eclipsing binary 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

Next close binary: nova Up: close binary, periodic variable

eclipsing binary comparison table

Subject has energy release has spectral type is part of has surface temperature become has acceptance statu has orbital period has frequency is an instance of has velocity has eccentricity has color has erruption date has distance has absorption line has ejection velocity has acronym has temperature has primary star has prototype has recovery time has primary has period has secondary star has orbital eccentricity has eclipse duration has outburst start time has wavelength is a kind of has peak brightness has apparent magnitude has material has mass has use has synonym has definition has discovery date has luminosity class obey

AS Eri greater than 1000 Kelvin eclipsing binary determined from proper motion and radial velocity hydrogen, helium greater than 0.08 the sun's mass An eclipsing binary whose secondary is close to its Roche limit.

beta Lyrae star greater than 1000 Kelvin determined from proper motion and radial velocity eclipsing binary hydrogen, helium greater than 0.08 the sun's mass A class of eclipsing binary whose secondary minima are intermediate between those of Algol and those of W UMa. The prototype beta Lyr (B8.5 II, F V) is a complex eclipsing system and is presently in a state of rapid mass transfer. The spectrum of one companion is invisible; it may be a black hole. Beta Lyrae is also a weak radio source.

beta Persei star greater than 1000 Kelvin determined from proper motion and radial velocity Algol eclipsing binary hydrogen, helium greater than 0.08 the sun's mass A class of eclipsing binary (see Algol) with periods of from 2 to 5 days, the depth of whose secondary minimum is almost negligible.

BM Orionis Orion greater than 1000 Kelvin eclipsing binary determined from proper motion and radial velocity hydrogen, helium greater than 0.08 the sun's mass A peculiar eclipsing binary (B2-B3) in the Trapezium, with a flat-bottomed light curve suggesting a total eclipse. The spectrum of the secondary has never been seen.

Centaurus X-3 dark halo greater than 1000 Kelvin hypothetical 2.087 days inversely proportional to the wavelength eclipsing binary determined from proper motion and radial velocity 5-10 kpc PSR 4.8 s e < 0.002 0.488 days in X-ray inversely proportional to its momentum hydrogen, helium greater than 0.08 the sun's mass Krzeminski's star A pulsating binary X-ray source in the galactic plane. Optical component is Krzeminski's star, a B0 giant or supergiant. The X-ray component is probably a rotating neutron star of about 0.65-0.83 M_sun. Cen X-3 is speeding up at a rate of about 1 part in 10³-10⁵ per year and will at this rate fall into its companion in about 1000 years. uncertainty principle

CV Serpentis O, B, A, and early F Serpens greater than 1000 Kelvin 29.6 days eclipsing binary determined from proper motion and radial velocity 2000 km s^-1 up to 50000 K hydrogen, helium greater than 0.08 the sun's mass A sometimes-eclipsing binary composed of a Wolf-Rayet star and a B0 star.

DQ Herculis 10⁴⁴ ergs greater than 1000 Kelvin naked eye star 4^h39^m eclipsing binary determined from proper motion and radial velocity 1934 CV white dwarf M dwarf hydrogen, helium greater than 0.08 the sun's mass nova peak brightness distance determination Nova Herculis 1934 A slow nova which also happens to be an eclipsing binary. It also has a regular flickering period of 71 seconds, the shortest period of regular variations known, except for pulsars and compact X-ray objects. It is probably composed of an M dwarf and a white dwarf with an accretion disk.

epsilon Aurigae O, B, A, and early F Auriga 10000 K 27 years eclipsing binary determined from proper motion and radial velocity white 1 kpc H I A8 Ia hydrogen, helium greater than 0.08 the sun's mass An eclipsing binary with an invisible supergiant companion. The primary is an extremely luminous A8 Ia supergiant of 30 M_sun in a post-main-sequence stage of evolution; the secondary may be a collapsed star or black hole. It has at least six components.

Hercules X-1 dark halo greater than 1000 Kelvin hypothetical 1.7 days inversely proportional to the wavelength eclipsing binary determined from proper motion and radial velocity e < 0.1 5 kpc PSR 0.24 days (in X-rays) inversely proportional to its momentum hydrogen, helium greater than 0.08 the sun's mass 3U 1653+35 An X-ray pulsar, a member of an occulting binary system. The visible component has been identified as the blue variable HZ Herculis, whose spectrum varies from late A or early F to B. Her X- l has a pulsation period of 1.2378 seconds, presumably its rotation period, and exhibits a 35-day quasi-periodicity in the X-ray region (but not in the optical). It is probably a rotating neutron star in a circular orbit with a mass of about 0.7 M_sun, which is accreting matter from HZ Her. The orbital period is stable, but the pulsation period is speeding up at a rate of about 1 part in 10⁵ per year. The X-ray eclipse lasts 0.24 days. uncertainty principle

S Doradus Dorado greater than 1000 Kelvin 40 years eclipsing binary determined from proper motion and radial velocity hydrogen, helium greater than 0.08 the sun's mass A supergiant eclipsing binary (an Eta Carinae-type object) in the Large Magellanic Cloud.

Scorpius X-1 celestial sphere greater than 1000 Kelvin eclipsing binary 250 to 500 pc X-ray brightest X-ray source in the sky (besides the Sun) A compact eclipsing X-ray source. It has day-to-day variations (period about 0.78 days?) of as much as 1 mag; it also has optical and radio counterparts but no correlation has been found among the flares observed at the three different wavelengths. It is a thermal X-ray source, probably associated with a rotating collapsed star surrounded by an extensive envelope. Tentative optical identification with the 13th mag blue variable V818 Sco. The spectrum of Sco X-1 is similar to that of an old nova. (3U 1617-15) 1962

Vela X-1 B0.5 Ib celestial sphere 11000 to 28000 K 8.96 days single line spectroscopic binary determined from proper motion and radial velocity blue-white He I X-ray 7 hydrogen, helium of unseen companion 1.7 to 15 M_sun, with a probable value of about 2.6 M_sun. 3U 0900-40 I

VV Cephei star greater than 1000 Kelvin determined from proper motion and radial velocity eclipsing binary hydrogen, helium greater than 0.08 the sun's mass Eclipsing binaries with M supergiant primaries and blue (usually B) supergiant or giant secondaries. They have a rich emission spectrum. Sandage (1974) suggests M_v = - 7.3 for the M2p component of VV Cep.

W Ursae Majoris star greater than 1000 Kelvin determined from proper motion and radial velocity eclipsing binary hydrogen, helium greater than 0.08 the sun's mass A large class of double-lined eclipsing binaries with very short periods (a few hours) whose spectra indicate mass transfer. They are distinguished by the fact that their primary and secondary minima are equal. They are all F or G binaries on or near the main sequence. They may be the progenitors of dwarf novae.

Next close binary: nova Up: close binary, periodic variable

Subject	has energy release	has spectral type	is part of	has surface temperature	become	has acceptance statu	has orbital period	has frequency	is an instance of	has velocity	has eccentricity	has color	has erruption date	has distance	has absorption line	has ejection velocity	has acronym	has temperature	has primary star	has prototype	has recovery time	has primary	has period	has secondary star	has orbital eccentricity	has eclipse duration	has outburst start time	has wavelength	is a kind of	has peak brightness	has apparent magnitude	has material	has mass	has use	has synonym	has definition	has discovery date	has luminosity class	obey
AS Eri				greater than 1000 Kelvin					eclipsing binary	determined from proper motion and radial velocity																						hydrogen, helium	greater than 0.08 the sun's mass			An eclipsing binary whose secondary is close to its Roche limit.
beta Lyrae star				greater than 1000 Kelvin						determined from proper motion and radial velocity																			eclipsing binary			hydrogen, helium	greater than 0.08 the sun's mass			A class of eclipsing binary whose secondary minima are intermediate between those of Algol and those of W UMa. The prototype beta Lyr (B8.5 II, F V) is a complex eclipsing system and is presently in a state of rapid mass transfer. The spectrum of one companion is invisible; it may be a black hole. Beta Lyrae is also a weak radio source.
beta Persei star				greater than 1000 Kelvin						determined from proper motion and radial velocity										Algol									eclipsing binary			hydrogen, helium	greater than 0.08 the sun's mass			A class of eclipsing binary (see Algol) with periods of from 2 to 5 days, the depth of whose secondary minimum is almost negligible.
BM Orionis			Orion	greater than 1000 Kelvin					eclipsing binary	determined from proper motion and radial velocity																						hydrogen, helium	greater than 0.08 the sun's mass			A peculiar eclipsing binary (B2-B3) in the Trapezium, with a flat-bottomed light curve suggesting a total eclipse. The spectrum of the secondary has never been seen.
Centaurus X-3			dark halo	greater than 1000 Kelvin		hypothetical	2.087 days	inversely proportional to the wavelength	eclipsing binary	determined from proper motion and radial velocity				5-10 kpc			PSR						4.8 s		e < 0.002	0.488 days in X-ray		inversely proportional to its momentum				hydrogen, helium	greater than 0.08 the sun's mass		Krzeminski's star	A pulsating binary X-ray source in the galactic plane. Optical component is Krzeminski's star, a B0 giant or supergiant. The X-ray component is probably a rotating neutron star of about 0.65-0.83 M_sun. Cen X-3 is speeding up at a rate of about 1 part in 10³-10⁵ per year and will at this rate fall into its companion in about 1000 years.			uncertainty principle
CV Serpentis		O, B, A, and early F	Serpens	greater than 1000 Kelvin			29.6 days		eclipsing binary	determined from proper motion and radial velocity						2000 km s^-1		up to 50000 K														hydrogen, helium	greater than 0.08 the sun's mass			A sometimes-eclipsing binary composed of a Wolf-Rayet star and a B0 star.
DQ Herculis	10⁴⁴ ergs			greater than 1000 Kelvin	naked eye star		4^h39^m		eclipsing binary	determined from proper motion and radial velocity			1934				CV		white dwarf					M dwarf								hydrogen, helium	greater than 0.08 the sun's mass	nova peak brightness distance determination	Nova Herculis 1934	A slow nova which also happens to be an eclipsing binary. It also has a regular flickering period of 71 seconds, the shortest period of regular variations known, except for pulsars and compact X-ray objects. It is probably composed of an M dwarf and a white dwarf with an accretion disk.
epsilon Aurigae		O, B, A, and early F	Auriga	10000 K			27 years		eclipsing binary	determined from proper motion and radial velocity		white		1 kpc	H I							A8 Ia										hydrogen, helium	greater than 0.08 the sun's mass			An eclipsing binary with an invisible supergiant companion. The primary is an extremely luminous A8 Ia supergiant of 30 M_sun in a post-main-sequence stage of evolution; the secondary may be a collapsed star or black hole. It has at least six components.
Hercules X-1			dark halo	greater than 1000 Kelvin		hypothetical	1.7 days	inversely proportional to the wavelength	eclipsing binary	determined from proper motion and radial velocity	e < 0.1			5 kpc			PSR									0.24 days (in X-rays)		inversely proportional to its momentum				hydrogen, helium	greater than 0.08 the sun's mass		3U 1653+35	An X-ray pulsar, a member of an occulting binary system. The visible component has been identified as the blue variable HZ Herculis, whose spectrum varies from late A or early F to B. Her X- l has a pulsation period of 1.2378 seconds, presumably its rotation period, and exhibits a 35-day quasi-periodicity in the X-ray region (but not in the optical). It is probably a rotating neutron star in a circular orbit with a mass of about 0.7 M_sun, which is accreting matter from HZ Her. The orbital period is stable, but the pulsation period is speeding up at a rate of about 1 part in 10⁵ per year. The X-ray eclipse lasts 0.24 days.			uncertainty principle
S Doradus			Dorado	greater than 1000 Kelvin			40 years		eclipsing binary	determined from proper motion and radial velocity																						hydrogen, helium	greater than 0.08 the sun's mass			A supergiant eclipsing binary (an Eta Carinae-type object) in the Large Magellanic Cloud.
Scorpius X-1			celestial sphere	greater than 1000 Kelvin					eclipsing binary					250 to 500 pc														X-ray			brightest X-ray source in the sky (besides the Sun)					A compact eclipsing X-ray source. It has day-to-day variations (period about 0.78 days?) of as much as 1 mag; it also has optical and radio counterparts but no correlation has been found among the flares observed at the three different wavelengths. It is a thermal X-ray source, probably associated with a rotating collapsed star surrounded by an extensive envelope. Tentative optical identification with the 13th mag blue variable V818 Sco. The spectrum of Sco X-1 is similar to that of an old nova. (3U 1617-15)	1962
Vela X-1		B0.5 Ib	celestial sphere	11000 to 28000 K			8.96 days		single line spectroscopic binary	determined from proper motion and radial velocity		blue-white			He I													X-ray			7	hydrogen, helium	of unseen companion 1.7 to 15 M_sun, with a probable value of about 2.6 M_sun.		3U 0900-40			I
VV Cephei star				greater than 1000 Kelvin						determined from proper motion and radial velocity																			eclipsing binary			hydrogen, helium	greater than 0.08 the sun's mass			Eclipsing binaries with M supergiant primaries and blue (usually B) supergiant or giant secondaries. They have a rich emission spectrum. Sandage (1974) suggests M_v = - 7.3 for the M2p component of VV Cep.
W Ursae Majoris star				greater than 1000 Kelvin						determined from proper motion and radial velocity																			eclipsing binary			hydrogen, helium	greater than 0.08 the sun's mass			A large class of double-lined eclipsing binaries with very short periods (a few hours) whose spectra indicate mass transfer. They are distinguished by the fact that their primary and secondary minima are equal. They are all F or G binaries on or near the main sequence. They may be the progenitors of dwarf novae.