A rebound shock mechanism for solar fibrils

Journal Article · Tue Aug 01 04:00:00 EDT 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/167767· OSTI ID:5463771

Sterling, A C; Hollweg, J V ^[1]

---

1. New Hampshire Univ., Durham (USA)

Flows along a rigid solar magnetic flux tube which is horizontal over a substantial portion of its length are numerically investigated. A single, quasi-impulsive force near the base of the first vertical segment drives a series of upward propagating rebound shocks on the flux tube. When the horizontal segment is in the corona, the shocks raise the transition region onto the horizontal segment and eventually onto the coronal vertical segment. The material behind the displaced transition region resembles a fibril on the horizontal segment, and a short spicule on the second vertical segment. A full-sized spicule does not develop. The resulting density of the material on the horizontal segment is 10 to the -14th g/cu cm, which is consistent with the observed densities in fibrils. When the horizontal segment is in the chromosphere, the motions and densities induced on the horizontal segment do not resemble those of observed fibrils, and a full-sized spicule again does not develop. 23 refs.

• OSTI ID: 5463771
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 343; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
CHROMOSPHERE
DENSITY
FLUID MECHANICS
HEATING
HYDRODYNAMICS
MAGNETIC FIELD CONFIGURATIONS
MAGNETIC FIELDS
MAGNETIC FLUX
MAGNETOHYDRODYNAMICS
MATHEMATICS
MECHANICS
NUMERICAL ANALYSIS
PHYSICAL PROPERTIES
SHOCK WAVES
SOLAR ACTIVITY
SOLAR ATMOSPHERE
SOLAR CORONA
SOLAR PROMINENCES
STELLAR ATMOSPHERES
STELLAR CORONAE