According to Parker a nanoflare arises from an event of magnetic reconnection which converts the energy stored in the solar magnetic field into the motion of the plasma. The plasma motion (thought as fluid motion) occurs at length-scales so small that it is soon dumped by the turbulence and then by the viscosity. In such a way the energy is quickly converted into heat, and conducted by the free electrons along the magnetic field lines closer to the place where the nanoflare switches on. In order to heat a region of very high X-ray emission, over an area 1" x 1", a nanoflare of 1017 J should happen every 20 seconds, and 1000 nanoflares per second should occur in a large active region of 105 x 105 km2. On the basis of this theory, the emission coming from a big flare could be caused by a series of micro-nanoflares, not observable individually.
Nanoflares and coronal activity
The observations show that the solar magnetic field, which is frozen into the motion of the plasma in the photosphere, opens into semicirculal structures in the corona. These coronal loops, which can be seen in the EUV and X-ray images (see the figure on the left), confine very hot plasma, emitting as it were at a temperature of a few million degrees.
Many flux tubes are stable for several days on the solar corona in the 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 coronal heating is released by current dissipation or Joule effect.
However, at first, astronomers believed that a single event of magnetic reconnection was responsible for very dynamic processes like flares and other phenomena linked to coronal activity. On the other hand, the theory of nanoflares supposes that these events of magnetic reconnection, occurring at the same time on small length-scales wherever in the corona, are very numerous and give only a small fraction of energy. These nanoflares might be very tiny flares, so close one to each other, both in time and in space, to heat the corona and to cause all the phenomena due to solar activity.
The sudden light bursts periodically observed in active regions as well as flares and coronal mass ejections could be provoked by cascade effects, similar to those described by the mathematical theories of catastrophes. In the hypothesis that the solar corona is in a state of self-organized criticality, the stressing of the magnetic field should be enhanced until a small perturbation switches on many small instabilities, happening together as it occurs in avalanches.
One of the experimental results supporting this theory is the fact that the distribution of the number of flares observed in the hard X-rays is a function of the energy, following a power law with negative spectral index 1.8   . Actually, though, a negative spectral index larger than 2 is required in order to maintain the solar corona via the nanoflare hypothesis .
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 solar magnetic field can account for the coronal heating necessary to maintain the plasma at this temperature and to balance coronal radiative losses .
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 . 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 emission lines, which are formed from ionized atoms (oxygen, carbon, iron and so on).
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 corona or mainly in the higher corona, where the magnetic field lines open into the space heliosphere, driving the solar wind into the solar system.
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.
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 Alfvén waves generated by convective motions in the photosphere can go through the chromosphere and transition region, carrying an energy flux comparable to that required to sustain the corona. Anyway, wavetrain periods observed in the high chromosphere and in the lower transition region are of the order of 3-5 min. These times are longer than the time taken by Alfvén waves to cross a typical coronal loop. This means that most of the dissipative mechanisms may provide enough energy only at distances further from the solar corona. More probably, the Alfvén waves are responsible for the acceleration of the solar wind in coronal holes.
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 transformed into electric one and then into heat for Joule effect. 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 coronal loops are stable and so hot at the same time.
The Ohmic dissipation by currents could be a valid alternative to explain the coronal activity. For many years the magnetic reconnection has been invoked as the main power source of solar flares. However this heating mechanism is not very efficient in large current sheets, while more energy is released in turbulent regimes when nanoflares happen at much smaller scale-lengths, where non-linear effects are not negligible.
- "NASA - Tiny Flares Responsible for Outsized Heat of Sun's Atmosphere". Retrieved 23 September 2014.
- Gold, T. (1964). "The Physics of Solar Flares". Nasa Sp. 50, ed. W.Hess: 380.
- Parker, Eugene N. (1972). The Astrophysical Journal 174: 499. doi:10.1086/151512. Missing or empty
- Datlowe, D.W.; Elcan, M. J.; Hudson, H. S. (1974). "OSO-7 observations of solar x-rays in the energy range 10?100 keV". Solar Physics 39: 155. Bibcode:1974SoPh...39..155D. doi:10.1007/BF00154978.
- Lin, R. P.; Schwartz, R. A.; Kane, S. R.; Pelling, R. M. et al. (1984). "Solar hard X-ray microflares". The Astrophysical Journal 283: 421. Bibcode:1984ApJ...283..421L. doi:10.1086/162321.
- Dennis, Brian R. (1985). "Solar hard X-ray bursts". Solar Physics 100: 465. Bibcode:1985SoPh..100..465D. doi:10.1007/BF00158441.
- Porter, J. G.; Fontenla, J. M.; Simnett, G. M. (1995). "Simultaneous ultraviolet and X-ray observations of solar microflares". The Astrophysical Journal 438: 472. Bibcode:1995ApJ...438..472P. doi:10.1086/175091.
- Hudson; H.S. (1991). "Solar flares, microflares, nanoflares, and coronal heating". Solar Physics 133: 357. Bibcode:1991SoPh..133..357H. doi:10.1007/BF00149894.
- Withbroe, G. L.; Noyes, R. W. (1977). "Mass and energy flow in the solar chromosphere and corona". Annual Reviews Astronomy & Astrophysics 15: 363–387. Bibcode:1977ARA&A..15..363W. doi:10.1146/annurev.aa.15.090177.002051.
- Priest, Eric (1982). Solar Magneto-hydrodynamics. D.Reidel Publishing Company, Dordrecht, Holland. p. 208.
- Poletto G; Vaiana GS; Zombeck MV; Krieger AS et al. (Sep 1975). "A comparison of coronal X-ray structures of active regions with magnetic fields computed from photospheric observations". Solar Phys. 44 (9): 83–99. Bibcode:1975SoPh...44...83P. doi:10.1007/BF00156848.
- Rappazzo, A. F.; Velli, M.; Einaudi, G.; Dahlburg, R. B. (2008). "Nonlinear Dynamics of the Parker Scenario for Coronal Heating". The Astrophysical Journal 677 (2): 1348–1366. arXiv:0709.3687. Bibcode:2008ApJ...677.1348R. doi:10.1086/528786.
- Nasa news Tiny Flares Responsible for Outsized Heat of Sun's Atmosphere.