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Magnetic fields of low-mass main sequences stars: non-linear dynamo theory and mean-field numerical simulations. / Kleeorin, N.; Rogachevskii, I.; Safiullin, N. и др.
в: Monthly Notices of the Royal Astronomical Society, Том 526, № 2, 2023, стр. 1601-1612.

Результаты исследований: Вклад в журнал › Статья › Рецензирование

Harvard

Kleeorin, N, Rogachevskii, I, Safiullin, N, Gershberg, R & Porshnev, S 2023, 'Magnetic fields of low-mass main sequences stars: non-linear dynamo theory and mean-field numerical simulations', Monthly Notices of the Royal Astronomical Society, Том. 526, № 2, стр. 1601-1612. https://doi.org/10.1093/mnras/stad2708

APA

Kleeorin, N., Rogachevskii, I., Safiullin, N., Gershberg, R., & Porshnev, S. (2023). Magnetic fields of low-mass main sequences stars: non-linear dynamo theory and mean-field numerical simulations. Monthly Notices of the Royal Astronomical Society, 526(2), 1601-1612. https://doi.org/10.1093/mnras/stad2708

Vancouver

Kleeorin N, Rogachevskii I, Safiullin N, Gershberg R, Porshnev S. Magnetic fields of low-mass main sequences stars: non-linear dynamo theory and mean-field numerical simulations. Monthly Notices of the Royal Astronomical Society. 2023;526(2):1601-1612. doi: 10.1093/mnras/stad2708

Author

Kleeorin, N. ; Rogachevskii, I. ; Safiullin, N. и др. / Magnetic fields of low-mass main sequences stars: non-linear dynamo theory and mean-field numerical simulations. в: Monthly Notices of the Royal Astronomical Society. 2023 ; Том 526, № 2. стр. 1601-1612.

BibTeX

@article{9797e17ef3b34e61b0f9d5392c1bf5f2,
title = "Magnetic fields of low-mass main sequences stars: non-linear dynamo theory and mean-field numerical simulations",
abstract = "Our theoretical and numerical analysis have suggested that for low-mass main sequences stars (of the spectral classes from M5 to G0) rotating much faster than the Sun, the generated large-scale magnetic field is caused by the mean-field α2 dynamo, whereby the α2 dynamo is modified by a weak differential rotation. Even for a weak differential rotation, the behaviour of the magnetic activity is changed drastically from aperiodic regime to non-linear oscillations and appearance of a chaotic behaviour with increase of the differential rotation. Periods of the magnetic cycles decrease with increase of the differential rotation, and they vary from tens to thousand years. This long-term behaviour of the magnetic cycles may be related to the characteristic time of the evolution of the magnetic helicity density of the small-scale field. The performed analysis is based on the mean-field simulations (MFS) of the α2 and α2 dynamos and a developed non-linear theory of α2 dynamo. The applied MFS model was calibrated using turbulent parameters typical for the solar convective zone. {\textcopyright} 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.",
author = "N. Kleeorin and I. Rogachevskii and N. Safiullin and R. Gershberg and S. Porshnev",
note = "The work of NK and NS was supported by the Russian Science Foundation (grant 21-72-20067). IR acknowledges the hospitality of NORDITA.",
year = "2023",
doi = "10.1093/mnras/stad2708",
language = "English",
volume = "526",
pages = "1601--1612",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",

}

RIS

TY - JOUR

T1 - Magnetic fields of low-mass main sequences stars: non-linear dynamo theory and mean-field numerical simulations

AU - Kleeorin, N.

AU - Rogachevskii, I.

AU - Safiullin, N.

AU - Gershberg, R.

AU - Porshnev, S.

N1 - The work of NK and NS was supported by the Russian Science Foundation (grant 21-72-20067). IR acknowledges the hospitality of NORDITA.

PY - 2023

Y1 - 2023

N2 - Our theoretical and numerical analysis have suggested that for low-mass main sequences stars (of the spectral classes from M5 to G0) rotating much faster than the Sun, the generated large-scale magnetic field is caused by the mean-field α2 dynamo, whereby the α2 dynamo is modified by a weak differential rotation. Even for a weak differential rotation, the behaviour of the magnetic activity is changed drastically from aperiodic regime to non-linear oscillations and appearance of a chaotic behaviour with increase of the differential rotation. Periods of the magnetic cycles decrease with increase of the differential rotation, and they vary from tens to thousand years. This long-term behaviour of the magnetic cycles may be related to the characteristic time of the evolution of the magnetic helicity density of the small-scale field. The performed analysis is based on the mean-field simulations (MFS) of the α2 and α2 dynamos and a developed non-linear theory of α2 dynamo. The applied MFS model was calibrated using turbulent parameters typical for the solar convective zone. © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

AB - Our theoretical and numerical analysis have suggested that for low-mass main sequences stars (of the spectral classes from M5 to G0) rotating much faster than the Sun, the generated large-scale magnetic field is caused by the mean-field α2 dynamo, whereby the α2 dynamo is modified by a weak differential rotation. Even for a weak differential rotation, the behaviour of the magnetic activity is changed drastically from aperiodic regime to non-linear oscillations and appearance of a chaotic behaviour with increase of the differential rotation. Periods of the magnetic cycles decrease with increase of the differential rotation, and they vary from tens to thousand years. This long-term behaviour of the magnetic cycles may be related to the characteristic time of the evolution of the magnetic helicity density of the small-scale field. The performed analysis is based on the mean-field simulations (MFS) of the α2 and α2 dynamos and a developed non-linear theory of α2 dynamo. The applied MFS model was calibrated using turbulent parameters typical for the solar convective zone. © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

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U2 - 10.1093/mnras/stad2708

DO - 10.1093/mnras/stad2708

M3 - Article

VL - 526

SP - 1601

EP - 1612

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -

ID: 46917859