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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Vydáno v:	The Astrophysical journal Ročník 884; číslo 2; s. 102 - 112
Hlavní autoři:	Chang, Qing, Xu, Xiaojun, Xu, Qi, Zhong, Jun, Xu, Jiaying, Wang, Jing, Zhang, Tielong
Médium:	Journal Article
Jazyk:	angličtina
Vydáno:	Philadelphia The American Astronomical Society 20.10.2019 IOP Publishing
Témata:	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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Popis
Shrnutí:	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.
Bibliografie:	AAS17033 The Sun and the Heliosphere ObjectType-Article-1 SourceType-Scholarly Journals-1 ObjectType-Feature-2 content type line 14
ISSN:	0004-637X 1538-4357
DOI:	10.3847/1538-4357/ab412a