Sol88
Philosopher
- Joined
- Mar 23, 2009
- Messages
- 8,437
Observations have shown that these loops have axially uniform cross‐sections (Bellan 2003). Their very small inverse aspect ratios are often used to justify the neglect of curvature and to model them as straight cylinders, which is known as the thin flux tube approximation (see Zhugzhda 1996; Van der Linden & Hood 1999; Lothian & Browning 2000, and references therein). Coronal loops are line‐tied to the photosphere (Berger 1991). As such, boundary conditions at the ends of the cylindrical axis are important, as the coronal physics are influenced by conditions at the photosphere and chromosphere (Aschwanden, Nightingale & Alexander 2000). As the solar wind moves away from the Sun, it carries the coronal flux tubes along with it.
More specifically, coronal mass ejections (Low 2001) form solar flux ropes (also known as interplanetary magnetic clouds) as they move in the solar wind away from the Sun.
Usually the plasma β≪ 1 for these flux ropes (Burlaga 1988), and Shimazu & Vandas (2002) have shown that as the flux ropes expand due to the ambient pressure decrease with distance from the Sun, they maintain a force‐free state. As such, the flux ropes are modelled locally as infinitely long cylinders described by linear force‐free magnetic fields (Burlaga 1988; Lepping et al. 2001; Berdichevsky, Lepping & Farrugia 2003).
Cylindrical linear force‐free magnetic fields with toroidal flux surfaces G. J. J. Botha, E. A. Evangelidis
Jd116, you may benefit from jotting this down somewhere….
More specifically, coronal mass ejections (Low 2001) form solar flux ropes (also known as interplanetary magnetic clouds) as they move in the solar wind away from the Sun.
They, being the multitude of electric currents and current driven instabilities.
Plasma is not a gas and the solar wind is not quasi neutral.