The X-Ray Environment During the Epoch of Terrestrial Planet Formation: Chandra Observations of h Persei

Details The X-Ray Environment During the Epoch of Terrestrial Planet Formation: Chandra Observations of h Persei The X-Ray Environment During the Epoch of Terrestrial Planet Formation: Chandra Observations of h Persei

2008-11-11

arxiv.org/abs/0811.1753v1

Astronomy and Astrophysics

Astrophysics

34 pages, 7 Figures, 2 Tables; Accepted for publication in The Astronomical Journal

Scientific paper

10.1088/0004-6256/137/2/3210

We describe Chandra/ACIS-I observations of the massive ~ 13--14 Myr-old cluster, h Persei, part of the famous Double Cluster (h and chi Persei) in Perseus. Combining the list of Chandra-detected sources with new optical/IR photometry and optical spectroscopy reveals ~ 165 X-ray bright stars with V < 23. Roughly 142 have optical magnitudes and colors consistent with cluster membership. The observed distribution of Lx peaks at Lx ~ 10^30.3 ergs/s and likely traces the bright edge of a far larger population of ~ 0.4--2 Msun X-ray active stars. From a short list of X-ray active stars with IRAC 8 micron excess from warm, terrestrial-zone dust, we derive a maximum X-ray flux incident on forming terrestrial planets. Although there is no correlation between X-ray activity and IRAC excess, the fractional X-ray luminosity correlates with optical colors and spectral type. By comparing the distribution of Lx/L* vs. spectral type and V-I in h Per with results for other 1--100 Myr-old clusters, we show that stars slightly more massive than the Sun (> 1.5 Msun) fall out of X-ray saturation by ~ 10--15 Myr. Changes in stellar structure for > 1.5 Msun stars likely play an important role in this decline of X-ray emission.

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