Chromospheric activity in the late A- and early F-type stars of open clusters - II. Pleiades and Alpha Persei

Details Chromospheric activity in the late A- and early F-type stars of open clusters - II. Pleiades and Alpha Persei Chromospheric activity in the late A- and early F-type stars of open clusters - II. Pleiades and Alpha Persei

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.315...24r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 315, Issue 1, pp. 24-30.

Astronomy and Astrophysics

Astronomy

5

Stars: Activity, Stars: Chromospheres, Stars: Late-Type, Open Clusters And Associations: Individual: Alpha Persei, Open Clusters And Associations: Individual: Pleiades

Scientific paper

We report observations of the Hei λ5876 (D3) line in the late A- and early F-type stars in the Pleiades and Alpha Persei star clusters used to determine chromospheric activity levels. This represents the first sample of young stars in this temperature range with chromospheric activity measurements. We find the same average activity level in the young early F stars as in Hyades-age stars and field stars. In addition, the young star sample shows the same large star-to-star variation in activity as seen in the older stars. Thus, as a whole, chromospheric activity in this photospheric temperature range remains the same over nearly a factor of 100 in stellar age (50Myr to 3Gyr), in striking contrast to the behaviour of later-type stars. In the five late A stars we find three certain detections of D3 and one likely detection. This includes the bluest star yet observed with a chromospheric D3 line, Pleiades star HII 1362 at (B-V)0=0.22, making it one of the earliest stars with an observed chromosphere. The late A stars have D3 equivalent widths comparable to the weakest early F stars. However, when comparing D3 measurements in the young late A stars with older late A stars, we find evidence for a slight decrease in activity with age based on the large number of non-detections in the older stars. We find an apparently linear relationship between the activity upper limit and B-V over our entire range of B-V. Extrapolated blueward, this relationship predicts that the chromospheric D3 line would disappear for all stars at B-V ~0.13.

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