CV Serpentis Comparison Table

Astronomy View all facts Glossary Help

physical object > natural object > celestial body > collection of stars > star system > binary star > close binary > eclipsing binary > CV Serpentis

Next eclipsing binary: DQ Herculis Up: eclipsing binary, Wolf-Rayet Previous eclipsing binary: Centaurus X-3

CV Serpentis comparison table

Subject has spectral type is part of is an instance of has optical brightness variation has observational problem has ejection velocity has temperature has abundance is a kind of has name designated with has emission line has observable variation time scale has definition has number of star

eclipsing binary 0.2 magnitudes or greater some difficulty in distinguishing between various kinds half the stars in the solar neighborhood are members of star systems close binary
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 Eclipsing variables whose orbital plane lies so nearly in the line of sight that eclipses, as seen from the Earth, can occur and can be detected from their light curves. 2

Wolf-Rayet O, B, A, and early F 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.)

CV Serpentis O, B, A, and early F Serpens eclipsing binary 0.2 magnitudes or greater some difficulty in distinguishing between various kinds 2000 km s^-1 up to 50000 K half the stars in the solar neighborhood are members of star systems
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
He I, He II within a period of decades A sometimes-eclipsing binary composed of a Wolf-Rayet star and a B0 star. 2

Subject	has spectral type	is part of	is an instance of	has optical brightness variation	has observational problem	has ejection velocity	has temperature	has abundance	is a kind of	has name designated with	has emission line	has observable variation time scale	has definition	has number of star
eclipsing binary				0.2 magnitudes or greater	some difficulty in distinguishing between various kinds			half the stars in the solar neighborhood are members of star systems	close binary	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	Eclipsing variables whose orbital plane lies so nearly in the line of sight that eclipses, as seen from the Earth, can occur and can be detected from their light curves.	2
Wolf-Rayet	O, B, A, and early F					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.)
CV Serpentis	O, B, A, and early F	Serpens	eclipsing binary	0.2 magnitudes or greater	some difficulty in distinguishing between various kinds	2000 km s^-1	up to 50000 K	half the stars in the solar neighborhood are members of star systems		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	He I, He II	within a period of decades	A sometimes-eclipsing binary composed of a Wolf-Rayet star and a B0 star.	2

Next eclipsing binary: DQ Herculis Up: eclipsing binary, Wolf-Rayet Previous eclipsing binary: Centaurus X-3