chromosphere

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Words related to chromosphere

a gaseous layer of the sun's atmosphere (extending from the photosphere to the corona) that is visible during a total eclipse of the sun

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Energy losses (in erg [cm.sup.-2][s.sup.-1]) from the chromosphere and the corona (12) Region Quiet Sun Coronal hole Coronal temperature [K] 1.1-1.6 x [10.sup.6] [10.sup.6] Coronal energy loss 3 x [10.sup.5] 8 x [10.sup.5] Chromospheric energy 4 x [10.sup.6] 4 x [10.sup.6] loss Region Active region Coronal temperature [K] 2.5 x [10.sup.6] Coronal energy loss [10.sup.7] Chromospheric energy 2 x [10.sup.7] loss
These authors have presented MHD numerical simulations of solar X-ray jets based on magnetic reconnection model that includes chromospheric evaporation.
In the LMHSM, the presence of condensed matter and elevated chromospheric densities, well-beyond the densities of the Earth's atmosphere, are entirely compatible with a condensed solar photosphere.
If we discard this result that involves a chromospheric line, it can be concluded that without any exception, in the photosphere the observed vertical gradient is on the order of 3-4 G/km.
The scientists suggested that the gas movement is caused by a process of "chromospheric evaporation" in which "impulsive heating" on a small scale can result in the heating of the solar active regions but on a larger scale can lead to huge explosions, such as solar flares or coronal mass ejections.
As this binary has a spectral classification of G4V I suggest the dip in the light curve is due to chromospheric activity.
Segmenting Chromospheric Images with Markov Random Fields.
Starting at roughly 6,000 kelvins at the sun's surface, the solar atmosphere's temperature falls to nearly 4,300 kelvins at an altitude of 500 kilometers before rising to typical chromospheric temperatures.
2001) is the ratio of measurements from the core of the h and k Mg II emission lines (5) at 280 nm to measurements in the nearby wings (278 and 282 nm), and variability in the Mg II index is attributed to chromospheric extensions of the photospheric faculae.
Its bandpass covers some of the brightest spectral lines of iron ions emitted by the solar corona, Fe IX-XI, with maximum excitation temperatures (lg [T.sub.max] = 5.9 to 6.1) [6], and contains a small number of chromospheric and photospheric lines.
we assumed that the distribution in the continuous chromospheric spectrum is the same as that of a black body at 5700[degrees], and that the continuous spectrum from the extreme edge is that of a black body at 4700[degrees].
RS CVn type stars show optical variability (outside eclipses) which is characterised by an amplitude up to 0.6 mag in the V band and interpreted as the rotationally modulated effect of cool spots on their surfaces, a result of increased chromospheric activity.
Among the topics are gravitational wave foreground radiation from neutron star-dwarf binaries, the chromospheric activity of late-type stars of the different rotational periods, spectrophotometry and model atmosphere flux fitting, the light-time effect and tertiary companions in close binary stars, the age of the local interstellar bubble, and the current status and outreach activities of radio astronomy in Malaysia.