Solar Science with the Atacama Large Millimeter/Submillimeter Array-A New View of Our Sun
Journal article, 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.
Chromosphere
Flares
Prominences
Radiative transfer
Photosphere
Magnetohydrodynamics
Corona
Sun
Author
S. Wedemeyer
Astronomical Institute, Academy of Sciences of the Czech Republic v.v.i.
University of Oslo
T. Bastian
National Radio Astronomy Observatory
R. Brajsa
Astronomical Institute, Academy of Sciences of the Czech Republic v.v.i.
University of Zagreb
H. Hudson
University of Glasgow
University of California
G. Fleishman
New Jersey Institute of Technology
M. Loukitcheva
Max Planck Society
Saint Petersburg State University - Spsu
B. Fleck
NASA Goddard Space Flight Center
E. P. Kontar
University of Glasgow
B. De Pontieu
University of 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, Earth and Space Sciences, Radio Astronomy and Astrophysics
P. Antolin
National Astronomical Observatory of Japan
E. Scullion
Trinity College Dublin
S. Gunar
University of St Andrews
Astronomical Institute, Academy of Sciences of the Czech Republic v.v.i.
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
V. M. Nakariakov
The University of Warwick
T. Ayres
University of Colorado at Boulder
P. Heinzel
Astronomical Institute, Academy of Sciences of the Czech Republic v.v.i.
M. Karlicky
Astronomical Institute, Academy of Sciences of the Czech Republic v.v.i.
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 Society
Kyung Hee University
L. R. van der Voort
University of Oslo
M. Shimojo
National Astronomical Observatory of Japan
Y. Kato
University of Oslo
T. Zaqarashvili
University of Graz
Ilia State University (ISU)
E. Perez
University of Glasgow
C. L. Selhorst
Universidade do Vale do Paraiba
M. Barta
Astronomical Institute, Academy of Sciences of the Czech Republic v.v.i.
Space Science Reviews
0038-6308 (ISSN) 1572-9672 (eISSN)
Vol. 200 1-4 1-73Subject Categories
Astronomy, Astrophysics and Cosmology
DOI
10.1007/s11214-015-0229-9