Strömgren Sphere
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High Quality Content by WIKIPEDIA articles! In theoretical astrophysics, a Strömgren sphere is the sphere of ionized hydrogen (H II) around a young star of the spectral classes O or B. Its counterpart in the real world are the H II-regions, a type of an emission nebula, the most prominent of which is the Rosette Nebula. It was derived by Bengt Strömgren in 1937 and later named after him. Very hot stars, those of the spectral classes O or B, emit very energetic radiation, especially ultraviolet radiation, which is able to ionize the neutral hydrogen (H I) of the surrounding interstellar medium…mehr

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High Quality Content by WIKIPEDIA articles! In theoretical astrophysics, a Strömgren sphere is the sphere of ionized hydrogen (H II) around a young star of the spectral classes O or B. Its counterpart in the real world are the H II-regions, a type of an emission nebula, the most prominent of which is the Rosette Nebula. It was derived by Bengt Strömgren in 1937 and later named after him. Very hot stars, those of the spectral classes O or B, emit very energetic radiation, especially ultraviolet radiation, which is able to ionize the neutral hydrogen (H I) of the surrounding interstellar medium (ISM), i.e. the hydrogen atom loses its single electron. This state of hydrogen is called H II. After a while free electrons recombine with hydrogen ions.