Английская Википедия:Chromosphere
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 Шаблон:Convert 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 Шаблон:Convert 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.[1] 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).[2]
Chromospheres have also been observed on stars other than the Sun.[3] 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.[4]
Physical properties
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 Шаблон:Val at the chromosphere's inner boundary to under Шаблон:Val at the outer boundary.[5] The temperature initially decreases from the inner boundary at about Шаблон:Val[6] to a minimum of approximately Шаблон:Val,[7] but then increasing to upwards of Шаблон:Val[6] at the outer boundary with the transition layer of the corona (see Шаблон:Slink).
The density of the chromosphere is 10−4 times that of the underlying photosphere and 10−8 times that of the Earth's atmosphere at sea level. This makes the chromosphere normally invisible and it can be seen only during a total eclipse, where its reddish colour is revealed. The colour hues are anywhere between pink and red.[8] 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.Шаблон:Cn In particular, one of its strongest lines is the Hα at a wavelength of Шаблон:Val; 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 Шаблон:Val is in the red part of the spectrum, which causes the chromosphere to have a characteristic reddish colour.
Phenomena
Many different phenomena can be observed in chromospheres.
Plage
Шаблон:Main A plage is a particularly bright region within stellar chromospheres, which are often associated with magnetic activity.[9]
Spicules
Шаблон:Main The most commonly identified feature in the solar chromosphere are spicules. Spicules rise to the top of the chromosphere and then sink back down again over the course of about 10 minutes.[10]
Oscillations
Since the first observations with the instrument SUMER on board SOHO, periodic oscillations in the solar chromosphere have been found with a frequency from Шаблон:Val to Шаблон:Val, corresponding to a characteristic periodic time of three minutes.[11] Oscillations of the radial component of the plasma velocity are typical of the high chromosphere. The photospheric granulation pattern usually has no oscillations above Шаблон:Val; however, higher frequency waves (Шаблон:Val, or a Шаблон:Val period) were detected in the solar atmosphere (at temperatures typical of the transition region and corona) by TRACE.[12]
Loops
Шаблон:See also 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 Шаблон:Val (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[13] 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 Шаблон:Val), these features appear more stable and evolve over longer times.
Network
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.
On other stars
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.[9]
A spectroscopic measure of chromospheric activity on other stars is the Mount Wilson S-index.[14][15]
See also
References
External links
- Animated explanation of the Chromosphere (and Transition Region) Шаблон:Webarchive (University of South Wales).
Шаблон:The Sun Шаблон:Star Шаблон:Portal bar Шаблон:Authority control
- ↑ Шаблон:Cite journal
- ↑ [1] Шаблон:PD-notice
- ↑ Шаблон:Cite web
- ↑ Шаблон:Cite web
- ↑ Шаблон:Citation
- ↑ 6,0 6,1 Шаблон:Cite web
- ↑ Шаблон:Citation
- ↑ Шаблон:Cite book
- ↑ 9,0 9,1 Шаблон:Cite journal
- ↑ Шаблон:Cite book
- ↑ Шаблон:Cite journal
- ↑ Шаблон:Cite journal
- ↑ Шаблон:Cite journal
- ↑ Шаблон:Cite journal
- ↑ A small survey of the magnetic fields of planet-hosting stars (Шаблон:Webarchive) gives "Wright J. T., Marcy G. W., Butler R. P., Vogt S. S., 2004, ApJS, 152, 261" as a ref for s-index.
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