HEИндивидуална стипендия2022–2024

YPB · Young planetesimal belts

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

Период: 2022-12-01 → 2024-11-30
Финансиране от ЕС: 140 188 €
Участници: 2
Схема: HORIZON-TMA-MSCA-PF-EF

Линиите свързват координатора с партньорите.

Накратко на български

Взаимодействието между газа и праха в поясите от малки небесни тела около далечни звезди се анализира чрез компютърни модели. Те помагат за правилното тълкуване на наблюденията върху извънслънчевите планетарни системи.

Този кратък обзор е генериран от изкуствен интелект

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

Резултати накратко

Young planetesimal belts

Our Solar system is composed of eight planets and also a large number of smaller bodies, grouped mainly in two belts: the main asteroid belt and the Kuiper belt. Other stars are frequently also surrounded by such belts. These distant belts are mainly studied through observations of the dust produced in collisions of the planetesimals. Unlike in the Solar system, the extrasolar planetesimal belts sometimes also contain a high amount of gas. The gas can affect the small dust particles and our inferences about the planetesimals. This project objectives focused on understanding the gas-dust interaction by developing detailed computational models of these systems. Such models are needed to interpret existing and future observations of extrasolar planetary systems.

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

Цел на проекта

Recent discoveries of numerous and diverse exoplanetary systems and their debris discs have revolutionized our understanding of how planets and planetesimals form. One of the exciting recent developments is detection of a large number of young systems which appear to be hosting belts of planetesimals, yet also unexpectedly show high amounts of gas. To explain these observations novel computational models must be developed, which take into account all key physical processes shaping the distribution of dust in these systems. I propose to use a kinetic model of collisional evolution of planetesimals and dust, combined with models of dust evolution due to gas drag and radiation pressure, and models of gas structure shaped by viscous evolution and dispersal. To do this I will extend the capabilities of a kinetic model previously used in studies of gas-free debris discs to account for dynamics of small dust grains in the presence of a gaseous disc. This will allow to model the entire range of body sizes, from dust to planetesimals, in a self-consistent way. The project will require knowledge of collisional planetesimal belts as well as of the proto-planetary environment, and this knowledge will be directly drawn from the existing research experience of the candidate. The project will generate a transfer of knowledge to the host institution while developing the candidate’s theoretical and technical expertise. The results of the project will be of wide use to the planetary science community, as they will help to interpret future observations of young planetary systems, to constrain the process of protoplanetary disc dispersal, and determine properties of dust and gas that may be accreted onto planets in the last stages of their formation.

Оригинален текст от CORDIS (на английски).

Участници

INSTITUT ZA FIZIKU · BEOGRADКоординаторСърбия
THE CHANCELLOR MASTERS AND SCHOLARS OF THE UNIVERSITY OF CAMBRIDGE · CAMBRIDGEОбединеното кралство