| Name: | Avi Mudgal |
| Affiliation: | St. Xavier's College, Mumbai |
| Conference ID : | ASI2024_308 |
| Title : | Numerical Modelling of the Interstellar Medium Towards the Star Cluster NGC 6231 |
| Authors : | Avi Mudgal, Katherine Rawlins |
| Authors Affiliation: | Avi Mudgal, Katherine Rawlins (St. Xavier's College, Mumbai - 400001, India) |
| Mode of Presentation: | Poster |
| Abstract Category : | Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Abstract : | Detailed modelling of an H2 -bearing region using the spectral simulation code CLOUDY was
performed. The chief aim was to present a self-consistent calculation of the thermal,
ionization and chemical balance through numerical models and reproduce the observed
column densities to derive the underlying physical conditions in the Galactic ISM towards the
star cluster NGC 6231. The modelling inferred column density values of H 2 ground electronic
state rotational levels (J = 0 – 7), CO, C I fine-structure states and relative populations of
various elements reported in Marggraf et al. (2004) using spectra from Far Ultraviolet
Spectroscopic Explorer (FUSE). The best-fitting model concluded that the cloud was
subjected to a strong UV radiation field (χ = 10 G_0 ) along with enhanced X-ray radiation and
cosmic ray ionization rate. We find indications that the interstellar medium towards this star
cluster could be an X-ray dominated region. The density, temperature and gas pressure in the
absorbing region are also constrained, and they suggest that the cloud is cool and diffuse.
Turbulent pressure is identified as a significant constituent of the total pressure that increases
at the deeper end of the cloud. The various heating and cooling processes associated with the
cloud are also studied. We compare our detailed model with that presented by Marggraf et al.
(2004) and also investigate X-ray sources in the vicinity of the modelled interstellar region in
order to corroborate our model. |
