Young forming stars vary in brightness on various timescales and amplitudes. Investigating these variations at different wavelengths does allow us to infer the physical reasons for the variability. These could for example be: Changes in the mass accretion rate, changes in the line of sight column density caused by material in the protostellar accretion disk, hot or cold spots and rotation of the central star, or more likely a combination of these.
We are studying the long term changes of the mass accretion rate in young stars as well as the structure and properties in the inner accretion disks using long term, high cadence, multi filter datasets. These are either taken with our in house observatory (Beacon Observatory), taken as part of our HOYS-CAPS Citizen Science Project, or other publicly available datasets such as e.g. VVV(-X), GAIA, PTF, ASAS-SN or AAVSO.