SSALMON - The Solar Simulations for the Atacama Large Millimeter Observatory Network
arXiv:1502.05601 · doi:10.1016/j.asr.2015.05.027
Abstract
The Solar Simulations for the Atacama Large Millimeter Observatory Network (SSALMON) was initiated in 2014 in connection with two ALMA development studies. The Atacama Large Millimeter/submillimeter Array (ALMA) is a powerful new tool, which can also observe the Sun at high spatial, temporal, and spectral resolution. The international SSALMONetwork aims at coordinating the further development of solar observing modes for ALMA and at promoting scientific opportunities for solar physics with particular focus on numerical simulations, which can provide important constraints for the observing modes and can aid the interpretation of future observations. The radiation detected by ALMA originates mostly in the solar chromosphere - a complex and dynamic layer between the photosphere and corona, which plays an important role in the transport of energy and matter and the heating of the outer layers of the solar atmosphere. Potential targets include active regions, prominences, quiet Sun regions, flares. Here, we give a brief overview over the network and potential science cases for future solar observations with ALMA.
15 pages, 3 figures, to appear in Advances in Solar Physics (special issue of Advances in Space Research, AdSR), proceedings of the 14th European Solar Physics Meeting (ESPM-14, Dublin, Ireland, September 2014); (resubmitted version after minor revision)
References in corpus (27)
- Alfven Waves in the Lower Solar Atmosphere
- Dynamic Fibrils are driven by Magnetoacoustic Shocks
- Nonlinear Instability of kink oscillations due to shear motions
- On the prevalence of small-scale twist in the solar chromosphere and transition region
- Fine strand-like structure in the solar corona from MHD transverse oscillations
- Solar Carbon Monoxide, Thermal Profiling, and the Abundances of C, O, and their Isotopes
- Resonant Absorption of Transverse Oscillations and Associated Heating in a Solar Prominence. I- Observational aspects
- Coupling from the photosphere to the chromosphere and the corona
- Resonant absorption in complicated plasma configurations: applications to multi-stranded coronal loop oscillations
- Dynamics of the Solar Magnetic Network. II. Heating the Magnetized Chromosphere
- 3D Radio and X-Ray Modeling and Data Analysis Software: Revealing Flare Complexity
- Observations of Subarcsecond Bright Dots in the Transition Region above Sunspots with the Interface Region Imaging Spectrograph
- Damping of Fast Magnetohydrodynamic Oscillations in Quiescent Filament Threads
- Millimeter radiation from a 3D model of the solar atmosphere I. Diagnosing chromospheric thermal structure
- The signature of chromospheric heating in Ca II H spectra
- Unresolved fine-scale structure in solar coronal loop-tops
- Overdamped Alfven waves due to ion-neutral collisions in the solar chromosphere
- Inter-network regions of the Sun at millimetre wavelengths
- Conditions for Photospherically Driven Alfvenic Oscillations to Heat the Solar Chromosphere by Pedersen Current Dissipation
- South Pole Telescope Detections of the Previously Unconfirmed Planck Early SZ Clusters in the Southern Hemisphere
- Trigger Mechanism of Solar Subflares in a Braided Coronal Magnetic Structure
- Generation of electric currents in the chromosphere via neutral-ion drag
- ALMA observations of alpha Centauri: First detection of main-sequence stars at 3mm wavelength
- Carbon monoxide in the solar atmosphere II. Radiative cooling by CO lines
- ALMA as the ideal probe of the solar chromosphere
- The contribution of microbunching instability to solar flare emission in the GHz to THz range of frequencies
- On the Nature of the Solar Chromosphere