Search results
Results From The WOW.Com Content Network
Interstellar reddening is a phenomenon associated with interstellar extinction where the spectrum of electromagnetic radiation from a radiation source changes characteristics from that which the object originally emitted. Reddening occurs due to the light scattering off dust and other matter in the interstellar medium.
Download QR code; Print/export Download as PDF; Printable version; In other projects ... provided that the interstellar reddening of the star is either negligible or ...
interstellar reddening An effect produced by the incremental absorption and scattering of electromagnetic energy from interstellar matter, known as extinction. This effect causes more distant objects such as stars to appear redder and dimmer than expected. It is not to be confused with the separate phenomenon of redshift. invariable plane
An eagle-eyed TikToker found a clue in sci-fi epic Interstellar that changes the meaning of the entire movie.. Directed by Oscar-winner Christopher Nolan, the movie explores themes as diverse as ...
1P21 photomultiplier tube. The UBV photometric system (from Ultraviolet, Blue, Visual), also called the Johnson system (or Johnson-Morgan system), is a photometric system usually employed for classifying stars according to their colors.
In interstellar astronomy, visible spectra can appear redder due to scattering processes in a phenomenon referred to as interstellar reddening [50] —similarly Rayleigh scattering causes the atmospheric reddening of the Sun seen in the sunrise or sunset and causes the rest of the sky to have a blue color.
The Strömgren photometric system, abbreviated also as uvbyβ or simply uvby, and sometimes referred as Strömgren - Crawford photometric system, is a four-colour medium-passband photometric system plus Hβ (H-beta) filters for determining magnitudes and obtaining spectral classification of stars.
The binary HD 300933/4 is a probable VV Cephei-type star [11] with a composite spectrum similar to that of V381 Cephei (HR 8164), but with weaker emission lines of Fe II, S II, and Ni II [4] (the "II" indicates that the elements are in their singly ionized state in spectroscopic notation [12]).