Centaurus X-3 Comparison Table

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physical object > natural object > celestial body > collection of stars > star system > binary star > close binary > eclipsing binary > Centaurus X-3

Next eclipsing binary: CV Serpentis Up: eclipsing binary, X-ray pulsar Previous eclipsing binary: BM Orionis

Centaurus X-3 comparison table

Subject is part of has acceptance statu is an instance of has frequency has optical brightness variation has observational problem has distance has acronym has abundance has orbital eccentricity has wavelength is a kind of has name designated with has observable variation time scale has synonym has definition obey 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

X-ray pulsar dark halo hypothetical inversely proportional to the wavelength PSR inversely proportional to its momentum pulsar hidden mass Pulsar (q.v.) that radiates in the X-ray region of the spectrum. Best verified examples are Her X-1 and Cen X-3. They are thought to be rotating, strongly magnetic neutron stars of about 1 M_sun in a grazing orbit around a more massive star from which they are accreting matter. uncertainty principle

Centaurus X-3 dark halo hypothetical eclipsing binary inversely proportional to the wavelength 0.2 magnitudes or greater some difficulty in distinguishing between various kinds 5-10 kpc PSR half the stars in the solar neighborhood are members of star systems e < 0.002 inversely proportional to its momentum
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 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 2

Subject	is part of	has acceptance statu	is an instance of	has frequency	has optical brightness variation	has observational problem	has distance	has acronym	has abundance	has orbital eccentricity	has wavelength	is a kind of	has name designated with	has observable variation time scale	has synonym	has definition	obey	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
X-ray pulsar	dark halo	hypothetical		inversely proportional to the wavelength				PSR			inversely proportional to its momentum	pulsar			hidden mass	Pulsar (q.v.) that radiates in the X-ray region of the spectrum. Best verified examples are Her X-1 and Cen X-3. They are thought to be rotating, strongly magnetic neutron stars of about 1 M_sun in a grazing orbit around a more massive star from which they are accreting matter.	uncertainty principle
Centaurus X-3	dark halo	hypothetical	eclipsing binary	inversely proportional to the wavelength	0.2 magnitudes or greater	some difficulty in distinguishing between various kinds	5-10 kpc	PSR	half the stars in the solar neighborhood are members of star systems	e < 0.002	inversely proportional to its momentum		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	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	2

Next eclipsing binary: CV Serpentis Up: eclipsing binary, X-ray pulsar Previous eclipsing binary: BM Orionis