-22) Sharma, Mohit; Sharma, Monika; Verma, U. P.; et al.
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    Star formation activity around NGC7538-IRS9 region
    (2011-11-22) Mallick, K. K.; Ojha, D.K.; Dewangan, L.K.; et al.
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    Interstellar extinction: Amorphous carbon and nanodiamonds
    (2011-11-22) Rai, Rakesh K.; Rastogi, Shantanu
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    Interstellar elemental depletion
    (2011-11-22) Haris, U.; Preethi, K.; Gudennavar, S. B.; et al.
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    Compolation of interstellar lines
    (2011-11-22) Preethi, K.; Gudennavar, S. B.; Bubbly, S. G.; et al.
    We have collated absorption line data toward 3014 stars (Fig. 1) in order to create a unified database of interstellar column densities. These data have been taken from a number of different published sources and include many different species and ionizations. The preliminary results from our analysis show a tight relation between N(H) and E(B-V) i.e. [N(H)/E(B-V)=6.12x10²¹]. Similar plots have been obtained with many different species, and their correlations along with the correlation coefficients are presented.