# Why is T Tauri So Dim?

I'm looking at stellar objects and doing some math here and...

Now, I can't find these values directly listed, but from it's relative magnitude and distance, (10.27, 471ly,) I calculate T Tauri to have an absolute magnitude of 4.47, and when I convert that to solar luminosities I get 1.39.

I've run that on objects for which I can find absolute magnitudes and solar luminosities listed, and I'm getting the correct values.

But every description of T Tauri stars I find says they are brighter than main sequence stars of equivalent mass. A main-sequence star about twice the mass of the sun should be much more than 1.39 times the brightness of the sun.

Now I must turn to people who actually know something about astronomy: Is the prototype T Tauri star "weird" in some way, and not actually typical of the class of objects that were named after it, or do I have some bad math or bad data here? What else could be the problem?

• Well T Tauri is a variable star, so its brightness may vary. Commented Feb 4, 2021 at 16:56

According to Herczeg & Hillenbrand (2014) the intrinsic bolometric luminosity of T Tau is about $$7L_\odot$$ (for an assumed distance of 479 light years).
T Tau is in a multiple system with a much lower mass companion (which contributes little to the luminosity), but this has led to a quite accurate mass determination of $$(2.12 \pm 0.10)\ M_\odot$$ (Kohler et al. 2015). Given a main-sequence mass-luminosity trend of around $$L \sim M^3$$, then it is apparent that T Tau has around the luminosity it would be expected to have on the main sequence. This would suggest that it has finished descending its Hayashi track in the HR diagram and is currently traversing, roughly horizontally, towards hotter temperatures and slightly rising luminosity, in excellent accordance with stellar evolutionary models (see below) if its age is $$\sim 2$$ Myr.
T Tau is only unsusual compared with most "T-Tauri stars" in that it has quite a high mass. Most "T-Tauri stars" are a solar mass or lower, and if found in young stellar clusters and associations with ages $$<10$$ Myr, you can see from the plot below that they would have higher luminosities than they end up with on the main sequence.