CONFIRMED
MILKY WAY
|
| UV Aur | IRAS 05185+3227 | GSC2.4.2 N9V5042692 | AAVSO 000-BCT-850 |
| SIMBAD V* UV Aur | Pan-STARRS 147010804541743958 | SAO - | VSX 3797 |
| GAIA DR3 180919213811383680 | SkyMapper - | WRAY - | GCVS UV Aur |
| 2MASS J05214891+3230404 | HIP - | Hen - | BD +32 957A |
| WISE J052148.91+323040.2 | TYC 2394-373-1 | ESO - | HD 34842A |
| Bidelman (1954) | - | Allen (1984) | UV Aur (Conf.) | Belzcyński et al. (2001) | UV Aur (Conf.) |
| Gaposchkin (1957) | - | Kenyon (1986) | UV Aur (Conf.) | Akras et al. (2019) | UV Aur (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | UV Aur (Conf.) |
| Right ascension (°) | 80.4538Ref | Parallax (mas) | 0.993±0.028Ref | Reddening E(B-V) (mag) | 0.6±0.03Ref, Note |
| Declination (°) | 32.5111Ref | Distance (kpc) | 0.96Ref, Note, 0.96Ref, Note | ||
| Galactic longitude (°) | 174.2183Ref | Proper motion in α (mas/yr) | -0.98±0.03Ref | ||
| Galactic latitude (°) | -2.3494Ref | Proper motion in δ (mas/yr) | -3.27±0.02Ref |
| X-Ray | YesRef | IR type | SRef | Radio | YesRef |
| X-Ray type | β/δRef | J (mag) | 4.03Ref | Flickering | NoRef |
| GALEX FUV (mag) | - | H (mag) | 3.02Ref | Outbursts | - |
| GALEX NUV (mag) | - | K (mag) | 2.13Ref | Outburst type | - |
| IUE | YesRef | WISE W1 (mag) | -1.21Ref | Jets | - |
| FUSE | NoRef | WISE W2 (mag) | -1.29Ref | Resolved nebula | - |
| U (mag) | - | WISE W3 (mag) | -0.30Ref | IPmax (eV) | 40.7Ref |
| B (mag) | 11.16Ref | WISE W4 (mag) | -0.88Ref | [O III] lines | NoRef |
| V (mag) | 10.41Ref | IRAS 12μm (Jy) | 69.40Ref | He II lines | NoRef |
| R (mag) | 9.15Ref | IRAS 25μm (Jy) | 20.60Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 3.37Ref | O VI lines | NoRef |
| BP (mag) | 10.04Ref | IRAS 100μm (Jy) | 4.38Ref | ||
| G (mag) | 7.57Ref | AKARI S09 (Jy) | - | ||
| RP (mag) | 6.51Ref | AKARI S18 (Jy) | 21.40Ref |
| Orbital period (days) | 5100?Ref | γ velocity (km/h) | - | Size of giant’s orbit (AU) | - |
| Eccentricity | - | RV of giant (km/h) | - | Separation (AU) | - |
| Inclination (°) | - | Inferior conj. of giant (JD) | - | Mass function | - |
| Eclipses | - | Mass ratio | - | ||
| Orbital ephemeris | - |
| Spectral type | C8.1JRef | Mass (M⊙) | - | Pulsation | YesRef |
| Eff. temperature (K) | 2920Ref | Radius (R⊙) | - | Type | MiraRef |
| IR type | SRef | Luminosity (L⊙) | - | Pulsation period (days) | 393.4Ref, 394.42Ref |
| Metallicity [Fe/H] | - | Pulsation ephemeris | Max (V) = 2441062 + 394.42 x ERef |
| Type/Spectral type | WDRef | Mass (M⊙) | - | Spin period (min) | - |
| Shell-burning/Accreting-only | accreting-onlyRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
The UV Aur system consists of a carbon Mira-type variable (UV Aur A) and a B8.5-type star (UV Aur B), at a projected separation of about 3400 AU (Herbig, 2009). UV Aur A has been classified as a symbiotic star based on the detection of [O III] and [Ne III] lines (Sanford (1950)). This classification was later supported by the detection of [Fe VII] lines by Seal, 1988. However, this was disputed by Herbig (2009), who claimed that previous spectra had not shown He II lines (e.g., Ikeda & Tamura, 2004). In addition, Reimers & Groote (1983) suggested the presence of a hot white dwarf in the system. Furthermore, Khudyakova (1985) suggested a 14-year-long orbital period based on polarimetric observations. Luna et al. (2013) detected strong UV and X-ray emission from UV Aur A.