HR 297
| Observation data Epoch 2000 Equinox 2000 |
|
|---|---|
| Constellation | Cassiopeia |
| Right ascension | 01h 04m 19.45075s[1] |
| Declination | +61° 34′ 48.6596″[1] |
| Apparent magnitude (V) | 5.84[2] |
| Characteristics | |
| Spectral type | F6V[3] |
| U−B color index | +0.11[2] |
| B−V color index | +0.56[2] |
| Astrometry | |
| Radial velocity (Rv) | −20.40[4] km/s |
| Proper motion (μ) | RA: −80.06[1] mas/yr Dec.: −25.06[1] mas/yr |
| Parallax (π) | 12.38 ± 0.39[1] mas |
| Distance | 263 ± 8 ly (81 ± 3 pc) |
| Absolute magnitude (MV) | 1.30[5] |
| Details | |
| Mass | 1.953[3] M☉ |
| Radius | 4.52 ± 0.15[3] R☉ |
| Luminosity | 25.16 ± 1.59[3] L☉ |
| Surface gravity (log g) | 3.86[6] cgs |
| Temperature | 6,089 ± 35[3] K |
| Metallicity [Fe/H] | −0.01[3] dex |
| Rotational velocity (v sin i) | 42.0[7] km/s |
| Age | 1.3[3] Gyr |
| Other designations | |
HR 297 is a solitary star in the northern circumpolar constellation of Cassiopeia. It has an apparent visual magnitude of 5.8,[2] making it faintly visible to the naked eye from dark suburban skies. Parallax measurements with the Hipparcos spacecraft put this system at a distance of roughly 263 light years.[1]
This is an F-type main sequence star with a stellar classification of F7V.[3] Because of the stability of this star, it is used as a standard in the photometric WBVR system.[9] The angular diameter of this star has been measured directly using the CHARA Array, yielding an estimate of 4.5 times the diameter of the Sun. Stellar models suggest a mass equal to about twice that of the Sun, with 25 times the Sun's luminosity.[3]
This is a young star with an estimated age of 1.3 billion years.[10] It is rotating rapidly, with a projected rotational velocity of 42 km/s.[11] The abundance of elements other than hydrogen and helium is about the same as that in the Sun. The effective temperature of the stellar atmosphere is 6,089 K,[3] giving it the yellow-white hued glow of an F-type star.[10]
This star has been examined for the presence of an infrared excess, but no statistically significant amount was detected. The detection of such an excess can indicate the presence of a dusty circumstellar disk.[12]
References
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01h 04m 19.45s, ++61° 34′ 48.66″
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