The Old Feeble Coronae of Solar-like Dwarf Stars in the Arcturus Moving Group

Details The Old Feeble Coronae of Solar-like Dwarf Stars in the Arcturus Moving Group The Old Feeble Coronae of Solar-like Dwarf Stars in the Arcturus Moving Group

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8905b&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #89.05; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

The Arcturus Moving Group (AMG) is very likely a remnant of the merger of a dwarf galaxy with the Milky Way Galaxy in the distant past. This kinematically distinct group has members located very close to the Sun, allowing study of coronal activity on very old stars that would typically not be possible. We are investigating a sample of nearby AGM dwarfs to study the properties of stellar magnetic activity on old (7-8 Gyr), low metallicity stars. Our sample has metallicities between 0.4 and 0.04 solar, spectral types F9 K0, and distances less than 35 pc from the Sun. We have detected X-ray emission from two AMG dwarfs with the Chandra ACIS-S S3 BI detector during Cycle 7 and two further stars have been approved for observation in Cycle 8. The detected stars are HD199288 (G0 V, V=6.6, d = 21.6 pc, [Fe/H] = -0.68) and HD65583 (G8 V, V=6.9, d = 16.8 pc, [Fe/H] = -0.68) and their derived X-ray luminosities are 4.4 and 1.9 1026 erg s-1 respectively. These X-ray luminosities are somewhat less than the minimum solar Lx (range 6 -20 1026 erg s-1 ) but are comparable with that of the inactive, more metal rich ([Fe/H] = -0.42] G8 dwarf Tau Cet. All the detected source X-rays are very soft with energies of 0.2-0.3 keV, indicating very cool (˜ 1 MK) coronal temperatures.
These results were obtained and funded by CXO project 7200977.

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