We describe our calculations of the cohesive property of matter in strong magnetic fields, and discuss the implications of our results to the recent observations of neutron star surface emission as well as to the detection/non-detection of radio emission from magnetars.
Such stars are rich in carbon, and it is believed that the fall in brightness is due to the star's emission of carbon, which then condenses to a dense cloud near the star, rather than to a change in luminosity of the star itself.
With the exception of some planetary nebulae, there is no green object in the deep-sky: there are no green stars and emission nebulae are deeply red, whilst reflection nebulae are blue; so if there are green pixels on a color balanced, deep-sky astrophoto, they will be noise; consequently such kind of noise can be removed easily and very efficiently.
The astronomers used the 3.6-meter Canada-France-Hawaii Telescope on Mauna Kea, Hawaii, to study five sunlike stars for emissions from excited calcium ions--a good measure of activity in a layer of hot gas just above the visible surface.
The implications of these observations for models of magnetic activity in late-type stars, of wind emission in early-type stars, and of X-ray production in the early stages of stellar evolution are briefly discussed.
A star's energy emission as a function of wavelength is influenced by both its temperature and composition.
Contrary to expectations, the γ-rays from a distant cluster of stars are dominated by emission from a single neutron star.
MXB 0656-072 is an accreting X-ray pulsar with a Be star companion, showing notable emission in Hα.
(2013) predicted that exoplanets orbiting F, G, K and M stars would produce a visible ozone spectral signature, with the strength of the signature varying depending on the star's UV radiation emission as well as the planet's molecular oxygen content.
Srinivasan et al. (2010) has determined the composition of the dust shell of a typical, albeit only one, C-rich AGB star, without the MgS emission feature at 30 μm, and finds that about 12% (in a range of 10 16%) of the dust by mass is contained in SiC, and that the remainder is in the form of amorphous carbon.
