<p class="content_title1"><b>TUESDAY, FEBRUARY 12 - EPS</b><br></p>
<font style="font-family: arial,sans-serif;" size="2"><span style="border-collapse: separate; color: rgb(0, 0, 0); font-size: 18px; font-style: normal; font-variant: normal; font-weight: normal; letter-spacing: normal; line-height: normal; text-indent: 0px; text-transform: none; white-space: normal; word-spacing: 0px;"><font style="font-family: Times New Roman; font-style: normal; font-variant: normal; font-weight: normal; font-size: 18px; line-height: normal; font-size-adjust: none; font-stretch: normal;"><font style="font-family: arial,helvetica,sans-serif;" size="2"><b>2:00 PM </b><br>
"Some recent paleomagnetic, geologic, and geophysical insights into impact cratering in the solar system."<br><br></font><font size="2"><span style="font-family: arial,helvetica,sans-serif;">Ian Garrick-Bethell, MIT</span></font><br>
<font size="2"><span style="font-family: arial,sans-serif;"><br>EPS Faculty Lounge, 4th floor, Hoffman Laboratory, 20 Oxford Street</span></font><br><br></font></span></font><b><br></b><p class="content_title1"><b>THURSDAY, FEBRUARY 14 - CfA</b><br>
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<p><b>11:00 am:</b> <a href="http://www.cfa.harvard.edu/itc/events/thu.htm">Institute for Theory and Computation (ITC) Colloquium</a>. <br></p><p>"Gas Giants and Rocky Planets Around G and M Dwarfs" <br></p><p>
Dr. Doug Lin,
University of California, Santa Cruz. <br></p><p>Pratt Conference Room, 60 Garden St., CfA<br>
</p><p><strong>Abstract:</strong> Outstanding issues in the sequential
accretion scenario for gas giant planet formation include, 1) the
retention of dust grains in the presence of gas drag and that of cores
despite type I migration, 2) time scale for gas giant formation, 3)
halting migration at stellar proximity, and 4) the structural and
dynamical diversities. In these context, we investigate the influence
of the snow line and other transition regions in MRI induced turbulent
protostellar disks and show that they naturally provide retention
barriers for planetary building blocks. We also examine the role of
protoplanetary disks in speeding up the gas giant formation process and
the dynamical consequences of rapidly emerging gas giant planets. We
present planetary population synthesis which reproduce the observed
distribution of extra solar gas giants. Radial velocity and transit
surveys will soon be able to detect Earth-mass rocky planets close to G
and M main-sequence dwarf stars. There are many several avenues through
which such planets may be formed. Although rocky planets may be formed
in situ from the grains which migrated to the stellar proximity, their
mass is likely to be severely limited by dynamical isolation. More
massive rocky planets can form near the snow line barrier and migrate
to their proximity of their stars with or without the presence of gas
giant planets. Their statistical properties will provide a caliberation
on the efficiency of migration and the frequency of rocky planets in
the habital zone.</p><br>