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O Type Star biography, O Type Star discography
Oe stars have prominent hydrogen emission lines.The spectra of Of stars are usually variable, and the intensities of their emission lines vary in an irregular way.Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer.Jerry Bonnell
(USRA)
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NASA Official: Jay Norris.Stars can be classified by their surface temperatures as determined from Wien's Displacement Law, but this poses practical difficulties for distant stars.Spectral Class Characteristics
Data from J.The thermal energy is so great at these temperatures that most surface hydrogen is completely ionized so hydrogen (HI) lines are weak.Unionized helium (HeI) is visible but the stronger spectra are of mulitple ionized atoms (HeII, CIII, NIII,OIII,SiV).The radiation rises in intensity toward the blue end of the spectrum.The blackbody peak will be in the ultraviolet.Type stars shows the presence of hydrogen and helium.The radiation from O5 stars is so intense that it can ionize hydrogen over a volume of space 1000 light years across.They light the stellar nurseries with ultraviolet light and cause the clouds to glow in some of the dramatic nebulae associated with the H II regions.HeI) lines are strongest at B2.The neutral hydrogen (HI) lines are getting stronger and singly ionized OII, SiII and Mg II are visible.Most other lines are from at least doubly ionized elements, though H and He I lines are also present.Runaway star which diverges from a comparatively small area in Orion.One of the three stars in Orion's belt, and the star along whose line of sight interstellar gas was first spectroscopically detected.III and 4686 from He II are present.Its spectrum can be interpreted to mean that each component has a mass of 75 Msun.Subdwarf O star showing few very broad and shallow Balmer lines and a very strong He II 4686 line.It is well known for its strong interstellar absorption lines in the visible part of the spectrum.Click here for more information on site membership.The Sun is a as a G2V type star, a yellow dwarf and a main sequence star.The core contracts as the outer layers expand.These stars will eventually explode (becoming a planetary nebula or supernova, depending on their mass) and then become white dwarfs, neutron stars, or black holes (again depending on their mass).Smaller stars (like our Sun) eventually become faint white dwarfs (hot, white, dim stars) that are below the main sequence.Neutral helium lines (H II) in absorption.Hydrogen (H) lines strongest for A0 stars, decreasing for other A's.Absorption lines of neutral metallic atoms and ions (e.Some molecular bands of titanium oxide.The Yerkes Luminosity Classes: (by William Wilson Morgan and Philip Keenan)
TYPEStar
IaVery luminous supergiants
IbLess luminous supergiants
IILuminous giants
IIIGiants
IVSubgiants
VMain sequence stars (dwarf stars)
VISubdwarf
VIIWhite Dwarf
Luminosity is the total brightness of a star (or galaxy).Luminosity is the total amount of energy that a star radiates each second (including all wavelengths of electromagnetic radiation).For these stars, the hotter they are, the brighter they are.The sun is a typical Main Sequence star.Dwarf stars are relatively small stars, up to 20 times larger than our sun and up to 20,000 times brighter.Our sun is a dwarf star.YELLOW DWARF
Yellow dwarfs are small, main sequence stars.RED DWARF
A red dwarf is a small, cool, very faint, main sequence star whose surface temperature is under about 4,000 K.Proxima Centauri is a red dwarf.Old, Large Stars
RED GIANT
A red giant is a relatively old star whose diameter is about 100 times bigger than it was originally, and had become cooler (the surface temperature is under 6,500 K).Betelgeuse is a red giant.BLUE GIANTA blue giant is a huge, very hot, blue star.Betelgeuse and Rigel are supergiants.Faint, Virtually Dead Stars:
WHITE DWARFA white dwarf is a small, very dense, hot star that is made mostly of carbon.These faint stars are what remains after a red giant star loses its outer layers.Their nuclear cores are depleted.They are about the size of the Earth (but tremendously heavier)!They will eventually lose their heat and become a cold, dark black dwarf.Our sun will someday turn into a white dwarf and then a black dwarf.The companion of Sirius is a white dwarf.BROWN DWARF
A brown dwarf is a "star" whose mass is too small to have nuclear fusion occur at its core (the temperature and pressure at its core are insufficient for fusion).PULSAR
A pulsar is a rapidly spinning neutron star that emits energy in pulses.Binary Stars:
DOUBLE STAR
A double star is two stars that appear close to one another in the sky.BINARY STAR
A binary star is a system of two stars that rotate around a common center of mass (the barycenter).ECLIPSING BINARY
An eclipsing binary is two close stars that appear to be a single star varying in brightness.The variation in brightness is due to the stars periodically obscuring or enhancing one another.This binary star system is tilted (with respect ot us) so that its orbital plane is viewed from its edge.Stars that Vary in Luminosity:
CEPHEID VARIABLE STARS
Cepheid variables are stars that regularly pulsate in size and change in brightness.As the star increases in size, its brightness decreases; then, the reverse occurs.Cepheid Variables may not be permanently variable; the fluctuations may just be an unstable phase the star is going through.Mira variables were named after the star Mira, whose variations were discovered in 1596.History
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