Astronomy:Nu Eridani
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Eridanus |
| Right ascension | 04h 36m 19.141s[2] |
| Declination | −03° 21′ 08.86″[2] |
| Apparent magnitude (V) | +3.930±0.023[3] |
| Characteristics | |
| Spectral type | B1.5 IV[4] |
| U−B color index | −0.879±0.007[3] |
| B−V color index | −0.210±0.009[3] |
| Variable type | SPB and Beta Cephei[5] |
| Astrometry | |
| Radial velocity (Rv) | 14.9[6] km/s |
| Proper motion (μ) | RA: +1.53[2] mas/yr Dec.: −5.01[2] mas/yr |
| Parallax (π) | 4.83 ± 0.19[2] mas |
| Distance | 680 ± 30 ly (207 ± 8 pc) |
| Absolute magnitude (MV) | −2.84±0.15[4] |
| Details[4] | |
| Mass | 9.3±0.3 M☉ |
| Radius | 6.2±0.5 R☉ |
| Luminosity | 7,943 L☉ |
| Surface gravity (log g) | 3.85±0.05 cgs |
| Temperature | 22,000±250 K |
| Rotational velocity (v sin i) | 26±2 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Nu Eridani (ν Eri) is a star in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.93.[3] The distance to this star is roughly 520 light years, based upon an annual parallax shift of 0.00625 arcseconds.[2] If the star were 33 ly (10 pc) from the Sun, it would be the brightest star in the night sky with an apparent magnitude of −2.84.[4] (Currently, the brightest star is Sirius at magnitude −1.46.)
This is a B-type subgiant star with a stellar classification of B1.5 IV.[4] It is a hybrid pulsator variable, lying as it does on the overlapping instability strips for Beta Cephei variables and slowly pulsating B-type stars.[5] The star shows at least fourteen pulsations frequencies, with nine that also display radial velocity variations.[8] It has about nine times the mass of the Sun and six times the Sun's radius. Nu Eridani shines with 7,943 times the solar luminosity from its outer atmosphere at an effective temperature of 22,000 K.[4]
References
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 3.0 3.1 3.2 3.3 Nieva, M.-F. (February 2013), "Temperature, gravity, and bolometric correction scales for non-supergiant OB stars", Astronomy & Astrophysics 550: A26, doi:10.1051/0004-6361/201219677, Bibcode: 2013A&A...550A..26N.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Nieva, María-Fernanda; Przybilla, Norbert (2014), "Fundamental properties of nearby single early B-type stars", Astronomy & Astrophysics 566: A7, doi:10.1051/0004-6361/201423373, Bibcode: 2014A&A...566A...7N.
- ↑ 5.0 5.1 Moravveji, Ehsan (January 2016), "The impact of enhanced iron opacity on massive star pulsations: updated instability strips", Monthly Notices of the Royal Astronomical Society: Letters 455 (1): L67–L71, doi:10.1093/mnrasl/slv142, Bibcode: 2016MNRAS.455L..67M.
- ↑ Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Carnegie Institute of Washington D.C.), Bibcode: 1953GCRV..C......0W.
- ↑ "nu. Eri". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=nu.+Eri.
- ↑ Daszyńska-Daszkiewicz, J.; Walczak, P. (March 2010), "Complex asteroseismology of the β Cep/slowly pulsating B-type pulsator ν Eridani: constraints on opacities", Monthly Notices of the Royal Astronomical Society 403 (1): 496–504, doi:10.1111/j.1365-2966.2009.16141.x, Bibcode: 2010MNRAS.403..496D.
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