This study deals with Molecular Line Emissions in Star Forming Regions, we have
considered N98 an... more This study deals with Molecular Line Emissions in Star Forming Regions, we have considered N98 and N69 Infrared Bubble and molecular lines studied from them are CO, (13)CO, C(18)O, CN, HCN, HCO + , N_2H + . The data is obtained from Taeduk Radio Astronomy Observatory (TRAO), South Korea at 8μm (mid IR). Results: The CO is molecular line is highly abundant in both the IR Cloud, followed by significant amount of 13 CO and rest all are of very low intensity.
A review of Stellar Evolution through Astrophysical Multipurpose Software Environment (AMUSE) cod... more A review of Stellar Evolution through Astrophysical Multipurpose Software Environment (AMUSE) code and the variation of evolution time of star as the mass of star varies. The stellar evolution has dependence mainly on the mass of the star. So, to describe stellar evolution first a Hertzsprung-Russel (H-R) diagram is plotted for certain mass of stars in each stellar types. To see the variation of evolved time with mass the plotting of evolved time vs stellar mass was done.
This study deals with Molecular Line Emissions in Star Forming Regions, we have
considered N98 an... more This study deals with Molecular Line Emissions in Star Forming Regions, we have considered N98 and N69 Infrared Bubble and molecular lines studied from them are CO, (13)CO, C(18)O, CN, HCN, HCO + , N_2H + . The data is obtained from Taeduk Radio Astronomy Observatory (TRAO), South Korea at 8μm (mid IR). Results: The CO is molecular line is highly abundant in both the IR Cloud, followed by significant amount of 13 CO and rest all are of very low intensity.
A review of Stellar Evolution through Astrophysical Multipurpose Software Environment (AMUSE) cod... more A review of Stellar Evolution through Astrophysical Multipurpose Software Environment (AMUSE) code and the variation of evolution time of star as the mass of star varies. The stellar evolution has dependence mainly on the mass of the star. So, to describe stellar evolution first a Hertzsprung-Russel (H-R) diagram is plotted for certain mass of stars in each stellar types. To see the variation of evolved time with mass the plotting of evolved time vs stellar mass was done.
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considered N98 and N69 Infrared Bubble and molecular lines studied from them
are CO, (13)CO, C(18)O, CN, HCN, HCO + , N_2H + . The data is obtained from Taeduk
Radio Astronomy Observatory (TRAO), South Korea at 8μm (mid IR).
Results: The CO is molecular line is highly abundant in both the IR Cloud, followed
by significant amount of 13 CO and rest all are of very low intensity.
considered N98 and N69 Infrared Bubble and molecular lines studied from them
are CO, (13)CO, C(18)O, CN, HCN, HCO + , N_2H + . The data is obtained from Taeduk
Radio Astronomy Observatory (TRAO), South Korea at 8μm (mid IR).
Results: The CO is molecular line is highly abundant in both the IR Cloud, followed
by significant amount of 13 CO and rest all are of very low intensity.