The Accretion Disc Dynamo in the Solar Nebula

Abstract

The nearest accretion disc to us in space if not time was the protosolar nebula. Remnants of this nebula thus potentially offer unique insight into how discs work. In particular the existence of chondrules, which must have formed in the disc as small molten droplets, requires strong and intermittent heating of disc material. We argue that this places important constraints on the way gravitational energy is released in accretion discs, which are not met by current shearing--box simulations of MRI--driven dynamos. A deeper understanding of accretion energy release in discs may require a better model for these dynamos.

MNRAS, accepted

References in corpus (9)

• Accretion disc viscosity: how big is alpha?
• MHD simulations of the magnetorotational instability in a shearing box with zero net flux. II. The effect of transport coefficients
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• New composite models of partially ionized protoplanetary disks
• Reconnection in Marginally Collisionless Accretion Disk Coronae
• Buoyant Bubbles in Intracluster Gas: Effects of Magnetic Fields and Anisotropic Viscosity
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• A Reconnecting Flux Rope Dynamo

Cited by in corpus (5)

• Mineral Processing by Short Circuits in Protoplanetary Disks
• Short Circuits in Thermally Ionized Plasmas: A Mechanism for Intermittent Heating of Protoplanetary Disks
• Universality of the Small-Scale Dynamo Mechanism
• Temperature Fluctuations driven by Magnetorotational Instability in Protoplanetary Disks
• Forming chondrules in impact splashes - II Volatile retention