Coronal Holes and the High-Speed Solar Wind

By S. Cranmer. 2002

194 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/d99f70a536130c3c8a534179c7cf712ccc92606c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

The Solar Orbiter magnetometer (2020, background): “While it is well established that high-speed solar wind originates in coronal holes (Cranmer 2002), the origin of slower wind is less clear, with multiple sources being possible.”
Geoeffective Properties of Solar Transients and Stream Interaction Regions (2017, background): “…slowly narrowing to the actual cause (Toman 1958; Saemundsson 1962), it was only the discovery of coronal holes with Skylab X-ray observations and associations of fast solar wind streams with them (Krieger et al. (1973) and Nolte et al. (1976), see also Cranmer (2002)) that resolved this puzzle.”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “There is gradual heat input into the solar wind plasma that begins in the corona and extends far out into interplanetary space (see reviews by Parker 1963; Leer et al. 1982; Tu & Marsch 1995; Goldstein et al. 1995; Marsch 1999; Hollweg & Isenberg 2002; Cranmer 2002; Matthaeus et al. 2003).”
Magnetohydrodynamic Oscillations in the Solar Corona and Earth’s Magnetosphere: Towards Consolidated Understanding (2016, background): “Another important difference is connected with the minor species, which should be taken into account in the consideration of low-frequency cyclotron resonances (e.g. Cranmer 2002).”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “Interested readers are urged to fill in the gaps by surveying other reviews, such as those by Dessler (1967), Holzer and Axford (1970), Hundhausen (1972), Leer et al. (1982), Barnes (1992), Parker (1997), Cranmer (2002, 2009), Marsch (2006), Velli (2010), Abbo et al. (2016), and Chen (2016).”
Ultraviolet spectroscopy of the extended solar corona (2006, methodology): “A model of Alfvén wave action conservation, with a lower boundary amplitude of 30 km s , was convolved with the empirically determined kinetic temperature in order to compute this curve (see also Esser et al. 1999; Cranmer 2002a, 2004b).”