Simulating galaxy formation with black hole driven thermal and kinetic feedback

• Verfasst von: Weinberger, Rainer [VerfasserIn]
• Verfasst von: Springel, Volker [VerfasserIn]
• Verfasst von: Hernquist, Lars [VerfasserIn]
• Verfasst von: Pillepich, Annalisa [VerfasserIn]
• Verfasst von: Marinacci, Federico [VerfasserIn]
• Verfasst von: Pakmor, Rüdiger [VerfasserIn]
• Verfasst von: Nelson, Dylan [VerfasserIn]
• Verfasst von: Genel, Shy [VerfasserIn]
• Verfasst von: Vogelsberger, Mark [VerfasserIn]
• Verfasst von: Naiman, Jill P. [VerfasserIn]
• Verfasst von: Torrey, Paul [VerfasserIn]
• Titel: Simulating galaxy formation with black hole driven thermal and kinetic feedback
• Verf.angabe: Rainer Weinberger, Volker Springel, Lars Hernquist, Annalisa Pillepich, Federico Marinacci, Rüdiger Pakmor, Dylan Nelson, Shy Genel, Mark Vogelsberger, Jill Naiman, Paul Torrey
• E-Jahr: 2017
• Jahr: February 2017
• Umfang: 20 S.
• Fussnoten: Gesehen am 24.10.2017
• Titel Quelle: Enthalten in: De.arxiv.org
• Ort Quelle: [S.l.] : Arxiv.org, 1991
• Jahr Quelle: 2017
• Band/Heft Quelle: (2017) Artikel-Nummer 1607.03486, 20 Seiten
• Datenträger: Online-Ressource
• Sprache: eng
• Sach-SW: Astrophysics - Astrophysics of Galaxies
• K10plus-PPN: 1564708500

Abstract

The inefficiency of star formation in massive elliptical galaxies is widely believed to be caused by the interactions of an active galactic nucleus (AGN) with the surrounding gas. Achieving a sufficiently rapid reddening of moderately massive galaxies without expelling too many baryons has however proven difficult for hydrodynamical simulations of galaxy formation, prompting us to explore a new model for the accretion and feedback effects of supermassive black holes. For high accretion rates relative to the Eddington limit, we assume that a fraction of the accreted rest mass energy heats the surrounding gas thermally, similar to the `quasar mode' in previous work. For low accretion rates, we invoke a new, pure kinetic feedback model which imparts momentum into the surrounding gas in a stochastic manner. These two modes of feedback are motivated both by theoretical conjectures for the existence of different types of accretion flows as well as recent observational evidence for the importance of kinetic AGN winds in quenching galaxies. We find that a large fraction of the injected kinetic energy in this mode thermalises via shocks in the surrounding gas, thereby providing a distributed heating channel. In cosmological simulations, the resulting model produces red, non star-forming massive elliptical galaxies, and achieves realistic gas fractions, black hole growth histories and thermodynamic profiles in large haloes.