A T Tauri star is a type of young, pre-main sequence star that is still in the process of forming. They are typically less than 10 million years old and are found in regions of active star formation.
The spectral energy distribution of a T Tauri star refers to the amount of energy emitted by the star at different wavelengths. It is characterized by a steep rise in the infrared region due to the presence of a circumstellar disk, and a drop off in the ultraviolet region due to absorption by dust grains.
The spectral energy distribution of a T Tauri star can be studied through multi-wavelength observations, including infrared, optical, and ultraviolet. These observations can be used to construct a plot of the energy emitted by the star at different wavelengths and provide insights into the properties of the star's circumstellar disk.
The spectral energy distribution of a T Tauri star can provide information about the star's age, mass, and temperature. It can also reveal the presence of a circumstellar disk and help us understand the physical processes at work in the formation of these stars.
The spectral energy distribution of T Tauri stars is typically much steeper in the infrared region and shows a significant drop off in the ultraviolet. This is due to the presence of a circumstellar disk and the absorption of UV light by dust grains. In contrast, main sequence stars have a more gradual rise in energy towards the ultraviolet region.