T Tauri stars are usually found in less dense environments.

Like all T Tauri stars, it is very young, being only a million years old.

At this point, they are known as T Tauri stars and continue to contract, but much more slowly.

At this point in its evolution, the Sun is thought to have been a T Tauri star.

T Tauri star, it is extremely luminous.

After more contraction, a T Tauri star ignited and evolved into the Sun.

T Tauri stars like the young Sun have far stronger stellar winds than more stable, older stars.

The T Tauri stars, with masses less than twice the mass of our Sun, are thought to follow this process:

The star is the closest T Tauri star to the Solar System.

Jet-driven shocks are formed from jets of material sprouting off newborn T Tauri stars.

Young stellar groups can contain a number of infant T Tauri stars that are still in the process of entering the main sequence.

At the next stage the envelope completely disappears, having been gathered up by the disk, and the protostar becomes a classical T Tauri star.

These sparse populations of up to a thousand T Tauri stars are known as T associations.

Haro also discovered a number of T Tauri stars, one supernova, more than 10 novae, and one comet.

Similar wavelength-dependent radial velocity variations, also caused by starspots, have been detected on other T Tauri stars.

T Tauri stars generally increase their rotation rates as they age, through contraction and spin-up, as they conserve angular momentum.

Like classical T Tauri stars, many brown dwarfs are surrounded by disks of gas and dust which accrete onto the brown dwarf.

Other systems which often contain polar jets include cataclysmic variable stars, X-ray binaries and T Tauri stars.

Variability of T Tauri stars is due to spots on the stellar surface and gas-dust clumps, orbiting in the circumstellar disks.

Protoplanetary disks around T Tauri stars differ from the disks surrounding the primary components of close binary systems with respect to their size and temperature.

T Tauri stars are pre-main sequence stars in the process of contracting to the main sequence along the Hayashi track.

SU Aurigae is T Tauri Star in the Taurus-Auriga complex.

The constellation contains a number of molecular clouds (the Chamaeleon dark clouds) that are forming low-mass T Tauri stars.

Less massive T Tauri stars follow this track to the main sequence, while more massive stars turn onto the Henyey track.

Studies of T Tauri stars show that they are often accompanied by discs of pre-planetary matter with masses of 0.001-0.1 solar masses.