early star Comparison Table

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early star comparison table

Subject has spectral type has surface temperature has rotation velocity has optical brightness variation has light curve has observational problem has color has symbol has absorption line has ejection velocity has acronym has temperature has relative abundance has lifetime has amplitude is a kind of has name designated with has emission line has observable variation time scale has synonym has definition

A star O, B, A, and early F 10000 K white H I early star Star with spectral type A in which the spectrum of the Balmer lines of hydrogen attain their greatest strength. Helium lines can no longer be seen. Some metallic lines are present; in late A stars the H and K lines of ionized calcium appear. A0 stars have a color index of zero.

B star O, B, A, and early F 11000 to 28000 K blue-white He I early star Blue-white star of spectral type B whose spectra are characterized by absorption lines of neutral helium which reach their maximum intensity at B2. The Balmer lines of hydrogen are strong, and lines of singly ionized oxygen and other gases are also present.

central star of planetary nebula O, B, A, and early F greater than 1000 Kelvin CPN early star planerary nuclei

F star O, B, A, and early F 6000 to 7500 K yellow-white early star Star of spectral type F in which lines of hydrogen and Ca II are of about equal strength. Metal lines also become noticeable.

luminous blue variable O, B, A, and early F greater than 1000 Kelvin 0.2 magnitudes or greater some difficulty in distinguishing between various kinds early star
R, S, T, U, V, W, X, Y, or Z and the genitive of the latin constellation name
RR, RS, RT, RU, RV, RW, RX, RY, or RZ and the genitive of the latin constellation name when the single letter designations are exhausted
AA...AZ, BB...BZ, etc. (omitting J), which ends with QQ...QZ and the genitive of the latin constellation namewhen the RR...RZ designations are exhausted
V 335, V 336, etc., when the double letter designations are exhausted
within a period of decades Hubble-Sandage variable A variable-star designation for the high-luminosity early type objects.

O star O, B, A, and early F 35000 K very high blue-white He II rare 3 to 6 million years early star Very hot blue star, whose spectra is dominated by the lines of singly ionized helium (see Pickering series). (Most other lines are from at least doubly ionized elements, though H and He I lines are also present.) O stars are useful because they are found in dust clouds and virtually define the spiral arms.

peculiar star O, B, A, and early F greater than 1000 Kelvin early star Star with spectra that cannot be conveniently fitted into any of the standard spectral classifications. Denoted by a p after spectral type.

runaway star O star, B star greater than 1000 Kelvin early star Star of spectral type O or early B with unusually high space velocities. Runaway stars are thought to be produced when there is a supernova explosion in a close binary system.

white dwarf O, B, A, and early F greater than 1000 Kelvin wd early star Faint very-compact stars at the end of their life. Also used as convenient photometric and flux standards.

Wolf-Rayet O, B, A, and early F greater than 1000 Kelvin 2000 km s^-1 up to 50000 K emission line star He I, He II One of a class of very luminous, very hot (as high as 50000 K) stars whose spectra have broad emission lines (mainly He I and He II), which are presumed to originate from material ejected from the star at very high (~ 2000 km s^-1 ) velocities. Some W-R spectra show emission lines due to carbon (WC stars); others show emission lines due to nitrogen (WN stars). (Hiltner and Schild classification: WN-A, narrow lines; WN-B, broad lines.)

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Subject	has spectral type	has surface temperature	has rotation velocity	has optical brightness variation	has light curve	has observational problem	has color	has symbol	has absorption line	has ejection velocity	has acronym	has temperature	has relative abundance	has lifetime	has amplitude	is a kind of	has name designated with	has emission line	has observable variation time scale	has synonym	has definition
A star	O, B, A, and early F	10000 K					white		H I							early star					Star with spectral type A in which the spectrum of the Balmer lines of hydrogen attain their greatest strength. Helium lines can no longer be seen. Some metallic lines are present; in late A stars the H and K lines of ionized calcium appear. A0 stars have a color index of zero.
B star	O, B, A, and early F	11000 to 28000 K					blue-white		He I							early star					Blue-white star of spectral type B whose spectra are characterized by absorption lines of neutral helium which reach their maximum intensity at B2. The Balmer lines of hydrogen are strong, and lines of singly ionized oxygen and other gases are also present.
central star of planetary nebula	O, B, A, and early F	greater than 1000 Kelvin									CPN					early star				planerary nuclei
F star	O, B, A, and early F	6000 to 7500 K					yellow-white									early star					Star of spectral type F in which lines of hydrogen and Ca II are of about equal strength. Metal lines also become noticeable.
luminous blue variable	O, B, A, and early F	greater than 1000 Kelvin		0.2 magnitudes or greater		some difficulty in distinguishing between various kinds										early star	R, S, T, U, V, W, X, Y, or Z and the genitive of the latin constellation name RR, RS, RT, RU, RV, RW, RX, RY, or RZ and the genitive of the latin constellation name when the single letter designations are exhausted AA...AZ, BB...BZ, etc. (omitting J), which ends with QQ...QZ and the genitive of the latin constellation namewhen the RR...RZ designations are exhausted V 335, V 336, etc., when the double letter designations are exhausted		within a period of decades	Hubble-Sandage variable	A variable-star designation for the high-luminosity early type objects.
O star	O, B, A, and early F	35000 K	very high				blue-white		He II				rare	3 to 6 million years		early star					Very hot blue star, whose spectra is dominated by the lines of singly ionized helium (see Pickering series). (Most other lines are from at least doubly ionized elements, though H and He I lines are also present.) O stars are useful because they are found in dust clouds and virtually define the spiral arms.
peculiar star	O, B, A, and early F	greater than 1000 Kelvin														early star					Star with spectra that cannot be conveniently fitted into any of the standard spectral classifications. Denoted by a p after spectral type.
runaway star	O star, B star	greater than 1000 Kelvin														early star					Star of spectral type O or early B with unusually high space velocities. Runaway stars are thought to be produced when there is a supernova explosion in a close binary system.
white dwarf	O, B, A, and early F	greater than 1000 Kelvin						wd								early star					Faint very-compact stars at the end of their life. Also used as convenient photometric and flux standards.
Wolf-Rayet	O, B, A, and early F	greater than 1000 Kelvin								2000 km s^-1		up to 50000 K				emission line star		He I, He II			One of a class of very luminous, very hot (as high as 50000 K) stars whose spectra have broad emission lines (mainly He I and He II), which are presumed to originate from material ejected from the star at very high (~ 2000 km s^-1 ) velocities. Some W-R spectra show emission lines due to carbon (WC stars); others show emission lines due to nitrogen (WN stars). (Hiltner and Schild classification: WN-A, narrow lines; WN-B, broad lines.)