Is There AN Age-Spread among Low-Mass Members of the Alpha Persei Cluster? -- CYCLE3 High

Details Is There AN Age-Spread among Low-Mass Members of the Alpha Persei Cluster? -- CYCLE3 High Is There AN Age-Spread among Low-Mass Members of the Alpha Persei Cluster? -- CYCLE3 High

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4345k&link_type=abstract

HST Proposal ID #4345

Computer Science

Hst Proposal Id #4345 Cool Stars

Scientific paper

We propose to search for visual binaries having component magnitude differences not exceeding 1 mag, and separations >= 0.05" in the relatively young open cluster Alpha Persei (~ 7-8 x 10^7 yrs). The candidate sample consists of those K and M dwarfs between V=14 and 16 which lie more than 0.3 mag above the fiducial single-star main sequence, and which are believed to be members on the basis of proper motions, spectral type, and strong H-alpha emission. These stars either represent a group of stars younger than the majority of Alpha Per members by factors of 3 to 10, or are binaries having nearly equal components. If these stars are binaries, then nearly half of them should have separations >= 8 AU and periods >= 21 years and thus be detectable as visual binaries with the PC. If the stars are binaries with separations < 8 AU, most of them should be identifiable as spectroscopic binaries (either as SB2's or because their radial velocities are deviant from the cluster mean) using high S/N echelle spectra to be obtained at the Keck Telescope. If binarity is excluded for these stars, then we will conclude that they must owe their displacement above the single star main sequence to youth, and we will be able to directly measure the time spread of star formation within the Alpha Persei cluster.

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