Triggered Star Formation and Evolution of T-Tauri stars in and around Bright-Rimmed Clouds
Neelam Chauhan, A. K. Pandey, K. Ogura, D. K. Ojha, B. C. Bhatt, S. K., Ghosh, P. S. Rawat

TL;DR
This study provides evidence for small-scale sequential star formation in bright-rimmed clouds, showing age gradients, evolution of T-Tauri stars, and variations in mass functions, supported by photometry and infrared data.
Contribution
It offers a quantitative test of the sequential star formation hypothesis in BRCs, extending previous work with new observations and deeper data, and analyzes star evolution and mass functions.
Findings
Age gradients observed in BRCs support sequential star formation.
WTTSs are generally older than CTTSs, indicating evolutionary progression.
Mass functions vary with BRC morphology, with steeper MF in B/C types.
Abstract
The aim of this paper is to quantitatively testify the "{\it small-scale sequential star formation}" hypothesis in and around bright-rimmed clouds (BRCs). As a continuation of the recent attempt by Ogura et al. (2007, Paper I), we have carried out photometry of four more BRC aggregates along with deeper re-observations of 2 previously observed BRCs. Again quantitative age gradients are found in almost all the BRCs studied in the present work. Archival Spitzer/IRAC data also support this result. The global distribution of NIR excess stars in each HII region studied here clearly shows evidence that a series of radiation driven implosion (RDI) processes proceeded in the past from near the central O star(s) towards the peripheries of the HII region. We found that in general weak-line T-Tauri stars (WTTSs) are somewhat older than classical T-Tauri stars (CTTSs). Also the fraction…
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