High-resolution Modeling of Coronae and Winds in Solar-type Stars with Varying Rotation Rates. II. Stellar Winds
7 affiliations
- 1Nanjing University
- 2Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University)
- 3Leibniz Institute for Astrophysics Potsdam
- 4University of Birmingham
- 5Aalto University
- 6Max-Planck-Institut für Sonnensystemforschung
- 7KTH Royal Institute of Technology & Stockholm University
Abstract
Observations suggest a connection between steady-wind mass loss and coronal X-ray activity in low-mass main-sequence stars. Interpreting this connection is challenging because the wind is controlled mainly by the large-scale open field, whereas X-ray emission traces heating in small-scale closed fields often unresolved in global wind models. Here we use Space Weather Modeling Framework–Alfvén-Wave Solar Model with global convective dynamo-generated magnetic maps and solar magnetograms. We model Alfvén-wave-heated winds for four solar-type stars plus the Sun, spanning rotation rates of 1.0–23.3 times the solar rate, and magnetic field strengths of 6.0–1200 G. Our models show that faster rotation yields a more tightly wound spiral, a larger Alfvén surface, higher terminal wind speeds, and a harsher wind-pressure environment for orbiting exoplanets, different from that of the present-day Sun. We estimate the mass- and angular-momentum-loss rates and find systematic differences from Zeeman–Doppler imaging based predictions. Building on the successful reproduction of X-ray coronae in our Paper I, we obtain the first self-consistent activity–wind relation in a unified modeling framework: the mass-loss rate scales with the surface X-ray flux following a power law with an index of ∼0.67. We also reexamine magnetic braking via open-flux magnetization, finding that the effective Alfvénic lever arm depends on the magnetization parameter with a power-law index of ∼0.35. Finally, we quantify the stellar wind pressure at the orbits of several super-Earths. Together with our Paper I, the series of results shows the distinct roles of multiscale magnetic fields and provides physically grounded inputs for assessing habitable-zone space weather.
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BibTeX
@article{陈2026highresolution,
title = {{High-resolution Modeling of Coronae and Winds in Solar-type Stars with Varying Rotation Rates. II. Stellar Winds}},
author = {Yue-Hong 悦虹 Chen 陈 and Julián D. Alvarado-Gómez and Xin Cheng and Victor See and Yu Dai and Maarit J. Korpi-Lagg and Jörn Warnecke and Chen Xing and Mingde Ding},
journal = {The Astrophysical Journal},
year = {2026},
month = oct,
doi = {10.3847/1538-4357/aeab7e},
url = {https://iopscience.iop.org/article/10.3847/1538-4357/aeab7e},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - High-resolution Modeling of Coronae and Winds in Solar-type Stars with Varying Rotation Rates. II. Stellar Winds
AU - Yue-Hong 悦虹 Chen 陈
AU - Julián D. Alvarado-Gómez
AU - Xin Cheng
AU - Victor See
AU - Yu Dai
AU - Maarit J. Korpi-Lagg
AU - Jörn Warnecke
AU - Chen Xing
AU - Mingde Ding
PY - 2026
DA - 2026/10/26
JO - The Astrophysical Journal
DO - 10.3847/1538-4357/aeab7e
UR - https://iopscience.iop.org/article/10.3847/1538-4357/aeab7e
AB - Observations suggest a connection between steady-wind mass loss and coronal X-ray activity in low-mass main-sequence stars. Interpreting this connection is challenging because the wind is controlled mainly by the large-scale open field, whereas X-ray emission traces heating in small-scale closed fields often unresolved in global wind models. Here we use Space Weather Modeling Framework–Alfvén-Wave Solar Model with global convective dynamo-generated magnetic maps and solar magnetograms. We model Alfvén-wave-heated winds for four solar-type stars plus the Sun, spanning rotation rates of 1.0–23.3 times the solar rate, and magnetic field strengths of 6.0–1200 G. Our models show that faster rotation yields a more tightly wound spiral, a larger Alfvén surface, higher terminal wind speeds, and a harsher wind-pressure environment for orbiting exoplanets, different from that of the present-day Sun. We estimate the mass- and angular-momentum-loss rates and find systematic differences from Zeeman–Doppler imaging based predictions. Building on the successful reproduction of X-ray coronae in our Paper I, we obtain the first self-consistent activity–wind relation in a unified modeling framework: the mass-loss rate scales with the surface X-ray flux following a power law with an index of ∼0.67. We also reexamine magnetic braking via open-flux magnetization, finding that the effective Alfvénic lever arm depends on the magnetization parameter with a power-law index of ∼0.35. Finally, we quantify the stellar wind pressure at the orbits of several super-Earths. Together with our Paper I, the series of results shows the distinct roles of multiscale magnetic fields and provides physically grounded inputs for assessing habitable-zone space weather.
SN - 0004-637X
SN - 1538-4357
ER -