H2020Индивидуална стипендия2017–2019

ICED · Initial conditions of exoplanet formation in protoplanetary disks

„Хоризонт 2020“ — Действия „Мария Склодовска-Кюри“

Период: 2017-10-01 → 2019-09-30
Финансиране от ЕС: 177 599 €
Участници: 1
Схема: MSCA-IF-EF-ST

Линиите свързват координатора с партньорите.

Накратко на български

Разпределението на елементи в газовите дискове около младите звезди показва как се формират екзопланети, например газовите гиганти. Това помага да разберем как жизненоважни вещества като въглерод и азот са попаднали в Земята и кои планети могат да поддържат живот.

Този кратък обзор е генериран от изкуствен интелект

Кратко обяснение, генерирано от езиков модел по текста на CORDIS. Оригиналът е по-долу.

Резултати накратко

Initial conditions of exoplanet formation in protoplanetary disks

Astronomers are now beginning the process of measuring the compositions of extrasolar planets. The precise combination of elements in the atmospheres of these planets should reflect their formation location and time. To this end, the distribution of elements as a function of radius in protoplanetary disks (where planets form) can provide a map with which to compare extrasolar planet compositions. Ultimately this knowledge will help us to understand how certain elements that are critical to life, e.g. carbon, hydrogen, oxygen, and nitrogen, came to be incorporated into Earth and which types of extrasolar planets should have the necessary bulk elemental ingredients to support life. This issue is important for our society to understand our place in the universe and to motivate future exploration and potentially resource management of the bodies in our own solar system. The first overall objective of the program was to measure the gas phase composition in a range of protoplanetary disks at the radial distance from the central star analogous to the location of most observed extrasolar hot gas giant planet, to determine what these planets' atmospheric composition would be if they formed in situ. A second goal was to use the deficit of certain elements in the gas in this region of protoplanetary disks to infer the solid rocky and icy composition of forming planetesimals in these disks. We met these objectives successfully. We have concluded that the gas in the inner regions of some protoplanetary disks is depleted in ice-forming elements, suggesting that hot gas giants that form in situ should have relatively little of these elements in their atmospheres (McClure 2019; McClure & Dominik, submitted & under revision). We also found that rock-bearing elements like iron, silicon, and calcium were depleted in one disk by ~100 times more than the ice-forming elements, suggesting that asteroid-like planetesimal formation was underway in these disks. We also determined that the first steps of forming the planetesimal cores must happen already by ~100,000 years after the protostar forms (McClure, Dominik, & Kama, drafting).

Текст от CORDIS, на английски · Данни: CORDIS, © Европейски съюз

Цел на проекта

There is now a substantial population of exoplanets with well-determined masses, radii, and orbital parameters in a range of host stellar systems. JWST will bring an increase in exoplanets with atmospheric spectroscopy measurements, moving the field from pure discovery to population synthesis and characterization. Many of the best-studied planetary systems are massive and located within 1AU of their central stars; it is not clear whether all of these planets migrated from farther out in their natal disks to this location or if they could have formed in situ. Both scenarios should produce distinct compositions resulting from multiple strong, time-dependent chemical gradients in their disks due to thermal sublimation and grain processing effects. These effects likely set the bulk chemical composition of the planet’s core and atmosphere, which are accreted from different material in the disk. By determining the physical conditions within 1AU, I will confirm whether they are sufficient to support in situ planet formation. I will also map the distribution of key planetary building blocks in both the solid phase (dust grains) and gas phase. This will be accomplished by interpreting disks’ flux as a function of wavelength with radiative transfer models including detailed sublimation and condensation physics, and comparing observed spectral features in both the solid and gaseous phases in molecular and atomic form to those predicted by models. This project will provide training through research in numerical methods and exoplanet characterization techniques, which are important in the long term for my career goals to lead a research group in planetary formation. Through development courses, I will improve my marketability for senior research positions and in turn transfer my infrared observing skills and US and European network connections to the host. This project increases the visibility of the host and European exoplanetary astronomy on an international scale.

Оригинален текст от CORDIS (на английски).

Участници

UNIVERSITEIT VAN AMSTERDAM · AmsterdamКоординаторНидерландия