### Abstract

We carried out global three-dimensional resistive magnetohydrodynamic simulations of galactic gaseous disks to investigate how the galactic magnetic fields are amplified and maintained. We adopt a steady axisymmetric gravitational potential given by Miyamoto & Nagai and Miyamoto et al. As the initial condition, we assume a warm (T ∼ 10^{5} K) rotating gas torus centered at ω̄ = 10 kpc threaded by weak azimuthal magnetic fields. Numerical results indicate that in differentially rotating galactic gaseous disks, magnetic fields are amplified due to magnetorotational instability and magnetic turbulence develops. After the amplification of magnetic energy saturates, the disk stays in a quasi-steady state. The mean azimuthal magnetic field increases with time and shows reversals with a period of 1 Gyr (2 Gyr for a full cycle). The amplitude of B_{φ} near the equatorial plane is B_{φ} ∼ 1.5 μG at ω̄ = 5 kpc. The magnetic fields show large fluctuations whose standard deviation is comparable to the mean field. The mean azimuthal magnetic field in the disk corona has a direction opposite to the mean magnetic field inside the disk. The mass accretion rate driven by the Maxwell stress is ∼10^{-3} M _{⊙} yr^{-1} at ω̄ = 2.5 kpc when the mass of the initial torus is ∼5 × 10^{8} M_{⊙}. When we adopt an absorbing boundary condition at r = 0.8 kpc, the rotation curve obtained by numerical simulations almost coincides with the rotation curve of the stars and the dark matter. Thus, even when magnetic fields are not negligible for gas dynamics of a spiral galaxy, the galactic gravitational potential can be derived from observations of the rotation curve using the gas component of the disk.

Original language | English |
---|---|

Pages (from-to) | 862-877 |

Number of pages | 16 |

Journal | Astrophysical Journal |

Volume | 641 |

Issue number | 2 I |

DOIs | |

Publication status | Published - Apr 20 2006 |

Externally published | Yes |

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### All Science Journal Classification (ASJC) codes

- Astronomy and Astrophysics
- Space and Planetary Science

### Cite this

*Astrophysical Journal*,

*641*(2 I), 862-877. https://doi.org/10.1086/500525

**Global three-dimensional magentohydrodynamic simulations of galactic gaseous disks. I. amplification of mean magnetic fields in an axisymmetric gravitational potential.** / Nishikori, Hiromitsu; Machida, Mami; Matsumoto, Ryoji.

Research output: Contribution to journal › Article

*Astrophysical Journal*, vol. 641, no. 2 I, pp. 862-877. https://doi.org/10.1086/500525

}

TY - JOUR

T1 - Global three-dimensional magentohydrodynamic simulations of galactic gaseous disks. I. amplification of mean magnetic fields in an axisymmetric gravitational potential

AU - Nishikori, Hiromitsu

AU - Machida, Mami

AU - Matsumoto, Ryoji

PY - 2006/4/20

Y1 - 2006/4/20

N2 - We carried out global three-dimensional resistive magnetohydrodynamic simulations of galactic gaseous disks to investigate how the galactic magnetic fields are amplified and maintained. We adopt a steady axisymmetric gravitational potential given by Miyamoto & Nagai and Miyamoto et al. As the initial condition, we assume a warm (T ∼ 105 K) rotating gas torus centered at ω̄ = 10 kpc threaded by weak azimuthal magnetic fields. Numerical results indicate that in differentially rotating galactic gaseous disks, magnetic fields are amplified due to magnetorotational instability and magnetic turbulence develops. After the amplification of magnetic energy saturates, the disk stays in a quasi-steady state. The mean azimuthal magnetic field increases with time and shows reversals with a period of 1 Gyr (2 Gyr for a full cycle). The amplitude of Bφ near the equatorial plane is Bφ ∼ 1.5 μG at ω̄ = 5 kpc. The magnetic fields show large fluctuations whose standard deviation is comparable to the mean field. The mean azimuthal magnetic field in the disk corona has a direction opposite to the mean magnetic field inside the disk. The mass accretion rate driven by the Maxwell stress is ∼10-3 M ⊙ yr-1 at ω̄ = 2.5 kpc when the mass of the initial torus is ∼5 × 108 M⊙. When we adopt an absorbing boundary condition at r = 0.8 kpc, the rotation curve obtained by numerical simulations almost coincides with the rotation curve of the stars and the dark matter. Thus, even when magnetic fields are not negligible for gas dynamics of a spiral galaxy, the galactic gravitational potential can be derived from observations of the rotation curve using the gas component of the disk.

AB - We carried out global three-dimensional resistive magnetohydrodynamic simulations of galactic gaseous disks to investigate how the galactic magnetic fields are amplified and maintained. We adopt a steady axisymmetric gravitational potential given by Miyamoto & Nagai and Miyamoto et al. As the initial condition, we assume a warm (T ∼ 105 K) rotating gas torus centered at ω̄ = 10 kpc threaded by weak azimuthal magnetic fields. Numerical results indicate that in differentially rotating galactic gaseous disks, magnetic fields are amplified due to magnetorotational instability and magnetic turbulence develops. After the amplification of magnetic energy saturates, the disk stays in a quasi-steady state. The mean azimuthal magnetic field increases with time and shows reversals with a period of 1 Gyr (2 Gyr for a full cycle). The amplitude of Bφ near the equatorial plane is Bφ ∼ 1.5 μG at ω̄ = 5 kpc. The magnetic fields show large fluctuations whose standard deviation is comparable to the mean field. The mean azimuthal magnetic field in the disk corona has a direction opposite to the mean magnetic field inside the disk. The mass accretion rate driven by the Maxwell stress is ∼10-3 M ⊙ yr-1 at ω̄ = 2.5 kpc when the mass of the initial torus is ∼5 × 108 M⊙. When we adopt an absorbing boundary condition at r = 0.8 kpc, the rotation curve obtained by numerical simulations almost coincides with the rotation curve of the stars and the dark matter. Thus, even when magnetic fields are not negligible for gas dynamics of a spiral galaxy, the galactic gravitational potential can be derived from observations of the rotation curve using the gas component of the disk.

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U2 - 10.1086/500525

DO - 10.1086/500525

M3 - Article

AN - SCOPUS:33745318682

VL - 641

SP - 862

EP - 877

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 I

ER -