### Abstract

Original language | English |
---|---|

Pages (from-to) | 33 - 50 |

Number of pages | 18 |

Journal | Solar Physics |

Volume | 280 |

Issue number | 1 |

DOIs | |

Publication status | Published - 2012 |

### Cite this

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*Solar Physics*, vol. 280, no. 1, pp. 33 - 50. https://doi.org/10.1007/s11207-012-0052-3

**Alfven reflection and reverberation in the solar atmosphere.** / Cally, Paul Stuart.

Research output: Contribution to journal › Article › Research › peer-review

TY - JOUR

T1 - Alfven reflection and reverberation in the solar atmosphere

AU - Cally, Paul Stuart

PY - 2012

Y1 - 2012

N2 - Magneto-atmospheres with Alfven speed [a] that increases monotonically with height are often used to model the solar atmosphere, at least out to several solar radii. A common example involves a uniform vertical or inclined magnetic field in an isothermal atmosphere, for which the Alfven speed is exponential. We address the issue of internal reflection in such atmospheres, both for time-harmonic and for transient waves. It is found that a mathematical boundary condition may be devised that corresponds to perfect absorption at infinity, and, using this, that many atmospheres where a(x) is analytic and unbounded present no internal reflection of harmonic Alfven waves. However, except for certain special cases, such solutions are accompanied by a wake, which may be thought of as a kind of reflection. For the initial-value problem where a harmonic source is suddenly switched on (and optionally off), there is also an associated transient that normally decays with time as or , depending on the phase of the driver. Unlike the steady-state harmonic solutions, the transient does reflect weakly. Alfven waves in the solar corona driven by a finite-duration train of p-modes are expected to leave such transients.

AB - Magneto-atmospheres with Alfven speed [a] that increases monotonically with height are often used to model the solar atmosphere, at least out to several solar radii. A common example involves a uniform vertical or inclined magnetic field in an isothermal atmosphere, for which the Alfven speed is exponential. We address the issue of internal reflection in such atmospheres, both for time-harmonic and for transient waves. It is found that a mathematical boundary condition may be devised that corresponds to perfect absorption at infinity, and, using this, that many atmospheres where a(x) is analytic and unbounded present no internal reflection of harmonic Alfven waves. However, except for certain special cases, such solutions are accompanied by a wake, which may be thought of as a kind of reflection. For the initial-value problem where a harmonic source is suddenly switched on (and optionally off), there is also an associated transient that normally decays with time as or , depending on the phase of the driver. Unlike the steady-state harmonic solutions, the transient does reflect weakly. Alfven waves in the solar corona driven by a finite-duration train of p-modes are expected to leave such transients.

UR - http://link.springer.com/article/10.1007%2Fs11207-012-0052-3

U2 - 10.1007/s11207-012-0052-3

DO - 10.1007/s11207-012-0052-3

M3 - Article

VL - 280

SP - 33

EP - 50

JO - Solar Physics

JF - Solar Physics

SN - 0038-0938

IS - 1

ER -