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When energy is deposited in air, the air molecules become excited. As air is composed primarily of nitrogen and oxygen, excited N 2 and O 2 molecules are produced. These can react with other molecules, forming mainly ozone and nitrogen(II) oxide. Water vapor, when present, may also play a role; its presence is characterized by the hydrogen ...
Of the gas in the ISM, by number 91% of atoms are hydrogen and 8.9% are helium, with 0.1% being atoms of elements heavier than hydrogen or helium, [3] known as "metals" in astronomical parlance. By mass this amounts to 70% hydrogen, 28% helium, and 1.5% heavier elements.
A monochromatic sensor does not have a Bayer matrix. This means the entire sensor can be utilised to capture specific wavelengths using specialised colour filters known as narrowband filters. [4] Many nebulae are made up of hydrogen, oxygen and sulphur. These nebulae emit light in red, blue and orange wavelengths respectively. A narrowband ...
NGC 604, a giant H II region in the Triangulum Galaxy, taken by the Hubble Space Telescope. An H II region is a region of interstellar atomic hydrogen that is ionized. [1] It is typically in a molecular cloud of partially ionized gas in which star formation has recently taken place, with a size ranging from one to hundreds of light years, and density from a few to about a million particles per ...
Oxygen is hard to produce without the continuous energy that comes from sunlight, but other scientists have also encountered unexpected oxygen molecules in remote, light-deprived places.
The spectral series of hydrogen, on a logarithmic scale. The emission spectrum of atomic hydrogen has been divided into a number of spectral series, with wavelengths given by the Rydberg formula. These observed spectral lines are due to the electron making transitions between two energy levels in an atom.
The red H-alpha spectral line of the Balmer series of atomic hydrogen, which is the transition from the shell n = 3 to the shell n = 2, is one of the conspicuous colours of the universe. It contributes a bright red line to the spectra of emission or ionisation nebula, like the Orion Nebula , which are often H II regions found in star forming ...
At the same time, hydrogen may begin fusion in a shell just outside the burning helium shell. This puts the star onto the asymptotic giant branch, a second red-giant phase. [15] The helium fusion results in the build-up of a carbon–oxygen core. A star below about 8 M ☉ will never start fusion in its degenerate carbon–oxygen core. [13]