Sleuthing the Dynamo: Hubble Space Telescope Faint Object Spectrograph Observations of Solar-Type Dwarfs in Young Galactic Clusters

Details Sleuthing the Dynamo: Hubble Space Telescope Faint Object Spectrograph Observations of Solar-Type Dwarfs in Young Galactic Clusters Sleuthing the Dynamo: Hubble Space Telescope Faint Object Spectrograph Observations of Solar-Type Dwarfs in Young Galactic Clusters

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...473..279a&link_type=abstract

Astrophysical Journal v.473, p.279

Astronomy and Astrophysics

Astronomy

20

Galaxy: Open Clusters And Associations: General, Stars: Coronae, Stars: Emission-Line, Be, Stars: Rotation, Ultraviolet: Stars

Scientific paper

We have used the Faint Object Spectrograph of the Hubble Space Telescope to record the ultraviolet emissions of solar-type [(B - V)0 ˜0.6 mag] dwarf stars in young galactic clusters: five in the Hyades (t 600 Myr); three in the Pleiades (t ˜ 70 Myr); and two in αPersei (t ˜ 50 Myr). Despite high levels of scattered light in the G130H (1140-1606 Å) spectra, the key C IV λ1549 blend was detected in all of the targets. The 105 K emission displays a dramatic decline from the youngest to the oldest stars of the sample, well correlated with rotational velocity; evidence of flaring in the most active of the G dwarfs; a wide spread in intensity among the Pleiades stars; but a small dispersion among the Hyades stars. The Mg II λ2800 emission is strongly enhanced in the younger stars, and the 2000 Å continuum is significantly elevated in the Hyades stars compared with the Sun. The hyperactive stars of the sample show an apparent saturation of their C IV emission at high rotational velocities, analogous to that seen in X-rays. The rotation-activity relations possibly exhibit mild curvature, in addition to the saturation, which nevertheless maps onto a simple power law in fX/fbol versus fCIV/fbol. The Sun apparently tracks a similar power law over the course of its magnetic activity cycle.
We discuss these results in terms of simple magnetic loop models. We show that the nonlinear power- law variation of CIV/fbol with rotational velocity (slope ˜1.5, contrary to the suspected linear dependence of the magnetic filling factor) very likely arises from a systematic increase in the base pressures of the dominant coronal loops compared with their counterparts on the Sun. The nonlinear X-ray/C IV power law (slope ˜1.7) separately indicates a significant increase in the mean apex temperature of the dominant coronal loops. We argue that the distribution of loop structures might change character from inactive stars like the Sun (dominated by X-ray-bright points and Active Region loops) to the hyperactive cluster stars (dominated by interregion large-scale structures or postflare loops).

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