We propose to search for far-infrared emission from remnant dusty
 disks around 16 solar type stars that are members of the 30 Myr old
 open cluster IC2602.  According to the accepted models, pre-main
 sequence gas and dust disks (like those around classical T Tauri
 stars) agglomerate into planetesimals in a runaway process, leaving
 only large bodies and very little of the original gas and dust
 particles by an age of order 10 Myr.  Subsequent collisions of the
 planetesimals create a new population of small particles which
 should produce detectable IR excesses around young main sequence
 stars.  Thus, these Vega-type disks can be interpreted as signposts
 of planet formation.   IC2602 is the youngest nearby open cluster
 observable by ISO whose age is older than 10 Myr, and thus ISO
 photometry of G dwarfs in IC2602 may provide the best estimate
 of the fraction of solar mass stars that form planets.  In order
 to determine this fraction so that small number statistics do
 not dominate, a sample size of at least 20 stars is needed.  A
 GTO program will also search for debris disks around G dwarf
 members of IC2602; however, based on our ROSAT xray images of the
 cluster, we believe that only 4 of the 10 stars proposed by the
 GTO team are actually members of the cluster.  By contrast, the
 16 stars on our target list are confirmed as members by the xray
 data and by new optical photometry and high resolution spectroscopy.
 Our proposed observations are therefore essential to meeting the
 original goals of the GTO program and will insure that ISO data
 capable of verifying the presence or absence of dust associated
 with young planetary systems will be obtained for a statistically
 significant sample of ZAMS G dwarfs.  Moreover, our sample is
 large enough to enable deeper physical understanding of the
 planet-formation process via correlation of the presence of debris
 disks with the observed stellar rotational velocities.