late star Comparison Table

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late star comparison table

Subject has surface temperature has optical brightness variation has metallic line strength has observational problem has color is a kind of has name designated with has observable variation time scale has synonym has definition has luminosity class

carbon star greater than 1000 Kelvin late star In the HD system, a rather loose category of peculiar red-giant star, usually of spectral types R and N, whose spectra show strong bands of C₂, CN, or other carbon compounds and unusually high abundances of lithium. Carbon stars resemble S stars in the relative proportion of heavy and light metals, but they contain so much carbon that these bands dominate their spectra. (C2,0. The number following the comma is an abundance parameter.)

CN-strong star greater than 1000 Kelvin giant Late type giant with strong CN bands. Metallic lines are also stronger than in normal giants. III

G star 5000 to 6000 K yellowish late star Yellowish star in which the H and K lines of Ca II have become dominant and in which a tremendous profusion of spectral lines of both neutral and ionized metals, particularly iron, begins to show. The Balmer lines of hydrogen are still recognizable. Examples are the Sun and Capella.

H and K emission line star greater than 1000 Kelvin emission line star Late objects (F4 to M), which exhibit emission features in their Ca II HK lines.

K star 3600 to 5000 K orange to red late star Cool star with spectral type K with spectra resembling those of sunspots, in which the hydrogen lines have been greatly weakened. The HK lines (q.v.) reach their greatest intensity. Strongest lines are Ca I (4227 Å) and the G-band (4303 Å).

M star greater than 1000 Kelvin late star Having a spectral type of M, that is, red like Betelgeuse and Antares.

S star greater than 1000 Kelvin heavy-metal star Late type giant (K5 to M) showing distinct bands of ZrO. III

semiregular variable greater than 1000 Kelvin 0.2 magnitudes or greater some difficulty in distinguishing between various kinds late 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 A class of giant and supergiant pulsating stars of spectral class M, K, N, R, or S with a periodic (or semiperiodic) light curve of varying amplitude.

T Tauri star greater than 1000 Kelvin 0.2 magnitudes or greater some difficulty in distinguishing between various kinds emission line 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 nebular variable Also called T Tauri variable, a type of variable star of spectral classification F, G or K (giants above the main sequence on the Hertzsprung-Russell diagram) that loses an appreciable proportion of its mass in its (irregular) more luminous periods, and is thus surrounded by volumes of gas and dust.

weak line star greater than 1000 Kelvin small late star Late stars in which the lines of all metals are weakened when compared with normal stars of the same temperature. Also called metal-weak stars.

Subject	has surface temperature	has optical brightness variation	has metallic line strength	has observational problem	has color	is a kind of	has name designated with	has observable variation time scale	has synonym	has definition	has luminosity class
carbon star	greater than 1000 Kelvin					late star				In the HD system, a rather loose category of peculiar red-giant star, usually of spectral types R and N, whose spectra show strong bands of C₂, CN, or other carbon compounds and unusually high abundances of lithium. Carbon stars resemble S stars in the relative proportion of heavy and light metals, but they contain so much carbon that these bands dominate their spectra. (C2,0. The number following the comma is an abundance parameter.)
CN-strong star	greater than 1000 Kelvin					giant				Late type giant with strong CN bands. Metallic lines are also stronger than in normal giants.	III
G star	5000 to 6000 K				yellowish	late star				Yellowish star in which the H and K lines of Ca II have become dominant and in which a tremendous profusion of spectral lines of both neutral and ionized metals, particularly iron, begins to show. The Balmer lines of hydrogen are still recognizable. Examples are the Sun and Capella.
H and K emission line star	greater than 1000 Kelvin					emission line star				Late objects (F4 to M), which exhibit emission features in their Ca II HK lines.
K star	3600 to 5000 K				orange to red	late star				Cool star with spectral type K with spectra resembling those of sunspots, in which the hydrogen lines have been greatly weakened. The HK lines (q.v.) reach their greatest intensity. Strongest lines are Ca I (4227 Å) and the G-band (4303 Å).
M star	greater than 1000 Kelvin					late star				Having a spectral type of M, that is, red like Betelgeuse and Antares.
S star	greater than 1000 Kelvin					heavy-metal star				Late type giant (K5 to M) showing distinct bands of ZrO.	III
semiregular variable	greater than 1000 Kelvin	0.2 magnitudes or greater		some difficulty in distinguishing between various kinds		late 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		A class of giant and supergiant pulsating stars of spectral class M, K, N, R, or S with a periodic (or semiperiodic) light curve of varying amplitude.
T Tauri star	greater than 1000 Kelvin	0.2 magnitudes or greater		some difficulty in distinguishing between various kinds		emission line 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	nebular variable	Also called T Tauri variable, a type of variable star of spectral classification F, G or K (giants above the main sequence on the Hertzsprung-Russell diagram) that loses an appreciable proportion of its mass in its (irregular) more luminous periods, and is thus surrounded by volumes of gas and dust.
weak line star	greater than 1000 Kelvin		small			late star				Late stars in which the lines of all metals are weakened when compared with normal stars of the same temperature. Also called metal-weak stars.

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