Results 1 to 10 of about 418 (148)

Thermal structuring of the quiet solar corona

Astronomy & Astrophysics
Context. The quiet solar atmosphere is populated with plasma loops that are typically observed in the ultraviolet (UV) and extreme-ultraviolet (EUV) wavelengths.
Milanović N., Peter H., Chitta L. P., Young P. R.   +3 more
doaj   +5 more sources

LOFAR observations of the quiet solar corona [PDF]

Astronomy and Astrophysics, 2018
Context. The quiet solar corona emits meter-wave thermal bremsstrahlung. Coronal radio emission can only propagate above that radius, Rω, where the local plasma frequency equals the observing frequency. The radio interferometer LOw Frequency ARray (LOFAR) observes in its low band (10–90 MHz) solar radio emission originating from the middle and upper ...
Christian Vocks, Peter T Gallagher, Frank Breitling   +2 more
exaly   +5 more sources

Formation of suprathermal electron distributions in the quiet solar corona [PDF]

Astronomy and Astrophysics, 2008
Summary: Context. Solar wind electron velocity distribution functions (VDFs) show enhanced levels of suprathermal electrons as compared to a Maxwellian distribution. Previous studies show that the suprathermal tails of solar wind VDFs can be fitted by kappa distributions, and that a coronal origin of the suprathermal electrons is possible. Aims.
Vocks, C., Mann, G., Rausche, G.
exaly   +2 more sources

Multifrequency Microwave Imaging of Weak Transients from the Quiet Solar Corona

The Astrophysical Journal, 2023
Understanding the dynamics of the quiet solar corona is important for answering key questions including the coronal heating problem. Multiple studies have suggested small-scale magnetic-reconnection events may play a crucial role.
Surajit Mondal, Bin Chen, Sijie Yu
doaj   +3 more sources

Relevant heating of the quiet solar corona by Alfvén waves: a result of adiabaticity breakdown. [PDF]

Sci Rep, 2019
AbstractIon heating by Alfvén waves has been considered for long as the mechanism explaining why the solar corona has a temperature several orders of magnitude higher than the photosphere. Unfortunately, as the measured wave frequencies are much smaller than the ion cyclotron frequency, particles were expected to behave adiabatically, impeding a direct
Escande DF, Gondret V, Sattin F.
europepmc   +5 more sources

Transient small-scale brightenings in the quiet solar corona: A model for campfires observed with Solar Orbiter [PDF]

Astronomy and Astrophysics, 2021
Context. Recent observations by the Extreme Ultraviolet Imager (EUI) on board Solar Orbiter have characterized prevalent small-scale transient brightenings in the corona above the quiet Sun termed campfires. Aims. In this study we search for comparable brightenings in a numerical model and then investigate their relation to the magnetic field and the ...
Yajie Chen, Hardi Peter, Hui Tian
exaly   +5 more sources

Measuring the Magnetic-Field Strength of the Quiet Solar Corona Using “EIT Waves” [PDF]

Solar Physics, 2013
20 pages, 7 figures, accepted for publication in Solar ...
Stéphane Regnier, David R Williams, David M Long   +2 more
exaly   +5 more sources

Slow wind belt in the quiet solar corona

Physics of Plasmas, 2023
The slow solar wind belt in the quiet corona, observed with the Metis coronagraph on board Solar Orbiter on May 15, 2020, during the activity minimum of the cycle 24, in a field of view extending from 3.8 R⊙ to 7.0 R⊙, is formed by a slow and dense wind stream running along the coronal current sheet, accelerating in the radial direction and reaching at
Fabio Frassetto, Vania da Deppo, Luca Teriaca   +2 more
exaly   +5 more sources

A nanoflare heating model for the quiet solar corona [PDF]

Astronomy and Astrophysics, 2001
11 pages, 7 figures, updated spelling of 1st autor's ...
A O Benz
exaly   +3 more sources

First Radio Evidence for Impulsive Heating Contribution to the Quiet Solar Corona [PDF]

Astrophysical Journal Letters, 2020
Abstract This Letter explores the relevance of nanoflare-based models for heating the quiet Sun corona. Using meterwave data from the Murchison Widefield Array, we present the first successful detection of impulsive emissions down to flux densities of ∼mSFU, about two orders of magnitude weaker than earlier attempts.
Atul Mohan, Surajit Mondal, Divya Oberoi   +2 more
exaly   +3 more sources