HD 34626
File:HD34626LightCurve.png A light curve for HD 34626 from KELT data, adapted from Labadie-Bartz et al. (2017)[1] | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | Template:RA[2] |
| Declination | Template:DEC[2] |
| Apparent magnitude (V) | 8.16[3] |
| Characteristics | |
| Spectral type | B1.5 IVnp[4] |
| U−B Template:Engvar | −0.68[5] |
| B−V Template:Engvar | +0.03[5] |
| Variable type | SX Ari?[6] |
| Astrometry | |
| Radial velocity (Rv) | −6[7] km/s |
| Proper motion (μ) | RA: −0.630[2] mas/yr Dec.: −4.017[2] mas/yr |
| Parallax (π) | 0.9831±0.0356 mas[2] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Details | |
| Mass | 4.4[2] Template:Solar mass |
| Radius | 21[2] Template:Solar radius |
| Luminosity | 556[2] Template:Solar luminosity |
| Temperature | 22,675[3] K |
| Rotational velocity (v sin i) | 310[8] km/s |
| Age | 200[9] Myr |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| MZ Aurigae, MZ Aur, BD+36°1090, HD 34626, HIP 24938, SAO 57915. | |
| Database references | |
| SIMBAD | data |
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HD 34626, also known as MZ Aurigae, is an unusual variable star in the northern constellation of Auriga. It has an apparent magnitude of 8.2 and is about 3,300 light years away.
The spectrum of HD 34626 had long been known to be unusual, with very broad lines indicating rapid rotation and emission lines marking it as a Be star. In 1970, John R. Percy found that it varies in brightness by 0.1 magnitude over time scales of 8 to 12 hours, but these variations are not periodic.[10] This indicates the variability is not caused by ellipsoidal effects, and the nature of the variability remains unknown.[8] It may be a type of SX Arietis variable.[6] It was given its variable star designation in 1972.[11]
HD 34626 has exhausted its core hydrogen and evolved away from the main sequence. Its spectral type indicates that it is a subgiant, but evolutionary models suggest it may be in the giant stage.[2]
References
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