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 -

Identifiers

omi Cet IRAS 02168-0312 GSC2.4.2 S0F2000125 AAVSO 000-BBD-706
SIMBAD * omi Cet Pan-STARRS 104420348370417356 SAO 29825 VSX 9237
GAIA DR3 2493390319631956352 SkyMapper - WRAY - GCVS omi Cet
2MASS J02192081-0258393 HIP 10826 Hen - BD -03 353
WISE J021920.76-025841.3 TYC 4693-1144-1 ESO - HD 14386

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) -        

Links

SIMBAD   CDS Portal   ARAS Database


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


Last updated: April 14, 2022