| Name: | Gautam Das |
| Affiliation: | Indian Institute of Science Education and Research Kolkata |
| Conference ID: | ASI2025_471 |
| Title: | Introducing Time Evolution into a Parameterised YSO Accretion Disk Model and Predicting Changes in Observational Signatures |
| Authors: | Gautam Das 1, Lynne Hillenbrand 2 |
| Authors Affiliation: | 1 Gautam Das Affiliation (Department of Physical Sciences, Indian Institute of Science Education and Research Kolkata, Mohanpur, Nadia, 741246, West Bengal, India)
2 Lynne Hillenbrand Affiliation (Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA) |
| Mode of Presentation: | Oral |
| Abstract Category: | Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Abstract: | During star formation, young stars have been observed to be quite dynamic, often associated with accretion disks and termed Young Stellar Objects (YSOs). FUOrs are a class of YSOs characterized by a rise in lightcurve brightness by a few orders of magnitude, followed by fading in decadal to century time scales. When we look at the lightcurves of FUOrs during their outburst epoch, we find that lightcurve profiles are quite different for each star. Thus, modelling the lightcurves of these objects is crucial to understanding how different components of these systems evolve during outbursts.
We use a simple parameterized model called YSOpy which couples passively irradiated dust disk, viscously heated gas disk, stellar photosphere and magnetospheric accretion funnel emissions. We develop a pipeline that tracks how various parameters of these emission components couple and evolve to generate the observed lightcurves in optical and near-infrared bands.
We use this pipeline for FUOrs like GAIA 17bpi, V960 Mon and HBC 722 to see how observational signatures change with time. This provides important insights into the disk-magnetospheric interactions throughout the cycle by enabling us to predict which parts of the model can be best observed at each point of the outburst cycle. We find that these stars can take very different evolutionary pathways during their transition from low to high state in an outbursting epoch. |
