English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We explore the effect magnetic fields have on self-gravitating accretiondisks around spinning black holes via numerical evolutions in full dynamicalmagnetohydrodynamic spacetimes. The configurations we study are unstable to thePapaloizou-Pringle Instability (PPI). PPI-saturated accretion tori have beenshown to produce gravitational waves, detectable to cosmological distances bythird-generation gravitational wave (GW) observatories. While the PPI operatesstrongly for purely hydrodynamic disks, the situation can be different fordisks hosting initially small magnetic fields. Evolutions of disks withoutself-gravity in fixed BH spacetimes have shown that small seed fields caninitiate the rapid growth of the magneto-rotational instability (MRI), whichthen strongly suppresses the PPI. Since realistic astrophysical disks areexpected to be magnetized, PPI-generated GW signals may be suppressed as well.However, it is unclear what happens when the disk self-gravity is restored.Here, we study the impact of magnetic fields on the PPI-saturated state of aself-gravitating accretion disk around a spinning BH ($\chi = 0.7$) alignedwith the disk angular momentum, as well as one around a non-spinning BH. Wefind the MRI is effective at reducing the amplitude of PPI modes and theirassociated GWs, but the systems still generate GWs. Estimating thedetectability of these systems accross a wide range of masses, we show thatmagnetic fields reduce the maximum detection distance by Cosmic Explorer from300Mpc (in the pure hydrodynamic case) to 45Mpc for a $10 M_{\odot}$ system, byLISA from 11500Mpc to 2700Mpc for a $2 \times 10^{5} M_{\odot}$ system, and byDECIGO from $z \approx 5$ down to $z \approx 2$ for a $1000 M_{\odot}$ system.

Effect of magnetic fields on the dynamics and gravitational wave emission of PPI-saturated self-gravitating accretion disks: simulations in full GR