![gas of sun corona gas of sun corona](https://www.scu.edu/media/portals/illuminate/blog/Illuminate-PhilKesten-28.2.png)
![gas of sun corona gas of sun corona](https://solar.physics.montana.edu/YPOP/Spotlight/SunInfo/Images/sundiag.gif)
![gas of sun corona gas of sun corona](https://www.lpi.usra.edu/publications/slidesets/3dsolarsystem/images/s3d_s01.gif)
The solar magnetic field plays a key role in the heating mechanism in the Sun. However, it is not clear whether this mechanism can universally explain the formation of the ultra-high temperature gas and the radiation emitted at different wavelengths in all active solar-type stars. In the Sun, the main theory is that convective motion on the solar surface shakes the magnetic field lines, and this energy is transmitted upwards to heat the corona and chromosphere. This suggests that active stars when young, including the Sun, had a strong influence on the evolution of the climate and habitability of their orbiting planets.ĭespite this importance, the mechanism of the corona and chromosphere remains poorly understood (※2). In particular, the Sun in the past (and young solar-type stars) is thought to have generated X-rays and ultraviolent rays that are 10 to 1000 times stronger than emitted today. These ultra-high temperature layers emit X-rays and ultraviolet radiation that play an important role in the formation and photochemical reactions in the atmosphere of Solar System and extrasolar planets. However, the stellar atmosphere of these stars includes the corona with a temperature of over 1 million degrees Celsius, and the chromosphere which can reach temperatures of 10,000 degrees Celsius. The stellar surface of the Sun and solar-type stars (※1) have temperatures of about 6000 degrees Celsius. Additionally, the extension of this research will provide X-ray and ultraviolent stellar spectra that can be used for input in planetary atmospheric formation and dissipation models, allowing us to examine the climate and habitability of exoplanets with greater precision. The heating mechanism of the corona and chromosphere shown in this study is expected to be understood more precisely in the up-coming detailed Sun and stellar observations by the next-generation satellites such as Solar-C (EUVST) and WSO-UV.Comparison with observational data of solar-type stars showed that this correlation is shared between the Sun and other solar-type stars. Multi-wavelength long-term observations of the Sun have revealed a correlation between the magnetic field on the Sun's surface and the emission lines at different wavelengths (X-ray, ultraviolet, visible light and radio waves) emitted from the corona and chromosphere.Dr TORIUMI Shin, an International Top Young Fellow (ITYF) at the Institute of Astronautical Science at JAXA, and Professor Vladimir AIRAPETIAN at NASA GSFC/American University combined and analyzed solar and stellar observational data to reveal that the ultra-hot gas universally present in these stars is heated by a common mechanism, independent of the age or activity level of the star.By combining the results of this work with detailed observations using the next-generation solar observation satellites and space telescopes, it will be possible to reproduce the X-ray and ultraviolet spectra from a variety of stars, which will allow the habitability of exoplanets to be examined more precisely. This is key evidence that the ultra-high temperature gas in the Sun and in solar-type stars is heated by a common mechanism, independent of the star's age or activity, and that specifically, the energy is transmitted through the magnetic field extending outwards from the stellar surface into space. The results found that the correlation between the magnetic field of the Sun and the emission lines is exactly replicated in solar-type stars at all wavelength bands.
![gas of sun corona gas of sun corona](https://study.com/cimages/multimages/16/bb08afed-7b31-4149-8212-855a79fb01b7_rsz_sun.jpg)
This study compared and analyzed 10 years of multi-wavelength observation data from the Sun, and that of previous observations of solar-type stars, and investigated correlations in their surface magnetic fields, and the emission lines at different wavelengths in the corona and chromosphere (X-rays, ultraviolet, visible light and radio waves). However, it has remained an unresolved mystery as to how this ultra-high temperature gas in the stars is heated, particularly whether a heating and radiation mechanism is common to all solar-type stars. These high-energy X-ray and UV photons can impact the climate and habitability of any surrounding planets by stripping their atmospheres and instigating photochemical reactions. The surface of the Sun and solar-type stars is at a cooler 6,000 degrees, but the ultra-hot gases of the corona and chromosphere are hot enough to emit X-rays and ultraviolet rays. The Sun and solar-type stars (stars similar to the Sun but with a variety of ages and activity levels) have coronae with temperatures exceeding 1 million degrees Celsius, and chromospheres whose temperatures extend up to 10,000 degrees.