Nanoflare
A nanoflare is a very small episodic heating event which happens in the
The hypothesis of small impulsive heating events as a possible explanation of the coronal heating was first suggested by Thomas Gold[2] and then later developed and dubbed "nanoflares" by Eugene Parker.[3]
According to Parker a nanoflare arises from an event of
The nanoflare model has long suffered from a lack of observational evidence. Simulations predict that nanoflares produce a faint, hot (~10 MK) component of the emission measure.[4] Current instruments, such as the Extreme-Ultraviolet Imaging Spectrometer on board Hinode, are not adequately sensitive to the range in which this faint emission occurs, making a confident detection impossible.[5] Recent evidence from the EUNIS sounding rocket has provided some spectral evidence for non-flaring plasma at temperatures near 9 MK in active region cores.[6]
Nanoflares and coronal activity
Telescopic observations suggest that the
Many flux tubes are relatively stable as seen in soft X-ray images, emitting at steady rate. However flickerings, brightenings, small explosions, bright points, flares and mass eruptions are observed very frequently, especially in active regions. These macroscopic signs of solar activity are considered by astrophysicists as the phenomenology related to events of relaxation of stressed magnetic fields, during which part of the energy they have stored is released ultimately into particle kinetic energy (heating); this could be via current dissipation, Joule effect, or any of several non-thermal plasma effects.
Theoretical work often appeals to the concept of magnetic reconnection to explain these outbursts. Rather than a single large-scale episode of such a process, though, modern thinking suggests that a multitude of small-scale versions reconnection, cascading together, might be a better description. The theory of nanoflares then supposes that these events of magnetic reconnection, occurring at nearly the same time on small length-scales wherever in the corona, are very numerous, each providing an imperceptibly small fraction of the total energy required in a macroscopic event. These nanoflares might themselves resemble very tiny flares, close one to each other, both in time and in space, effectively heating the corona and underlying many of the phenomena of solar magnetic activity.
Episodic heating often observed in
One of the experimental results often cited in supporting the nanoflare theory is the fact that the distribution of the number of flares observed in the hard X-rays is a function of their energy, following a power law with negative spectral index. A sufficiently large power-law index would allow the smallest events to dominate the total energy. In the energy range of normal flares, the index has a value of approximately -1.8[7] [8] [9] .[10] This falls short of the power-law index which would be required order to maintain the heating of the
Nanoflares and coronal heating
The problem of coronal heating is still unsolved, although research is ongoing and other evidence of nanoflares has been found in the solar corona. The amount of energy stored in the
The radiation is not the only mechanism of energy loss in the corona: since the plasma is highly ionized and the magnetic field is well organized, the thermal conduction is a competitive process. The energy losses due to the thermal conduction are of the same order of coronal radiative losses. The energy released in the corona which is not radiated externally is conducted back towards the chromosphere along the arcs. In the transition region where the temperature is about 104 -105 K, radiative losses are too high to be balanced by any form of mechanical heating.[13] The very high temperature gradient observed in this range of temperatures increases the conductive flux in order to supply for the irradiated power. In other words, the transition region is so steep (the temperature increases from 10kK to 1MK in a distance of the order of 100 km) because the thermal conduction from the superior hotter atmosphere must balance the high radiative losses, as indicated to the numerous
The solar convection can supply the required heating, but in a way not yet known in detail. Actually, it is still unclear how this energy is transmitted from the chromosphere(where it could be absorbed or reflected), and then dissipated into the corona instead of dispersing into the solar wind. Furthermore, where does it occur exactly? In the low
The importance of the magnetic field is recognized by all the scientists: there is a strict correspondence between the active regions, where the irradiated flux is higher (especially in the X-rays), and the regions of intense magnetic field.[14]
The problem of coronal heating is complicated by the fact that different coronal features require very different amounts of energy. It is difficult to believe that very dynamic and energetic phenomena such as flares and coronal mass ejections share the same source of energy with stable structures covering very large areas on the Sun: if nanoflares would have heated the whole corona, then they should be distributed so uniformly so as to look like a steady heating. Flares themselves – and microflares, which when studied in detail seem to have the same physics – are highly intermittent in space and time, and would not therefore be relevant to any requirement for continuous heating. On the other hand, in order to explain very rapid and energetic phenomena such as solar flares, the magnetic field should be structured on distances of the order of the metre.
The
The theory initially developed by Parker of micro-nanoflares is one of those explaining the heating of the corona as the dissipation of electric currents generated by a spontaneous relaxation of the magnetic field towards a configuration of lower energy. The magnetic energy is thus transformed into Joule heating. The braiding of the field lines of the coronal magnetic flux tubes provokes events of magnetic reconnection with a consequent change of the magnetic field at small length-scales without a simultaneous alteration of the magnetic field lines at large length-scales. In this way it can be explained why
The Ohmic dissipation by currents could be a valid alternative to explain the coronal activity. For many years the
In 2020, a study published in Nature
See also
- Chromosphere
- Stellar corona
- Coronal cloud
- Coronal loops
- Coronal mass ejection
- Coronal radiative losses
- Current sheet
- Magnetic reconnection
- Neupert effect
- Photosphere
- Plasma physics
- Solar flare
- Solar transition region
- Solar wind
- Sun
- Sunspot
- X-ray astronomy
References
- ^ "NASA - Tiny Flares Responsible for Outsized Heat of Sun's Atmosphere". Retrieved 23 September 2014.
- PMID 25897093.
- doi:10.1086/151512.
- S2CID 119329755.
- S2CID 120517153.
- .
- S2CID 122521337.
- doi:10.1086/162321.
- S2CID 189827655.
- doi:10.1086/175091.
- S2CID 120428719.
- .
- ^ Priest, Eric (1982). Solar Magneto-hydrodynamics. D.Reidel Publishing Company, Dordrecht, Holland. p. 208.
- S2CID 121538547.
- S2CID 15598925.
- ISSN 2397-3366.
- ^ "This May Be the First Complete Observation of a Nanoflare - NASA". Retrieved 2023-11-01.
External links
- Nasa news Tiny Flares Responsible for Outsized Heat of Sun's Atmosphere.