Multiple-point Modeling the Parker Spiral Configuration of the Solar Wind Magnetic Field at the Solar Maximum of Solar Cycle 24

By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r = R0 (neglecting solar gravitation and acceleration by high coronal temperature), the large-scale solar wind magnetic field lines are distorted into a Parker spiral...

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Published in:The Astrophysical journal Vol. 884; no. 2; pp. 102 - 112
Main Authors: Chang, Qing, Xu, Xiaojun, Xu, Qi, Zhong, Jun, Xu, Jiaying, Wang, Jing, Zhang, Tielong
Format: Journal Article
Language:English
Published: Philadelphia The American Astronomical Society 20.10.2019
IOP Publishing
Subjects:
Acceleration
Astrophysics
Empirical equations
Magnetic field configurations
Magnetic fields
Magnetism
Mercury
Mercury (planet)
Planetary magnetic fields
planets and satellites: magnetic fields
Solar corona
Solar cycle
Solar cycle-solar wind relationships
Solar gravitation
Solar magnetic field
Solar maximum
Solar probes
Solar wind
Solar wind flow
Solar wind magnetic fields
Solar wind velocity
Spirals
Sun: activity
Sun: magnetic fields
Venus
Wind flow
Wind speed
Wind velocities
ISSN:0004-637X, 1538-4357
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Abstract By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r = R0 (neglecting solar gravitation and acceleration by high coronal temperature), the large-scale solar wind magnetic field lines are distorted into a Parker spiral configuration, which is usually simplified to an Archimedes spiral. Using magnetic field observations near Mercury, Venus, and Earth during solar maximum of Solar Cycle 24, we statistically surveyed the Parker spiral angles and obtained the empirical equations of the Archimedes and Parker spirals by fitting the multiple-point results. We found that the solar wind magnetic field configurations are slightly different during different years. Archimedes and Parker spiral configurations are quite different from each other within 1 au. Our results provide empirical Archimedes and Parker spiral equations that depend on the solar wind velocity and the critical distance (R0). It is inferred that R0 is much larger than that previously assumed. In the near future, the statistical survey of the near-Sun solar wind velocity by Parker Solar Probe can help verify this result.
AbstractList By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r = R0 (neglecting solar gravitation and acceleration by high coronal temperature), the large-scale solar wind magnetic field lines are distorted into a Parker spiral configuration, which is usually simplified to an Archimedes spiral. Using magnetic field observations near Mercury, Venus, and Earth during solar maximum of Solar Cycle 24, we statistically surveyed the Parker spiral angles and obtained the empirical equations of the Archimedes and Parker spirals by fitting the multiple-point results. We found that the solar wind magnetic field configurations are slightly different during different years. Archimedes and Parker spiral configurations are quite different from each other within 1 au. Our results provide empirical Archimedes and Parker spiral equations that depend on the solar wind velocity and the critical distance (R0). It is inferred that R0 is much larger than that previously assumed. In the near future, the statistical survey of the near-Sun solar wind velocity by Parker Solar Probe can help verify this result.
By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r  =  R 0 (neglecting solar gravitation and acceleration by high coronal temperature), the large-scale solar wind magnetic field lines are distorted into a Parker spiral configuration, which is usually simplified to an Archimedes spiral. Using magnetic field observations near Mercury, Venus, and Earth during solar maximum of Solar Cycle 24, we statistically surveyed the Parker spiral angles and obtained the empirical equations of the Archimedes and Parker spirals by fitting the multiple-point results. We found that the solar wind magnetic field configurations are slightly different during different years. Archimedes and Parker spiral configurations are quite different from each other within 1 au. Our results provide empirical Archimedes and Parker spiral equations that depend on the solar wind velocity and the critical distance ( R 0 ). It is inferred that R 0 is much larger than that previously assumed. In the near future, the statistical survey of the near-Sun solar wind velocity by Parker Solar Probe can help verify this result.
By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r = R 0 (neglecting solar gravitation and acceleration by high coronal temperature), the large-scale solar wind magnetic field lines are distorted into a Parker spiral configuration, which is usually simplified to an Archimedes spiral. Using magnetic field observations near Mercury, Venus, and Earth during solar maximum of Solar Cycle 24, we statistically surveyed the Parker spiral angles and obtained the empirical equations of the Archimedes and Parker spirals by fitting the multiple-point results. We found that the solar wind magnetic field configurations are slightly different during different years. Archimedes and Parker spiral configurations are quite different from each other within 1 au. Our results provide empirical Archimedes and Parker spiral equations that depend on the solar wind velocity and the critical distance (R 0). It is inferred that R 0 is much larger than that previously assumed. In the near future, the statistical survey of the near-Sun solar wind velocity by Parker Solar Probe can help verify this result.
Author Xu, Xiaojun
Xu, Qi
Zhong, Jun
Chang, Qing
Xu, Jiaying
Zhang, Tielong
Wang, Jing
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  organization: Space Research Institute , Austrian Academy of Sciences, Graz, Austria
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Snippet By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r = R0 (neglecting solar...
By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r  =  R 0 (neglecting...
By assuming that the solar wind flow is spherically symmetric and that the flow speed becomes constant beyond some critical distance r = R 0 (neglecting solar...
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SubjectTerms Acceleration
Astrophysics
Empirical equations
Magnetic field configurations
Magnetic fields
Magnetism
Mercury
Mercury (planet)
Planetary magnetic fields
planets and satellites: magnetic fields
Solar corona
Solar cycle
Solar cycle-solar wind relationships
Solar gravitation
Solar magnetic field
Solar maximum
Solar probes
Solar wind
Solar wind flow
Solar wind magnetic fields
Solar wind velocity
Spirals
Sun: activity
Sun: magnetic fields
Venus
Wind flow
Wind speed
Wind velocities
Title Multiple-point Modeling the Parker Spiral Configuration of the Solar Wind Magnetic Field at the Solar Maximum of Solar Cycle 24
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