Global 3-D solar-type star-disc dynamo systems: I. MHD modeling

B  von Rekowski; N  Piskunov

doi:10.1002/asna.200510526

Global 3-D solar-type star-disc dynamo systems: I. MHD modeling

B von Rekowski, N Piskunov

Applied Mathematics

Research output: Contribution to journal › Article › peer-review

Abstract

We have carried out global three-dimensional magnetohydrodynamic simulations of the star-disc interaction region around a young solar-type star. T'he magnetic field is generated and maintained by dynamos in the star as well as in the disc. The developing mass flows possess non-periodic time-variable azimuthal structure and are controlled by the nonaxisymmetric magnetic fields. Since the stellar field drives a strong stellar wind, accretion is anti-correlated with the stellar field strength and disc matter is spiraling onto the star at low latitudes, both contrary to the generally assumed accretion picture. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.

Original language	English
Pages (from-to)	340-354
Number of pages	15
Journal	Astronomische Nachrichten
Volume	327
DOIs	https://doi.org/10.1002/asna.200510526
Publication status	Published - 2006

Keywords

ISM : jets and outflows
accretion, accretion disks
magnetohydrodynamics (MHD)
stars : mass-loss
stars : pre-main sequence
T-TAURI STARS
YOUNG STELLAR OBJECTS
MAGNETOSPHERIC ACCRETION
3-DIMENSIONAL SIMULATIONS
MAGNETIC-FIELDS
INCLINED DIPOLE
ORION NEBULA
SPIN-DOWN
ROTATION
OUTFLOWS

Access to Document

10.1002/asna.200510526

Cite this

@article{9f78fa70a4564d568822a35ed8db6276,

title = "Global 3-D solar-type star-disc dynamo systems: I. MHD modeling",

abstract = "We have carried out global three-dimensional magnetohydrodynamic simulations of the star-disc interaction region around a young solar-type star. T'he magnetic field is generated and maintained by dynamos in the star as well as in the disc. The developing mass flows possess non-periodic time-variable azimuthal structure and are controlled by the nonaxisymmetric magnetic fields. Since the stellar field drives a strong stellar wind, accretion is anti-correlated with the stellar field strength and disc matter is spiraling onto the star at low latitudes, both contrary to the generally assumed accretion picture. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.",

keywords = "ISM : jets and outflows, accretion, accretion disks, magnetohydrodynamics (MHD), stars : mass-loss, stars : pre-main sequence, T-TAURI STARS, YOUNG STELLAR OBJECTS, MAGNETOSPHERIC ACCRETION, 3-DIMENSIONAL SIMULATIONS, MAGNETIC-FIELDS, INCLINED DIPOLE, ORION NEBULA, SPIN-DOWN, ROTATION, OUTFLOWS",

author = "{von Rekowski}, B and N Piskunov",

year = "2006",

doi = "10.1002/asna.200510526",

language = "English",

volume = "327",

pages = "340--354",

journal = "Astronomische Nachrichten",

issn = "1521-3994",

publisher = "Wiley-VCH, Weinheim",

}

TY - JOUR

T1 - Global 3-D solar-type star-disc dynamo systems: I. MHD modeling

AU - von Rekowski, B

AU - Piskunov, N

PY - 2006

Y1 - 2006

N2 - We have carried out global three-dimensional magnetohydrodynamic simulations of the star-disc interaction region around a young solar-type star. T'he magnetic field is generated and maintained by dynamos in the star as well as in the disc. The developing mass flows possess non-periodic time-variable azimuthal structure and are controlled by the nonaxisymmetric magnetic fields. Since the stellar field drives a strong stellar wind, accretion is anti-correlated with the stellar field strength and disc matter is spiraling onto the star at low latitudes, both contrary to the generally assumed accretion picture. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.

AB - We have carried out global three-dimensional magnetohydrodynamic simulations of the star-disc interaction region around a young solar-type star. T'he magnetic field is generated and maintained by dynamos in the star as well as in the disc. The developing mass flows possess non-periodic time-variable azimuthal structure and are controlled by the nonaxisymmetric magnetic fields. Since the stellar field drives a strong stellar wind, accretion is anti-correlated with the stellar field strength and disc matter is spiraling onto the star at low latitudes, both contrary to the generally assumed accretion picture. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.

KW - ISM : jets and outflows

KW - accretion, accretion disks

KW - magnetohydrodynamics (MHD)

KW - stars : mass-loss

KW - stars : pre-main sequence

KW - T-TAURI STARS

KW - YOUNG STELLAR OBJECTS

KW - MAGNETOSPHERIC ACCRETION

KW - 3-DIMENSIONAL SIMULATIONS

KW - MAGNETIC-FIELDS

KW - INCLINED DIPOLE

KW - ORION NEBULA

KW - SPIN-DOWN

KW - ROTATION

KW - OUTFLOWS

U2 - 10.1002/asna.200510526

DO - 10.1002/asna.200510526

M3 - Article

SN - 1521-3994

VL - 327

SP - 340

EP - 354

JO - Astronomische Nachrichten

JF - Astronomische Nachrichten

ER -

Global 3-D solar-type star-disc dynamo systems: I. MHD modeling

Abstract

Keywords

Access to Document

Fingerprint

Cite this