9 Aurigae
9 Aurigae (9 Aur) is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years (26 parsecs) from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | 05h 06m 40.62967s |
| Declination | +51° 35′ 51.8025″ |
| Apparent magnitude (V) | 4.93 - 5.03 |
| Characteristics | |
| Spectral type | F2V |
| U−B color index | -0.03 |
| B−V color index | +0.34 |
| Variable type | γ Dor |
| Astrometry | |
| A | |
| Radial velocity (Rv) | −0.47±0.57 km/s |
| Proper motion (μ) | RA: −28.557 mas/yr Dec.: −171.822 mas/yr |
| Parallax (π) | 37.0551 ± 0.1371 mas |
| Distance | 88.0 ± 0.3 ly (26.99 ± 0.10 pc) |
| B | |
| Proper motion (μ) | RA: −54.582 mas/yr Dec.: −156.009 mas/yr |
| Parallax (π) | 37.0796 ± 0.0631 mas |
| Distance | 88.0 ± 0.1 ly (26.97 ± 0.05 pc) |
| C | |
| Radial velocity (Rv) | −1.88±0.17 km/s |
| Proper motion (μ) | RA: −32.386 mas/yr Dec.: −173.026 mas/yr |
| Parallax (π) | 37.2115 ± 0.0184 mas |
| Distance | 87.65 ± 0.04 ly (26.87 ± 0.01 pc) |
| Orbit | |
| Period (P) | 391.7 d |
| Eccentricity (e) | 0.37 |
| Semi-amplitude (K1) (primary) | 5.8 km/s |
| Details | |
| A | |
| Mass | 1.97 M☉ |
| Radius | 1.56 R☉ |
| Luminosity | 6.042 L☉ |
| Surface gravity (log g) | 4.07 cgs |
| Temperature | 7,023 K |
| Metallicity [Fe/H] | −0.12 dex |
| Rotational velocity (v sin i) | 21.0 km/s |
| B | |
| Mass | 0.49 M☉ |
| Temperature | 4,947 K |
| C | |
| Mass | 0.751 M☉ |
| Radius | 0.756 R☉ |
| Luminosity | 0.162 L☉ |
| Temperature | 4,633 K |
| Other designations | |
| Database references | |
| SIMBAD | 9 Aur A |
| 9 Aur B | |
| 9 Aur C | |
It is a well-studied Gamma Doradus variable, and was one of the first stars to be so-classified. This star type varies in luminosity due to non-radial pulsations. Its apparent magnitude varies from 4.93 to 5.03 over a period of 1.25804 days. For that reason it has been given the variable star designation V398 Aurigae.
9 Aurigae is a multiple star system. The naked-eye component A is a single-lined spectroscopic binary. Only the signature of an F-type main sequence star can be seen in the spectrum, but the periodic doppler shift of the absorption lines demonstrates that there is a hidden companion in a 391.7-day orbit. The gravitational interaction of the two bodies produces variations in their respective motions, which is what creates the doppler shift.
Four other companions to 9 Aurigae are listed in multiple star catalogs. The closest companion is a 12th-magnitude red dwarf 5″ away. 90″ away is component C, a 9th-magnitude star with a spectral class of K5Ve, which may also be a spectroscopic binary. Further-separated still is a 14th-magnitude star, component D, proposed to be a more distant red giant, although Gaia astrometry places it at a similar distance and with a similar proper motion. The most widely-separated companion is component E, a distant unrelated star.