Хромосфера звезды: структура и особенности

Layer of a star's atmosphere

A chromosphere ("sphere of color") is the second layer of a star's atmosphere, located above the photosphere and below the solar transition region and corona. The term usually refers to the Sun's chromosphere, but not exclusively. In the Sun's atmosphere, the chromosphere is roughly in height, or slightly more than 1% of the Sun's radius at maximum thickness. It possesses a homogeneous layer at the boundary with the photosphere. Hair like jets of plasma, called spicules, rise from this homogeneous region and through the chromosphere, extending up to into the corona above. The chromosphere has a characteristic red color due to electromagnetic emissions in the Hα spectral line. Information about the chromosphere is primarily obtained by analysis of its emitted electromagnetic radiation. The chromosphere is also visible in the light emitted by ionized calcium, Ca II, in the violet part of the solar spectrum at a wavelength of 393.4 nanometers (the Calcium K line). Chromospheres have also been observed on stars other than the Sun. On large stars, chromospheres sometimes make up a significant proportion of the entire star. For example, the chromosphere of supergiant star Antares has been found to be about 2.5 times larger in thickness than the star's radius.

The density of the Sun's chromosphere decreases exponentially with distance from the center of the Sun by a factor of roughly 10 million, from about 2 at the chromosphere's inner boundary to under 1.6 at the outer boundary. The temperature initially decreases from the inner boundary at about 6,000 to a minimum of approximately 3,800, but then increasing to upwards of 35,000 Without special equipment, the chromosphere cannot normally be seen due to the overwhelming brightness of the photosphere. The chromosphere's spectrum is dominated by emission lines. In particular, one of its strongest lines is the Hα at a wavelength of 656.3; this line is emitted by a hydrogen atom whenever its electron makes a transition from the n=3 to the n=2 energy level. A wavelength of 656.3 is in the red part of the spectrum, which causes the chromosphere to have a characteristic reddish colour.

Many different phenomena can be observed in chromospheres.

A plage is a particularly bright region within stellar chromospheres, which are often associated with magnetic activity.

Since the first observations with the instrument SUMER on board SOHO, periodic oscillations in the solar chromosphere have been found with a frequency from 3 to 10, corresponding to a characteristic periodic time of three minutes. Oscillations of the radial component of the plasma velocity are typical of the high chromosphere. The photospheric granulation pattern usually has no oscillations above 20; however, higher frequency waves (100, or a 10 period) were detected in the solar atmosphere (at temperatures typical of the transition region and corona) by TRACE.

Plasma loops can be seen at the border of the solar disk in the chromosphere. They are different from solar prominences because they are concentric arches with maximum temperature of the order 0.1 (too low to be considered coronal features). These cool temperature loops show an intense variability: they appear and disappear in some UV lines in a time less than an hour, or they rapidly expand in 10–20 minutes. Foukal studied these cool loops in detail from the observations taken with the EUV spectrometer on Skylab in 1976. When the plasma temperature of these loops becomes coronal (above 1), these features appear more stable and evolve over longer times.

Images taken in typical chromospheric lines show the presence of brighter cells, usually referred to as the network, while the surrounding darker regions are named internetwork. They look similar to granules commonly observed on the photosphere due to the heat convection.

Chromospheres are present on almost all luminous stars other than white dwarfs. They are most prominent and magnetically active on lower main sequence stars, on brown dwarfs of F and later spectral types, and on giant and subgiant stars. A spectroscopic measure of chromospheric activity on other stars is the Mount Wilson S index.