BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Talks.cam//talks.cam.ac.uk//
X-WR-CALNAME:Talks.cam
BEGIN:VEVENT
SUMMARY:Can we detect super-Earths in proto-planetary discs? - Giovanni Ro
 sotti (IoA)
DTSTART:20160119T130000Z
DTEND:20160119T140000Z
UID:TALK62367@talks.cam.ac.uk
CONTACT:Jean Teyssandier
DESCRIPTION:After the discovery of the first exoplanet in 1995 and the imp
 ressive expansion of the field\, we now know that most main sequence stars
  possess a planetary system. In contrast\, while we know that the formatio
 n environment of planets are the so-called proto-planetary discs\, we stil
 l lack conclusive evidence for the presence of planets in them. With instr
 uments such as ALMA and SPHERE we are entering an exciting era of high-res
 olution imaging which could finally bring this evidence. I will discuss th
 e prospects for observing how super-Earths shape the proto-planetary disc.
  While the effect on the gas disc\, that comprises most of the mass\, is v
 ery limited\, the impact is much stronger in the dust disc probed by obser
 vations\, and in particular for the mm-grains observed by ALMA\, due to th
 e perturbations induced in the pressure profile of the disc by the planet.
  I’ll highlight in particular how there exists a minimum planet mass tha
 t is able to produce a pressure maximum outside its orbit\, trapping dust 
 and eventually creating a hole in the mm dust. Smaller grains can still br
 eak through the trap because of dust diffusion. Planet masses lower than t
 he threshold can still affect the dust surface density\, by creating traff
 ic jams in the dust radial velocity. Finally\, I will discuss how it is po
 ssible to have an estimate of the mass of the planet from the observations
 \, highlighting in particular the dependence of the pressure maximum locat
 ion on the planet mass.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
END:VEVENT
END:VCALENDAR