The distance to the T Tauri stars in Taurus determined
from their rotational properties
Astronomy & Astrophysics, 322, 825, (1997)
We have determined the average distance to the young stars in the
Taurus star formation region through their rotational
properties. While most other distance estimates to star forming
regions give the distance
to the associated molecular clouds, the method used here gives the
distance to the stars.
Our statistical method assumes that the photometric variations
are due to surface starspots that co-rotate with the equatorial
surface speed and the rotation axes of the stars are randomly
distributed. Furthermore, we pay much attention to possible
A ``best fit'' distance of (152 +- 10) parsecs is
derived from our sample of 25
weak line T Tauri stars in Taurus. This is within the
range of distances found for the molecular cloud (140 pc - 160 pc)
and confirms that the T Tauri stars are embedded within.
Alternatively, the agreement of the distances to the stars and dark
along with their intimate sky location,
lends support to the interpretation
and assumptions. This means that we find a random orientation of
the rotation axes, which excludes a preferential orientation that
might be caused by large
scale magnetic fields in the molecular cloud.
Another aspect is that our results seem to exclude
strong differential rotation for the T Tauri stars.
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