catalogues and names

The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version)

SKY2000 - Master Star Catalog

Smithsonian Astrophysical Observatory Star Catalog

The Washington Visual Double Star Catalog, 1996.0

Combined General Catalogue of Variable Stars (Vol. I-III)

catalogues and names

catalogues and names

VV Cep, HR 8383, HD 208816, SAO 19753, BD +62 2007, FK5: 3756, WDS 21567+6338

data from The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version) (Hoffleit+, 1991)

position, motion, parallax:

position (J2000)	RA: 21h 56min 39.1sec	DEC: +63° 37' 32''
position (2000.73)	RA: 21h 56min 40sec	DEC: +63° 37' 45''
position (B1900)	RA: 21h 53min 49.9sec	DEC: +63° 8' 57''
proper motion (J2000)	RA: -0.005 arcsec/a	DEC: -0.004 arcsec/a
radial velocity	-19 km/s note: spectroscopic binaries note: orbital data avaible
rotational velocity	0 km/s
trigonometric parallax	0.004 arcsec
galactic coordinates	longitude: 104.92°	latitude: 7.05°

magnitude

visual magnitude

4.91 (V on UBV Johnson system)

spectral / color information

spectral class	M2Iaep+B8Ve
B-V-magnitude	1.77
U-B-magnitude	0.39
R-I-magnitude
IR-note	object is infrared source (NASA merged infrared catalogue, Schmitz et al., 1978)

note (category: spectra):

Companion variously classified B9, B8Ve, and B6II.

variability information

variable star identification

VV Cep

note (category: variability):

EA 4.80 - 5.36V, 6.65 - 7.46p, 7430d. Also slow oscillations, amp. 0.15, per. 13.7y and amp. 0.03, per. 349d. Red observations indicate Sr amp. 0.4m, 58d. H alpha varies in 118.37d, period stable over 20y interval. This is probably the pulsation period of the red component. Amplitude varies in period 825d or more. The blue companion may be intrinsically variable. VV Cep also magnetic variable.

double/multiple star system information

separation	0.1 arcsec
mag difference (of double or brightest multiple)	1.7
note	Worley (1978) update of the IDS

note (category: double and multiple data):

A* var. M2Iab, B6IIe. Combined mag., colors. Absolute magnitudes based on astrometric and spectroscopic data are -4.0V for red component, -2.3 for the blue.

note (category: spectroscopic binaries):

7430.5d, K 19.4k/s, V0 -20.2k/s, msin3i 18.0, asini 1860. The SB secondary is probably also the visual companion. Mass transfer from red star to the hot companion. SB unresolved by speckle interferometry at 4-meter Mayall telescope in 1975-6.

miscellaneous information

note (category: group membership):

Cep OB2.

data from SKY2000 - Master Star Catalog (Myers+ 1997)

position, motion, parallax:

position (J2000)	RA: 21h 56min 39.125sec	DEC: +63° 37' 32.03''	±0.22 arcsec	source: 15
position (2000.73)	RA: 21h 56min 40sec	DEC: +63° 37' 45''	JD: 2451810.11
proper motion (J2000)	RA: -0.0007 arcsec/a	DEC: -0.004 arcsec/a		source: 25
radial velocity	-19 km/s			source: 25
trigonometric parallax	0.004 arcsec		-	source: 25
galactic coord. (B1950)	longitude: 104.92°	latitude: 7.05°

magnitude:

visual	4.8 (observed)	source: 31
photovisual	5.4	source: 2

spectral information:

spectral class	M0		source: 96
Morgan-Keenan	M2Iaep+B8Ve		source: 25
B-magnitude	6.68 ±0.05	B-V-magnitude	1.77
U-magnitude	7.07 ±0.05	U-B-magnitude	0.39

variability information:

source of data: 30

variability type	10
var. amplitude	0.56
var. period	7430
var. epoch	2443360 4. August 1977, 12:00:00 UT
next max light	2458220 11. April 2018, 12:00:00 UT

double/multiple star system information:

source of data: 19

separation between brightest and second brightest component	0.1 arcsec
position angle	174 °

sources:

2	HD and HDE Catalogs
Cannon, A.J., and E.C. Pickering, Harvard Annals, Vols 91-99, 1918-24, Cambridge, Massachusetts: Harvard University; Cannon, A.J., Harvard Annals, Vol. 100, 1925-36, Cambridge, Massachusetts: Harvard University; and Cannon, A.J., and M. Walton Mayall, Harvard Annals, Vol. 112, 1949, Cambridge, Massachusetts: Harvard University
15	FK5, FK5 Extension and FK5 Supplement
Fricke, W., H. Schwan and T. Lederle, "Fifth Fundamental Catalogue (FK5), Part I. The Basic Fundamental Stars," Veroff. Astronomisches Recheninstitut, No. 32, Heidelberg, Germany, 1988, and Fricke, W., H. Schwan, and T.E. Corbin, "Fifth Fundamental Catalogue (FK5), Part II. The FK5 Extension," Veröff. Astronomisches Recheninstitut, No. 33, Heidelberg, Germany, 1991
19	WDS Catalog
Worley, C.E., and G.G. Douglass, Washington Catalog of Visual Double Stars 1996.0, United States Naval Observatory, 1996
25	Bright Star Catalogue, 5th edition
Hoffleit, D. and Warren, W.H. Jr., The Bright Star Catalogue, 5th Revised Edition, Version 2, 1994
30	GCVS, 4th edition
Kholopov, P.N., et al., General Catalogue of Variable Stars, fourth edition, Moscow: Nauka Publishing House, 1985-88
31	CRM' (non-GCVS variable data)
Warren, W.H. Jr., Northern Hemisphere Catalog of Red Magnitudes, 1994
96	SAO or HD/HDE Catalog
Reference from Value 1 or Reference from Value 2

data from Smithsonian Astrophysical Observatory Star Catalog (SAO Staff 1966; USNO, ADC 1990)

position and proper motion:

position (B1950)	RA: 21h 55min 14.453sec	DEC: +63° 23' 13.53''	±0.024 arcsec
position (2000.73)	RA: 21h 56min 40sec	DEC: +63° 37' 45''	JD: 2451810.11
position (J2000)	RA: 21h 56min 39.176sec	DEC: +63° 37' 32.3''
proper motion B1950 (FK4)	RA: -0.0004 arcsec/a	DEC: 0.006 arcsec/a	±0.004 arcsec/a in RA ±0.003 arcsec/a in DEC
proper motion J2000 (FK5)	RA: -0.0001 arcsec/a	DEC: 0.001 arcsec/a
source of proper motion data	Determined by source catalog

magnitude:

visual	4.9 (accuracy: 1 decimal)
source of visual magnitude data	Source cited in source catalog introduction.

spectral information:

spectral class	M2e
source of spectral data	Taken from the Henry Draper Catalogue or no spectrum in source catalog.

remarks for duplicity and variability

Variable star in visual magnitude in source catalog

catalogues

source catalogue	GC, catalogue number: 30731
Durchmusterung	BD+62 2007
Boss General Catalogue	30731
Henry Draper Catalogue	208816

data from The Washington Visual Double Star Catalog, 1996.0 (Worley+, 1996)

position and proper motion:

position (J2000)	RA: 21h 56.7min	DEC: +63° 38'
proper motion (J2000)	RA: -0.005 arcsec/a	DEC: -0.004 arcsec/a

double/multiple star system information:

component	year	number of measures	position angle	angular separation	magnitude of 1st component	magnitude of 2nd component	spectral class(es)	discoverer code
-	1949	2	147°	0.1''	5.4	-	M2Iape	WRH
	1950		174°	-

discoverer information:

discoverer code	discoverer	reference
WRH	Wilson, R.H.

notes:

note	Eclipsing binary VV Cep. Visual duplicity uncertain. Spectrum of the eclipsing pair composite; M21aep+B8Ve.

data from Combined General Catalogue of Variable Stars (Vol. I-III) (Kholopov+ 1998)

position:

position (equinox 1950.0)

RA: 21h 55min 14.5sec

DEC: +63° 23' 14''

variability informations:

variability type	EA/GS+SRC	close binary eclipsing system pulsating variable star
magnitute at max. brightness	4.8
magnitute at min. brightness	5.36
photometric system	visual, photovisual or Johnson's V
epoch for maximum light [JD]	2443360 4. August 1977, 12:00:00 UT
period [d]	7430
next maximum light [JD]	2458220 11. April 2018, 12:00:00 UT
duration of the eclipse	08 % of period

spectral information

spectral class

M2epIa-Iab+B8:eV

references

to a study	Vol. I GCVS (see Kholopov et al. 1985-1988)
to a chart/photograph	Vol. I GCVS (see Kholopov et al. 1985-1988)

miscanellous

ID in the GCVS catalogue	20/40
constellation	Cepheus
notes on existence	The star is equivalent to '0200041 VW'.
There are notes in published catalog.

variability type description

variability type	description
EA	Eclipsing binary systems. These are binary systems with orbital planes so close to the observer's line of sight (the inclination i of the orbital plane to the plane orthogonal to the line of sight is close to 90 deg) that the components periodically eclipse each other. Consequently, the observer finds changes of the apparent combined brightness of the system with the period coincident with that of the components' orbital motion. EA Algol (Beta Persei)-type eclipsing systems. Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes. EB Beta Lyrae-type eclipsing systems. These are eclipsing systems having ellipsoidal components and light curves for which it is impossible to specify the exact times of onset and end of eclipses because of a continuous change of a system's apparent combined brightness between eclipses; secondary minimum is observed in all cases, its depth usually being considerably smaller than that of the primary minimum; periods are mainly longer than 1 day. The components generally belong to early spectral types (B-A). Light amplitudes are usually <2 mag in V. EW W Ursae Majoris-type eclipsing variables. These are eclipsers with periods shorter than 1 days, consisting of ellipsoidal components almost in contact and having light curves for which it is impossible to specify the exact times of onset and end of eclipses. The depths of the primary and secondary minima are almost equal or differ insignificantly. Light amplitudes are usually <0.8 mag in V. The components generally belong to spectral types F-G and later.
GS	Systems with one or both giant and supergiant components; one of the components may be a main sequence star.
SRC	Semiregular variables, which are giants or supergiants of intermediate and late spectral types showing noticeable periodicity in their light changes, accompanied or sometimes interrupted by various irregularities. Periods lie in the range from 20 to >2000 days, while the shapes of the light curves are rather different and variable, and the amplitudes may be from several hundredths to several magnitudes (usually 1-2 mag in V). SRA Semiregular late-type (M, C, S or Me, Ce, Se) giants displaying persistent periodicity and usually small (<2.5 mag in V) light amplitudes (Z Aqr). Amplitudes and light-curve shapes generally vary and periods are in the range of 35-1200 days. Many of these stars differ from Miras only by showing smaller light amplitudes; SRB Semiregular late-type (M, C, S or Me, Ce, Se) giants with poorly defined periodicity (mean cycles in the range of 20 to 2300 days) or with alternating intervals of periodic and slow irregular changes, and even with light constancy intervals (RR CrB, AF Cyg). Every star of this type may usually be assigned a certain mean period (cycle), which is the value given in the Catalogue. In a number of cases, the simultaneous presence of two or more periods of light variation is observed; SRC Semiregular late-type (M, C, S or Me, Ce, Se) supergiants (Mu Cep) with amplitudes of about 1 mag and periods of light variation from 30 days to several thousand days; SRD Semiregular variable giants and supergiants of F, G, or K spectral types, sometimes with emission lines in their spectra. Amplitudes of light variation are in the range from 0.1 to 4 mag, and the range of periods is from 30 to 1100 days (SX Her, SV UMa).