An Analytic Model For Magnetically-Dominated Accretion Disks
Fuente:
arXiv
Salvato in:
| Autori principali: | , , , , , , , , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2023
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866911326764269568 |
|---|---|
| author | Hopkins, Philip F. Squire, Jonathan Quataert, Eliot Murray, Norman Su, Kung-Yi Steinwandel, Ulrich P. Kremer, Kyle Faucher-Giguere, Claude-Andre Wellons, Sarah |
| author_facet | Hopkins, Philip F. Squire, Jonathan Quataert, Eliot Murray, Norman Su, Kung-Yi Steinwandel, Ulrich P. Kremer, Kyle Faucher-Giguere, Claude-Andre Wellons, Sarah |
| contents | Recent numerical cosmological radiation-magnetohydrodynamic-thermochemical-star formation simulations have resolved the formation of quasar accretion disks with Eddington or super-Eddington accretion rates onto supermassive black holes (SMBHs) down to a few hundred gravitational radii. These 'flux-frozen' and hyper-magnetized disks appear to be qualitatively distinct from classical $α$ disks and magnetically-arrested disks: the midplane pressure is dominated by toroidal magnetic fields with plasma $β\ll 1$ powered by advection of magnetic flux from the interstellar medium (ISM), and they are super-sonically and trans-Alfvenically turbulent with cooling times short compared to dynamical times yet remain gravitationally stable owing to magnetic support. In this paper, we present a simple analytic similarity model for such disks. For reasonable assumptions, the model is entirely specified by the boundary conditions (inflow rate at the BH radius of influence [BHROI]). We show that the scalings from this model are robust to various detailed assumptions, agree remarkably well with the simulations (given their simplicity), and demonstrate the self-consistency and gravitational stability of such disks even in the outer accretion disk (approaching the BHROI) at hyper-Eddington accretion rates. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2310_04507 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | An Analytic Model For Magnetically-Dominated Accretion Disks Hopkins, Philip F. Squire, Jonathan Quataert, Eliot Murray, Norman Su, Kung-Yi Steinwandel, Ulrich P. Kremer, Kyle Faucher-Giguere, Claude-Andre Wellons, Sarah High Energy Astrophysical Phenomena Cosmology and Nongalactic Astrophysics Astrophysics of Galaxies Plasma Physics Space Physics Recent numerical cosmological radiation-magnetohydrodynamic-thermochemical-star formation simulations have resolved the formation of quasar accretion disks with Eddington or super-Eddington accretion rates onto supermassive black holes (SMBHs) down to a few hundred gravitational radii. These 'flux-frozen' and hyper-magnetized disks appear to be qualitatively distinct from classical $α$ disks and magnetically-arrested disks: the midplane pressure is dominated by toroidal magnetic fields with plasma $β\ll 1$ powered by advection of magnetic flux from the interstellar medium (ISM), and they are super-sonically and trans-Alfvenically turbulent with cooling times short compared to dynamical times yet remain gravitationally stable owing to magnetic support. In this paper, we present a simple analytic similarity model for such disks. For reasonable assumptions, the model is entirely specified by the boundary conditions (inflow rate at the BH radius of influence [BHROI]). We show that the scalings from this model are robust to various detailed assumptions, agree remarkably well with the simulations (given their simplicity), and demonstrate the self-consistency and gravitational stability of such disks even in the outer accretion disk (approaching the BHROI) at hyper-Eddington accretion rates. |
| title | An Analytic Model For Magnetically-Dominated Accretion Disks |
| topic | High Energy Astrophysical Phenomena Cosmology and Nongalactic Astrophysics Astrophysics of Galaxies Plasma Physics Space Physics |
| url | https://arxiv.org/abs/2310.04507 |