H2020Индивидуална стипендия2015–2017

FIRSTBHs · The formation of supermassive black holes in the early universe

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

Период: 2015-10-01 → 2017-09-30
Финансиране от ЕС: 173 076 €
Участници: 1
Схема: MSCA-IF

Линиите свързват координатора с партньорите.

Накратко на български

Свръхмасивните черни дупки в ранната Вселена се изследват чрез симулации на газови облаци, които се сриват директно в огромни звезди и след това в черни дупки. Това помага да се разбере как тези обекти са достигнали такава маса за толкова кратко време.

Този кратък обзор е генериран от изкуствен интелект

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

Резултати накратко

The formation of supermassive black holes in the early universe

Supermassive black holes of more than a billion solar masses have been observed when the Universe was less than a billion years old. As a reference, the entire mass in stars in the Milky Way is only about ten times larger, the black hole at the center of our galaxy is about 4 million solar masses, and the Universe is now almost 14 billion years old. Explaining the existence of the supermassive black holes at these early cosmic times is highly challenging, as they need to grow continuously during the chaotic early phases of the cosmos. Seed black holes with masses of 10,000-1,000,000 solar masses, as predicted by the “direct collapse” scenario, provide a promising pathway to explain their presence. In this project we simulated the formation and growth of these seeds, following the dynamics of the gas from cosmological scales down to scales comparable to the solar system. The gravitational collapse initially forms a rapidly accreting protostar, which subsequently moves to the main sequence and finally collapses to a massive black hole. In the first part of the project, we computed the properties of the forming supermassive stars and black holes. Subsequently, the simulations have been extended by incorporating ultraviolet and X-ray radiation from the black hole itself to assess its growth. This is a substantial step forward to understand the origin of high-redshift black holes.

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

Цел на проекта

Supermassive black holes (BHs) of more than a billion solar masses have been observed at z > 6 when the Universe was less than a billion years old. Forming such objects is highly challenging, as high accretion rates need to be maintained over very long time scales. Seed BHs with masses of 10^4 -10^6 solar masses, as predicted by the “direct collapse” scenario, provide a promising pathway to explain their presence. During this project, I will derive the mass distribution of the BHs to provide constraints on their masses and growth mechanisms which can tested with upcoming missions such as JWST and ATHENA. To achieve this goal, I will build up a statistical sample of high-resolution adaptive mesh refinement (AMR) simulations of massive primordial halos, following the dynamics of the gas from cosmological scales down to scales comparable to the solar system. The gravitational collapse initially forms a rapidly accreting protostar, which subsequently moves to the main sequence providing ultra-violet (UV) feedback and finally collapses to a massive BH. In the first part of the project, I will compute the impact of stellar feedback from the supermassive star and follow the time evolution of the mass accretion rates. Subsequently, the simulations will be extended by incorporating the X-ray feedback from the BH itself. Finally, scaling relations between the properties of the host halos and BH masses will be derived. This work will provide the first detailed assessment of the mass distribution of seed BHs, and their observational properties. Thisis a substantial step forward to understand the origin of high-redshift BHs.

Оригинален текст от CORDIS (на английски).

Участници

CENTRE NATIONAL DE LA RECHERCHE SCIENTIFIQUE CNRS · ParisКоординаторФранция