More detailed information about both hands-on sessions, including software that needs to be installed and installation instructions, will be available in the coming months, so stay tuned!
Attendees will explore a variety of circumstellar disks and their properties by analyzing models calculated with RADMC-3D, which is a code for radiative transfer calculations, including tools to produce produce images and plot spectral energy distributions.
As giant planets age and cool, much of the details of their formation history are slowly obscured. By a hundred million years or so, giant planets formed by core accretion are expected to look much like planets formed by gravitational instability. For this reason it is important to study young giant planets, ideally as young as ten or twenty million years or younger, as the combination of a planet's mass, radius, effective temperature, and atmospheric composition will paint a clear picture of its formation story. However discerning these key planet properties from spectra and photometry of directly imaged young planets, such as those in the HR 8977 system or 51 Eri b, has proven challenging. Our hands on activity will address why this is the case and allow attendees to devise their own observational tests of young planet properties that might be applied to future datasets from JWST, the ELTs, and other telescopes.
Attendees will use our planetary spectral modeling tool PICASO in combination with our cloud modeling framework VIRGA to create model spectra of young extrasolar giant planets. They will learn how traits like atmospheric composition, gravity, clouds, and temperature can produce degenerate spectral signatures at some wavelengths and will devise notional observing programs to better tease out these properties in order to best characterize young giant planets. By learning how to use this suite of open source modeling tools, attendees will be well-equipped to plan and conduct their own research on young giant planets in the future.
(last updated June 7th, 2021 12:58:29)