Waves in the Chromosphere: Observations

@article{Rutten2003WavesIT,
  title={Waves in the Chromosphere: Observations},
  author={Robert J. Rutten},
  journal={arXiv: Solar and Stellar Astrophysics},
  year={2003},
  pages={145-166}
}
  • R. Rutten
  • Published 6 December 2010
  • Physics
  • arXiv: Solar and Stellar Astrophysics
I review the literature on observational aspects of waves in the solar chromosphere in the first part of this contribution. High-frequency waves are invoked to build elaborate cool-star chromosphere heating theories but have not been detected decisively so far, neither as magnetic modes in network elements nor as acoustic modes in below- the-canopy internetwork regions. Three-minute upward-propagating acoustic shocks are thoroughly established through numerical simulation as the cause of… Expand

Figures from this paper

The quiet-Sun photosphere and chromosphere
  • R. Rutten
  • Physics, Medicine
  • Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences
  • 2012
The overall structure and the fine structure of the solar photosphere outside active regions are largely understood, except possibly the important roles of a turbulent near-surface dynamo at itsExpand
Nonlinear waves in the solar atmosphere
  • M. Ruderman
  • Physics, Biology
  • Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences
  • 2005
TLDR
This paper gives a brief description of propagation and damping of nonlinear sound waves in the stratified solar atmosphere, and points out that the acoustic heating remains the most popular theory of heating the lower chromosphere. Expand
Explaining Inverted Temperature Loops in the Quiet Solar Corona with Magnetohydrodynamic Wave Mode Conversion
Coronal loops trace out bipolar, arch-like magnetic fields above the Sun's surface. Recent measurements that combine rotational tomography, extreme ultraviolet imaging, and potential-fieldExpand
DOT tomography of the solar atmosphere. II. Reversed granulation in Ca II H
High-quality simultaneous image sequences from the Dutch Open Telescope (DOT) in the G band and the Ca  H line are used to quantify the occurrence of reversed granulation as a constituent of theExpand
A Hot Downflowing Model Atmosphere For Umbral Flashes And The Physical Properties Of Their Dark Fibrils
We perform NLTE inversions in a large set of umbral flashes, including the dark fibrils visible within them, and in the quiescent umbra by using the inversion code NICOLE on a set of full StokesExpand
Umbral chromospheric fine structure and umbral flashes modelled as one: The corrugated umbra
Small-scale umbral brightenings (SSUBs), umbral microjets, spikes or short dynamic fibrils (SDFs), and umbral dark fibrils are found in any observation of the chromosphere with sufficient spatialExpand

References

SHOWING 1-10 OF 141 REFERENCES
Oscillations of the Sun's chromosphere. VI: K grains, resonances, and gravity waves
We present observations of simultaneous filtergram time sequences in Mg b 2 , Ca K and Hα obtained from quiet Sun disc centre with the Vacuum Tower Telescope at Observatorio del Teide, Tenerife.Expand
Dynamics of the solar chromosphere - III. Ultraviolet brightness oscillations from TRACE
We analyze oscillations in the solar atmosphere using image sequences from the Transition Region and Coronal Explorer (TRACE) in three ultraviolet passbands which sample the upper solar photosphereExpand
Solar atmospheric dynamics. II - Nonlinear models of the photospheric and chromospheric oscillations
The one-dimensional, nonlinear dynamics of the solar atmosphere is investigated, and models of the observed photospheric (300 s) and chromospheric (200 s) oscillations are described. These areExpand
Dynamics of the solar chromosphere. I - Long-period network oscillations
We analyze differences in solar oscillations between the chromospheric network and internetwork regions from a 1 hr sequence of spectrograms of a quiet region near disk center. The spectrogramsExpand
Acoustic and magnetic wave heating in stars . II. On the range of chromospheric activity
In the rst paper of this series we developed a method to construct theoretical, time-dependent and two-component chromosphere models for late-type main sequence stars. The models consist ofExpand
DOES THE SUN HAVE A FULL-TIME CHROMOSPHERE?
The successful modeling of the dynamics of H2v bright points in the nonmagnetic chromosphere by Carlsson & Stein gave as a by-product a part-time chromosphere lacking the persistent outwardExpand
Excitation of Chromospheric Wave Transients by Collapsing Granules
The excitation of acoustic waves is studied using three-dimensional numerical simulations of the nonmagnetic solar atmosphere and the upper convection zone. Transient acoustic waves in the atmosphereExpand
An Observational Manifestation of Magnetoatmospheric Waves in Internetwork Regions of the Chromosphere and Transition Region
We discuss an observational signature of magnetoatmospheric waves in the chromosphere and transition region away from network magnetic fields. We demonstrate that when the observed quantity, line orExpand
Waves in the Magnetized Solar Atmosphere. I. Basic Processes and Internetwork Oscillations
We have modeled numerically the propagation of waves through magnetic structures in a stratified atmosphere. We first simulate the propagation of waves through a number of simple, exemplary fieldExpand
Excitation of Oscillations in the Magnetic Network on the Sun.
TLDR
The effects of turbulent convective flows on flux tubes in intergranular lanes and the wave energy flux in upward-propagating transverse waves is considered and it is found that the energy flux can in principle carry adequate energy for chromospheric heating. Expand
...
1
2
3
4
5
...