| Name: | Akhila D |
| Affiliation: | CHRIST(Deemed to be University) |
| Conference ID : | ASI2024_598 |
| Title : | Mid-infrared forbidden neon lines in Herbig Ae/Be stars |
| Authors : | Akhila D1, Blesson Mathew1, S Nidhi1, B Shridharan1, Suman Battacharyya1 |
| Authors Affiliation: | 1 CHRIST (Deemed to be University), Bangalore |
| Mode of Presentation: | Poster |
| Abstract Category : | Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Abstract : | Herbig Ae/Be (HAeBe) stars are intermediate-mass pre-main sequence stars characterized by the presence of emission lines in the spectrum and infrared excess in the continuum. They are considered as an intermediary between low-mass T Tauri stars and massive young stellar objects. In this study, we analyzed the moderate-resolution mid-infrared spectra of 76 well-known HAeBe stars using Spitzer InfraRed Spectrograph data. We have observed distinct emissions of [Ne II] at 12.81 μm and [Ne III] at 15.55 μm for a total of 36 sources. This is the largest sample of HAeBe stars showing forbidden neon lines in mid-infrared. Limited studies have been conducted on the detection of forbidden neon emission lines in low-mass young stellar sources and there is a lack of in-depth understanding on its characteristics and origin. Here, we are examining the correlations between neon lines with various spectral features, such as optical/infrared forbidden lines and Hα. Furthermore, we are analyzing neon line ratios to investigate a potential connection between the detected lines and the underlying emission mechanisms. We will also look into whether jets/outflows play a role in producing the high-energy photons needed to account for the large first ionization potential of neon (21.56 eV). [Ne II], being one of the commonly observed forbidden lines in our sources, serves as a tracer for either outflows or disk winds depending on the mass accretion rate. Examining the origin and formation of this line in HAeBe offers a means to expand our understanding of the gaseous region and serves as a probe for studying high-energy processes occurring there. Given that these lines are currently being detected in protostars using JWST, we aim to provide a strong foundation for future studies of young stars using the same. |
