Other
Scientific paper
Feb 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991phdt........51p&link_type=abstract
Thesis (PH.D.)--THE PENNSYLVANIA STATE UNIVERSITY, 1991.Source: Dissertation Abstracts International, Volume: 52-12, Section: B,
Other
Scientific paper
As part of a continuing study of magnetic activity in late-type stars, seven Weak-Lined T Tauri stars (WTTs) were observed. Spectra were obtained with the Kitt Peak National Observatory 2.1m telescope, using the Fiber Optic Echelle spectrograph (FOE). The objects are members of the Taurus-Auriga and Ophiuchus star-forming regions. They were observed for a total of eight nights during two observing runs. Accurate spectral types, rotational velocities (vsin i), and radial velocities were determined for each of the objects. The average radial velocity of the program stars in the Taurus-Auriga cloud is 17.77 +/- 0.59 km s^{-1} and the average radial velocity in the direction of Ophiuchus is -3.85 +/- 1.06 km s^{-1}. The data were examined for variations in the equivalent width of the Li 6708A line which is an important calibrator of stellar ages. The line was found to be significantly variable in four of the seven stars. This variability is not correlated with any other stellar activity. The first two Balmer lines, as well as the CaII (H, K, and infrared triplet), were also studied. Comparisons of these results with previous studies of the sun and RS CVn binaries have shown both similarities and differences in their behavior. The strengths of the excess emission in these systems are generally comparable, although no definite rotational modulation is seen. It appears that activity on the WTTs is either more uniformly distributed across the stellar disk or more random than activity in the RS CVn systems. Based on the results, it is concluded that the WTTs are intermediate between the sun and the most active RS CVn systems. They are similar in the gross properties of their activity, but they show detailed differences. The most active systems in this study mimic the behavior of the most active RS CVn systems.
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