3 Serpentis
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Serpens |
| Right ascension | 15h 15m 11.3569s[1] |
| Declination | +04° 56′ 21.680″[1] |
| Apparent magnitude (V) | 5.337[2] |
| Characteristics | |
| Spectral type | K0III[3] |
| Astrometry | |
| Proper motion (μ) | RA: −17.768±0.264[1] mas/yr Dec.: 4.496±0.225[1] mas/yr |
| Parallax (π) | 6.3077 ± 0.2396 mas[1] |
| Distance | 520 ± 20 ly (159 ± 6 pc) |
| Absolute magnitude (MV) | +1.15[4] |
| Orbit[5] | |
| Period (P) | 66±5 yr |
| Semi-major axis (a) | 229±2″ |
| Eccentricity (e) | 0.962±0.005 |
| Inclination (i) | 132±4° |
| Details | |
| Surface gravity (log g) | +2.77[6] cgs |
| Temperature | 4,550[6] K |
| Metallicity [Fe/H] | +0.03[6] dex |
| Rotational velocity (v sin i) | 1.5[7] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
3 Serpentis is a binary star in the constellation Serpens with an orbital period of approximately 66 years. It is dimly visible to the naked eye with an apparent magnitude of 5.337. Located around 114 parsecs (370 ly) distant, it is an orange giant of spectral type K0III, a star that has used up its core hydrogen.
The two components of 3 Serpentis can be resolved using speckle interferometry and were separated by 0.23" in 2014. The orbit is highly eccentric and at periastron passage in 1997, the two are calculated to have been only 6 mas apart.[5]
Individual spectra for the two components of 3 Serpentis cannot be obtained and the spectral type of K0III is for the two stars combined. The primary is 2.5 magnitudes brighter than the secondary and cooler. The combined spectral type indicates that the primary is likely to have evolved away from the main sequence, but comparison of the colour and brightness of the secondary suggest it is still a main sequence star.[5]
References
[edit]- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
- ^ Cenarro, A. J.; Peletier, R. F.; Sanchez-Blazquez, P.; Selam, S. O.; Toloba, E.; Cardiel, N.; Falcon-Barroso, J.; Gorgas, J.; Jimenez-Vicente, J.; Vazdekis, A. (2007). "Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters". Monthly Notices of the Royal Astronomical Society. 374 (2): 664–690. arXiv:astro-ph/0611618. Bibcode:2007MNRAS.374..664C. doi:10.1111/j.1365-2966.2006.11196.x. S2CID 119428437.
- ^ McWilliam, Andrew (1990). "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances". The Astrophysical Journal Supplement Series. 74: 1075. Bibcode:1990ApJS...74.1075M. doi:10.1086/191527.
- ^ a b c Horch, Elliott P.; et al. (2015). "Observations of Binary Stars with the Differential Speckle Survey Instrument. VI. Measures during 2014 at the Discovery Channel Telescope". The Astronomical Journal. 150 (5): 151. arXiv:1509.03498. Bibcode:2015AJ....150..151H. doi:10.1088/0004-6256/150/5/151. S2CID 119115316.
- ^ a b c Soubiran, Caroline; Le Campion, Jean-François; Brouillet, Nathalie; Chemin, Laurent (2016). "The PASTEL catalogue: 2016 version". Astronomy & Astrophysics. 591: A118. arXiv:1605.07384. Bibcode:2016A&A...591A.118S. doi:10.1051/0004-6361/201628497. S2CID 119258214.
- ^ De Medeiros, J. R.; Do Nascimento, J. D.; Sankarankutty, S.; Costa, J. M.; Maia, M. R. G. (2000). "Rotation and lithium in single giant stars". Astronomy and Astrophysics. 363: 239. arXiv:astro-ph/0010273. Bibcode:2000A&A...363..239D.
- ^ "* 3 Ser". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 July 2014.
