The energetic atmosphere of the Sun

@misc{wedemeyer2026energetic,
  title = {{The energetic atmosphere of the Sun}},
  author = {Sven Wedemeyer and Mats Kirkaune and Miroslav Barta and Astrid M. Veronig and Stanislav Gunar and Roman Brajsa and Manuela Temmer and Valery Nakariakov and Stephen White and Bart De Pontieu and Maryam Saberi and Atul Mohan and Masumi Shimojo and Davor Sudar and Galina Motorina and Maria Loukitcheva and Paulo Simoes and Stefaan Poedts and Raghavendra Sahai},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.20934},
  eprint = {2610.20934},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.20934},
  note = {CC BY 4.0},
}

TY  - UNPB
TI  - The energetic atmosphere of the Sun
AU  - Sven Wedemeyer
AU  - Mats Kirkaune
AU  - Miroslav Barta
AU  - Astrid M. Veronig
AU  - Stanislav Gunar
AU  - Roman Brajsa
AU  - Manuela Temmer
AU  - Valery Nakariakov
AU  - Stephen White
AU  - Bart De Pontieu
AU  - Maryam Saberi
AU  - Atul Mohan
AU  - Masumi Shimojo
AU  - Davor Sudar
AU  - Galina Motorina
AU  - Maria Loukitcheva
AU  - Paulo Simoes
AU  - Stefaan Poedts
AU  - Raghavendra Sahai
PY  - 2026
DA  - 2026/10/14
PB  - arXiv
DO  - 10.48550/arxiv.2610.20934
UR  - https://arxiv.org/abs/2610.20934
AB  - Understanding the mechanisms that heat the Sun's chromosphere and corona to temperatures far exceeding those of the solar photosphere below remains one of the central challenges in solar physics. Small-scale, rapidly evolving processes - including shocks, turbulence, magnetohydrodynamic waves, reconnection-driven jets, and nano-flares - are thought to contribute significantly to the heating budget. However, direct observational constraints on their spatial, temporal, and spectral signatures remain hard to obtain. At millimeter wavelengths, optically thick thermal emission provides a comparatively direct measure of gas temperature. While the Atacama Large Millimeter/submillimeter Array (ALMA) already provides unique diagnostic capabilities, offering temperature diagnostics and high-cadence imaging, the current capabilities are still limiting the study of such dynamic, small-scale phenomena. Improved spatial resolution, enhanced uv-coverage, and simultaneous multi-band observations, as proposed for ALMA2040, would enable transformative progress in capturing dynamic processes across multiple heights and enable time-dependent three-dimensional thermal and magnetic tomography of the chromosphere. Combined with complementary diagnostics and simulations, these measurements would test how small-scale processes contribute to atmospheric heating.
ER  -