Results 101 to 110 of about 3,043 (224)

Turbulence and Its Potential Impact on Solar Chromospheric and Coronal Heating

The Astrophysical Journal
Low-frequency turbulence in the solar chromosphere remains poorly understood. We address (1) the sources of low-frequency turbulence that potentially heat the chromosphere, and (2) how turbulence is transported and dissipated throughout the chromosphere ...
G. P. Zank, Xiaocan Li, K. Khanal, Alphonse C. Sterling, M. Nakanotani, L.-L. Zhao, L. Adhikari, M. Yalim, P. S. Athiray, Fan Guo, R. L. Moore   +10 more
doaj   +1 more source

A single frequency approach to nonequilibrium modeling of the chromosphere

Astronomy & Astrophysics
Context. The solar chromosphere is a region where radiation plays a critical role in energy transfer and interacts strongly with the plasma. In this layer, strong spectral lines, such as the Lyman lines, contribute significantly to radiative energy ...
Ruan W., Przybylski D., Cameron R., Solanki S. K.   +3 more
doaj   +1 more source

Current sheets in the solar corona : formation, fragmentation and heating

, 2011
In this thesis we investigate current sheets in the solar corona. The well known 1D model for the tearing mode instability is presented, before progressing to 2D where we introduce a non-uniform resistivity.
Bowness, Ruth
core  

Observations of Locally Excited Waves in the Low Solar Atmosphere Using the Daniel K. Inouye Solar Telescope

The Astrophysical Journal Letters
We present an interpretation of the recent Daniel K. Inouye Solar Telescope (DKIST) observations of propagating wave fronts in the lower solar atmosphere.
Shah Mohammad Bahauddin, Catherine E. Fischer, Mark P. Rast, Ivan Milic, Friedrich Woeger, Matthias Rempel, Peter H. Keys, Thomas R. Rimmele   +7 more
doaj   +1 more source

Solar Wind Acceleration from the Upper Chromosphere to the Corona in Coronal Hole Regions

, 1999
Flow speeds derived in recent years from chromospheric/transition region and coronal observations suggest that the solar wind acceleration process might start at heights in the solar atmosphere much lower than previously imagined.
Esser, Ruth
core  

The formation and stability of Petschek reconnection

, 2014
E. R. Priest is grateful to the Leverhulme Trust. T. G. Forbes received support from NASA grant NNX-10AC04G to the University of New Hampshire. H. Baty acknowledges support by French National Research Agency (ANR) through Grant ANR-13-JS05-0003-01 ...
E. R. Priest, Priest, E.R., Baty, H., T. G. Forbes, Forbes, T.G., H. Baty   +5 more
core   +1 more source

Determining the Magnetic Field in the Atmosphere of a Solar Active Region Observed by the CLASP2.1 Sounding Rocket Experiment

The Astrophysical Journal
We determine magnetic fields from the photosphere to the upper chromosphere combining data from the Hinode satellite and the CLASP2.1 sounding rocket experiment.
Ryohko Ishikawa, Javier Trujillo Bueno, David E. McKenzie, Donguk Song, Tanausú del Pino Alemán, Ernest Alsina Ballester, Luca Belluzzi, Hao Li, Frédéric Auchère, Christian Bethge, Bart De Pontieu, Ryouhei Kano, Ken Kobayashi, Adam R. Kobelski, Takenori J. Okamoto, Laurel A. Rachmeler, Taro Sakao, Jiří Štěpán, Genevieve D. Vigil, Amy Winebarger   +19 more
doaj   +1 more source

LIII. Ionization in the solar chromosphere [PDF]

The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science, 1920
1. 1. In the present paper it has been shown from a discussion of the high-level chromospheric spectrum that this region is chiefly composed of ionized atoms of Calcium, Barium, Strontium, Scandium...
openaire   +1 more source

The solar chromosphere at high resolution with IBIS

, 2008
Context. The exact nature of the quiet solar chromosphere and especially its temporal variation, are still subjects of intense debate. One of the contentious issues is the possible role of the magnetic field in structuring the quieter solar regions.
G. Cauzzi, Reardon, KP, K. P. Reardon, A. Vecchio, Cauzzi, G, Vecchio, Alberto   +5 more
core   +1 more source

Modeling the Solar Chromosphere

, 2007
Spectral diagnostic features formed in the solar chromosphere are few and difficult to interpret -- they are neither formed in the optically thin regime nor in local thermodynamic equilibrium (LTE). To probe the state of the chromosphere, both from observations and theory, it is therefore necessary with modeling.
openaire   +2 more sources