Giant planets are most frequently found around stars around 2Msun. In the narrow range from 1.5-3.5 Msun, these, typically A-type stars, are markedly distinct from all other types of stars in terms of the pre-main sequence evolution of their interior, their emission and consequently of the evolution of their protoplanetary discs. This is possibly one of the most prominent links between disc evolution, planet formation and exoplanet studies. Investigating this link is especially facilitated by the fact that the bright pre-main sequence (<10Myr old) A-type stars and their discs by far outrank all others as ideal observing targets as planet-formation laboratories. In this talk I will examine the existing observational and theoretical evidence arguing that the high giant planet incidence lies in the propensity of these discs to form giant planets. In particular, I will focus on the results from our recent ALMA survey which reveals that large gas masses and therefore giant planet formation around A-type stars can persist up to the main sequence, much longer than we would expect based on the studies of lower mass stars.
Unless announced otherwise, the lunch talks start at 12:30 sharp. The approximate duration of the lunch talk is given above, and additional time will be given for questions and discussion following the presentation. Please make sure that you take ample time to pick up your lunch beforehand.
Information for Speakers and Hosts: Talks by internal speakers are limited to 20 minutes, with additional time for questions. Visiting speakers can have up to 30 minutes, with additional time for questions. Hosts are responsible for bringing the speaker to the correct room in ample time to set up laptops etc., and for ensuring the speaker also has time for lunch.
For questions and/or suggestions concerning the lunch talks, please contact Themiya Nanayakkara () or Alvaro Hacar ()).