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physical object > natural object > celestial body > collection of stars > star system > binary star > UV Ceti
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UV Ceti comparison table
Subject has spectral type is part of is an instance of has optical brightness variation has eccentricity has observational problem has symbol has distance has acronym has abundance has prototype is a kind of has apparent magnitude has mass has name designated with has observable variation time scale has emission line has synonym has definition has luminosity class has angular separation has number of star
binary star         half the stars in the solar neighborhood are members of star systems star system greater than 0.08 the sun's mass    A system of two stars orbiting around a common center of gravity. Visual binaries are those whose components can be resolved telescopically (i.e., angular separation > 0'.5) and which have detectable orbital motion. Astrometric binaries are those whose dual nature can be deduced from their variable proper motion; spectroscopic binaries, those whose dual nature can be deduced from their variable radial velocity. At least half of the stars in the solar neighborhood are members of binary (or multiple) systems. (See photometric binaries; optical pairs.)  2
dMe stardKe star, dMe star     d   UV CetiM star greater than 0.08 the sun's mass  hydrogenmain sequence starM dwarf with hydrogen emission lines.V  
flare starM  0.2 magnitudes or greater some difficulty in distinguishing between various kindsd CV70 percent of all stars red dwarf greater than 0.08 the sun's mass
  1. R, S, T, U, V, W, X, Y, or Z and the genitive of the latin constellation name
  2. 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
  3. 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
  4. V 335, V 336, etc., when the double letter designations are exhausted
within a period of decades UV Ceti starStars undergoing erratic jumps in brightness (up to a few magnitudes) on time scales of the order of minutes. During the quiescent phase the spectrum is that of an M dwarf with emissions in the CaII and Balmer lines.V  
UV CetiM6e VCetusbinary star0.2 magnitudes or greatere = 0.615some difficulty in distinguishing between various kindsd2.8 pcCVhalf the stars in the solar neighborhood are members of star systemsUV Ceti Mv = 15.3 and 15.80.15 Msun
  1. R, S, T, U, V, W, X, Y, or Z and the genitive of the latin constellation name
  2. 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
  3. 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
  4. V 335, V 336, etc., when the double letter designations are exhausted
within a period of decadeshydrogenLuyten 726-8 BLate-type dwarf with spectra showing hydrogen emission lines. Faint flare star of very low mass. Like other flare stars, it is a member of a binary system in which both components are of nearly equal brightness. Radio flares have also been observed.V1".02

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