omi Cet
        
      
        
  
    
    
    CONFIRMED
    MILKY WAY  
    
Constellation 
Cetus | 
Equatorial coordinates 
α = 02 19 20.792 
δ =  -02 58 39.496 | 
Galactic coordinates 
l = 167.7563°  
b = -57.9835°  | 
 
  
| Suspected | 
1957Ref | 
 
| Confirmed | 
2010Ref | 
 
| Symbiotic IR type | 
DRef | 
 
| Hot component type | 
accreting-onlyRef | 
 
| Outbursts | 
- | 
 
 
   | 
    
      
      
      
     | 
  
     
    
    
      
      
  Symbiotic Catalogs
  
| Bidelman (1954) | 
- | 
Allen (1984) | 
- | 
Belzcyński et al. (2001) | 
o Ceti (Conf.) | 
| Gaposchkin (1957) | 
o Cet (Conf.) | 
Kenyon (1986) | 
- | 
Akras et al. (2019) | 
o Ceti (Conf.) | 
| Boyarchuk (1969) | 
- | 
Vaidis (1988, 1991) | 
- | 
   
  
  
Position
| Right ascension (°) | 
34.8366Ref | 
Parallax (mas) | 
- | 
Reddening E(B-V) (mag) | 
0.02±0.0Ref, Note | 
| Declination (°) | 
-2.9776Ref | 
Distance (kpc) | 
0.092±0.01Ref, 0.11Ref -, Note | 
  | 
  | 
| Galactic longitude (°) | 
167.7563Ref | 
Proper motion in α (mas/yr) | 
- | 
  | 
  | 
| Galactic latitude (°) | 
-57.9835Ref | 
Proper motion in δ (mas/yr) | 
- | 
  | 
  | 
 
  
  
Observations
  
     | X-Ray | 
     YesRef | 
     IR type | 
     DRef | 
     Radio | 
     YesRef | 
   
   
     | X-Ray type | 
     βRef | 
     J (mag) | 
     -0.73Ref | 
     Flickering | 
     YesRef | 
   
   
     | GALEX FUV (mag) | 
     15.20Ref | 
     H (mag) | 
     -1.57Ref | 
     Outbursts | 
     - | 
   
   
     | GALEX NUV (mag) | 
     12.93Ref | 
     K (mag) | 
     -2.21Ref | 
     Outburst type | 
     - | 
   
   
     | IUE | 
     YesRef | 
     WISE W1 (mag) | 
     4.75Ref | 
     Jets | 
     - | 
   
   
     | FUSE | 
     YesRef | 
     WISE W2 (mag) | 
     3.36Ref | 
     Resolved nebula | 
     NoRef | 
   
   
     | U (mag) | 
     - | 
     WISE W3 (mag) | 
     0.10Ref | 
     IPmax (eV) | 
     54.4 (UV)Ref | 
   
   
     | B (mag) | 
     7.67Ref | 
     WISE W4 (mag) | 
     -3.69Ref | 
     [O III] lines | 
     NoRef | 
   
   
     | V (mag) | 
     6.74Ref | 
     IRAS 12μm (Jy) | 
     4880.00Ref | 
     He II lines | 
     NoRef | 
   
   
     | R (mag) | 
     5.03Ref | 
     IRAS 25μm (Jy) | 
     2260.00Ref | 
     [Fe VII] lines | 
     NoRef | 
   
   
     | I (mag) | 
     - | 
     IRAS 60μm (Jy) | 
     301.00Ref | 
     O VI lines | 
     NoRef | 
   
   
     | BP (mag) | 
     - | 
     IRAS 100μm (Jy) | 
     88.40Ref | 
      | 
      | 
   
   
     | G (mag) | 
     - | 
     AKARI S09 (Jy) | 
     - | 
      | 
      | 
   
   
     | RP (mag) | 
     - | 
     AKARI S18 (Jy) | 
     - | 
      | 
      | 
   
 
Orbit
| Orbital period (days) | 
181857.975Ref | 
γ velocity (km/h) | 
- | 
Size of giant’s orbit (AU) | 
- | 
| Eccentricity | 
0.16±nanRef | 
RV of giant (km/h) | 
- | 
Separation (AU) | 
70Ref | 
| Inclination (°) | 
112Ref | 
Inferior conj. of giant (JD) | 
- | 
Mass function | 
- | 
| Eclipses | 
- | 
  | 
  | 
Mass ratio | 
2.85Ref | 
| Orbital ephemeris | 
- | 
  | 
  | 
  | 
  | 
 
Cool component
| Spectral type | 
M5-9 IIIRef | 
Mass (M⊙) | 
2Ref | 
Pulsation | 
YesRef | 
| Eff. temperature (K) | 
2918-3192Ref | 
Radius (R⊙) | 
332-402Ref | 
Type | 
MiraRef | 
| IR type | 
DRef | 
Luminosity (L⊙) | 
8400-9360Ref | 
Pulsation period (days) | 
333.09±0.04Ref | 
| Metallicity [Fe/H] | 
-0.15±0.18Ref | 
  | 
  | 
Pulsation ephemeris | 
Max (V) = 2444839 + 333.09±0.04 x ERef | 
 
Hot component
| Type/Spectral type | 
WDRef | 
Mass (M⊙) | 
0.6Ref, 0.7Ref | 
Spin period (min) | 
- | 
  | Shell-burning/Accreting-only | 
  accreting-onlyRef | 
Radius (R⊙) | 
0.012Ref | 
Accretion disk | 
- | 
  | Eff. temperature (K) | 
  10000-20000Ref | 
Luminosity (L⊙) | 
- | 
  | 
  | 
  | Lower limit (K) | 
  - | 
  | 
  | 
  | 
  | 
| Upper limit (K) | 
- | 
  | 
  | 
  | 
  | 
 
Notes
The nature of omi Cet was debated in the literature for a long time. Kenyon & Webbink (1984) listed the object as an extreme example of the symbiotic phenomenon. Nowadays, the system is considered to be an accreting-only symbiotic star consisting of a Mira pulsator and a WD (resolved at several wavelengths; Karovska, 2006) on an orbit with an orbital period of 497.9 years (Prieur et al., 2002). It was detected in X-ray outburst by Karovska et al. (2005). Many aspects have been well-reviewed in the Introduction of the paper by Nhung et al. (2022).
 
References
- Karovska, M., Hack, W., Raymond, J. et al., 1997, ApJL, 482, 2, L175, 1997ApJ...482L.175K
 
- Karovska, M., Schlegel, E., Hack, W. et al., 2005, ApJL, 623, 2, L137, 2005ApJ...623L.137K
 
- Karovska, M., 2006, The X-ray Universe 2005, 604, 183, 2006ESASP.604..183K
 
- Kastner, J. H., Soker, N., 2004, ApJ, 616, 2, 1188, 2004ApJ...616.1188K
 
- Kenyon, S. J., Webbink, R. F., 1984, ApJ, 279, 252, 1984ApJ...279..252K
 
- Nhung, P. T., Hoai, D. T., Tuan-Anh, P. et al., 2022, ApJ, 927, 2, 169, 2022ApJ...927..169N
 
- Prieur, J. L., Aristidi, E., Lopez, B. et al., 2002, ApJS, 139, 1, 249, 2002ApJS..139..249P
 
- Sokoloski, J. L., Bildsten, L., 2010, ApJ, 723, 2, 1188, 2010ApJ...723.1188S
 
- Templeton, M. R., Karovska, M., 2009, ApJ, 691, 2, 1470, 2009ApJ...691.1470T
 
- Woodruff, H. C., Eberhardt, M., Driebe, T. et al., 2004, A&A, 421, 703, 2004A&A...421..703W
 
- Zamanov, R. K., Boeva, S., Spassov, B. et al., 2019, BlgAJ, 31, 110, 2019BlgAJ..31..110Z
 
 
Last updated: April 14, 2022