In astronomy, reflection nebulae are clouds of interstellar dust which reflect the light of a nearby star or stars. The energy from the nearby stars is insufficient to ionize the gas of the nebula to create an emission nebula, but is enough to give sufficient scattering to make the dust visible. Thus, the frequency spectrum shown by reflection nebulae is similar to that of the illuminating stars. Among the microscopic particles responsible for the scattering are carbon compounds (e. g. diamond dust) and compounds of other elements such as iron and nickel. The latter two are often aligned with the galactic magnetic field and cause the scattered light to be slightly polarized.
- Discovery 1
- Luminosity law 2
- See also 3
- References 4
Analyzing the spectrum of the nebula associated with the star Merope in the Pleiades, Vesto Slipher concluded that the source of its light is most likely the star itself, and that the nebula reflects light from the star (and that of the star Alcyone). Calculations by Ejnar Hertzsprung the following year lend credence to that hypothesis. Edwin Hubble further distinguished between the emission and reflection nebulae in 1922.
Reflection nebulae are usually blue because the scattering is more efficient for blue light than red (this is the same scattering process that gives us blue skies and red sunsets).
Reflection nebulae and emission nebulae are often seen together and are sometimes both referred to as diffuse nebulae.
Some 500 reflection nebulae are known. Among the nicest of the reflection nebulae are those surrounding the stars of the Pleiades. A blue reflection nebula can also be seen in the same area of the sky as the Trifid Nebula. The giant star Antares, which is very red (spectral class M1), is surrounded by a large, red reflection nebula.
Reflection nebulae may also be the site of star formation.
In 1922, Hubble published the result of his investigations on bright nebulae. One part of this work is the Hubble luminosity law for reflection nebulae, which makes a relationship between the angular size (R) of the nebula and the apparent magnitude (m) of the associated star:
- 5 log(R) = -m + k
where k is a constant that depends on the sensitivity of the measurement.
- Kaler, 1997.
- Slipher, Vesto M. (1922). "On the spectrum of the nebula in the Pleiades ". Lowell Observatory Bulletin 2: 26–27.
- Hertzsprung, E. (1913). "Über die Helligkeit der Plejadennebel". Astronomische Nachrichten 195: 449–452.
- Hubble, E. P. (1922). "The source of luminosity in galactic nebulae". Astrophysi cal Journal 56: 400.
- "Sifting through Dust near Orion's Belt". ESO Press Release. Retrieved 2 May 2012.
- James B. Kaler (1997). Cosmic Clouds -- Birth, Death, and Recycling in the Galaxy, Scientific American Library, Freeman, New York, 1997.