V V CEPHEI

V V CEPHEI DATA

V V Cephei = HR8383 = HD208816
Name: ?

R.A. (2000) 21h 56m 39.1s
DEC. (2000) +63d 37' 33"
COMP
A
B
SPECT.
M2 Iaep
B8 Ve
DIAM
1621
MASS
100
?
LUM.
?
?
ABS.
?
?
MAG
?
?
TEMP.
?
?
I
1.86
 
V - I
+3.04
R
3.21
 
R - I
+1.40
V
4.91
 
B - V
+1.77
B
6.68
 
U - B
+0.39
U
7.07
     

Distance: 3000 light years

Epoch: JD 2,435,931.4

Period: 7430.5 days/ 20.34 years

Secondary Eclipse at Phase: ?

Ingress/Egress: 100/200? days
Totality: 490 days

Next Eclipse: (2017)

Secondary Eclipse - Fall/Winter 2005

Maximum Separation Date - ?

Recommended
Comparison Star: 20 Cep
HR8426
R.A. (2000) 22h 05m 00.4s
DEC. (2000) +62d 47m 09s

I = ?; R = ?; V = 5.27; B = 6.68; U = 8.46

Check Star: 19 Cep HR8428
R.A. (2000) 22h 05m 08.8s
DEC. (2000) +62d 16m 48s

R - I = 0.03 ; V = 5.11; B = 5.17; U =4.33

V V Cephei (Cep)

The V V Cephei star system has the second known longest period with a period of 20 years or 7430.5 days. V V Cep is a 5th magnitude system. The total eclipse is less than Epsilon Aurigae by nearly half a year (totality for Epsilon Aurigae is 670 days and for V V Cephei it is 490 days). The next eclipse of V V Cephei is due in 1997. V V Cep is one of the most massive binaries known. Its estimated mass is 100 solar masses and the primary star has a diameter of 1621 times the Sun. If it were our star, its surface would extend to between the orbits of Saturn and Uranus.

Reference: Van De Kamp, P. 1978, Sky and Telescope; The Distances of V V Cephei and Epsilon Aurigae, 397-399, November 1978.

Note:
Phil Bennett (CASA, U. of Colorado) has requested observations of VV Cep begnning summer of 2005 through spring of 2006 in order to try and catch the secondary eclispe. Any questions /data should be sent to Phil at pbennett@ap.stmarys.ca

 

Page Created 6 October 1996
Modified 15 February 2006

Jeff Hopkins (phxjeff@hposoft.com)

www.hposoft.com