Solar Science with the Atacama Large Millimeter/Submillimeter Array-A New View of Our Sun
Reviewartikel, 2016
The Atacama Large Millimeter/submillimeter Array (ALMA) is a new powerful tool for observing the Sun at high spatial, temporal, and spectral resolution. These capabilities can address a broad range of fundamental scientific questions in solar physics. The radiation observed by ALMA originates mostly from the chromosphere-a complex and dynamic region between the photosphere and corona, which plays a crucial role in the transport of energy and matter and, ultimately, the heating of the outer layers of the solar atmosphere. Based on first solar test observations, strategies for regular solar campaigns are currently being developed. State-of-the-art numerical simulations of the solar atmosphere and modeling of instrumental effects can help constrain and optimize future observing modes for ALMA. Here we present a short technical description of ALMA and an overview of past efforts and future possibilities for solar observations at submillimeter and millimeter wavelengths. In addition, selected numerical simulations and observations at other wavelengths demonstrate ALMA's scientific potential for studying the Sun for a large range of science cases.
Flares
Sun
Photosphere
Prominences
Magnetohydrodynamics
Corona
Chromosphere
Radiative transfer
Författare
S. Wedemeyer
Universitetet i Oslo
Czech Academy of Sciences
T. Bastian
National Radio Astronomy Observatory
R. Brajsa
Sveučilište u Zagrebu
Czech Academy of Sciences
H. Hudson
University of Glasgow
University of California
G. Fleishman
New Jersey Institute of Technology
M. Loukitcheva
Saint Petersburg State University - Spsu
Max-Planck-Gesellschaft
B. Fleck
NASA Goddard Space Flight Center
E. P. Kontar
University of Glasgow
B. De Pontieu
Universitetet i Oslo
Lockheed Martin Corporation
P. Yagoubov
European Southern Observatory (ESO)
S. K. Tiwari
NASA Marshall Space Flight Center
R. Soler
Universitat de les Illes Balears
John H Black
Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik
P. Antolin
National Astronomical Observatory of Japan
E. Scullion
Trinity College Dublin
S. Gunar
Czech Academy of Sciences
University of St Andrews
N. Labrosse
University of Glasgow
H. G. Ludwig
Astronomisches Rechen-Institut Heidelberg
A. O. Benz
Fachhochschule Nordwestschweiz
S. M. White
Kirtland Air Force Base
P. H. Hauschildt
Universität Hamburg
J. G. Doyle
Armagh Observatory and Planetarium
V. M. Nakariakov
The University of Warwick
T. Ayres
University of Colorado at Boulder
P. Heinzel
Czech Academy of Sciences
M. Karlicky
Czech Academy of Sciences
T. Van Doorsselaere
KU Leuven
D. Gary
New Jersey Institute of Technology
C. E. Alissandrakis
University of Ioannina
A. Nindos
University of Ioannina
S. K. Solanki
Max-Planck-Gesellschaft
Kyung Hee University
L. R. van der Voort
Universitetet i Oslo
M. Shimojo
National Astronomical Observatory of Japan
Y. Kato
Universitetet i Oslo
T. Zaqarashvili
Karl-Franzens-Universität Graz
Ilia State University (ISU)
E. Perez
University of Glasgow
C. L. Selhorst
Universidade do Vale do Paraiba
M. Barta
Czech Academy of Sciences
Space Science Reviews
0038-6308 (ISSN) 1572-9672 (eISSN)
Vol. 200 1-4 1-73Ämneskategorier
Astronomi, astrofysik och kosmologi
DOI
10.1007/s11214-015-0229-9