Astronomy:13 Scorpii
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Scorpius |
| Right ascension | 16h 12m 18.20490s[1] |
| Declination | −27° 55′ 34.9457″[1] |
| Apparent magnitude (V) | +4.568[2] |
| Characteristics | |
| Spectral type | B2V[3] |
| U−B color index | −0.74[4] |
| B−V color index | −0.16[4] |
| Astrometry | |
| Radial velocity (Rv) | 0 ± 5[5] km/s |
| Proper motion (μ) | RA: −10.38[1] mas/yr Dec.: −23.94[1] mas/yr |
| Parallax (π) | 6.81 ± 0.16[1] mas |
| Distance | 480 ± 10 ly (147 ± 3 pc) |
| Orbit[3] | |
| Period (P) | 5.7805 d |
| Eccentricity (e) | 0.19 |
| Periastron epoch (T) | JD 2443298.40 |
| Argument of periastron (ω) (secondary) | 115° |
| Semi-amplitude (K1) (primary) | 31.5 km/s |
| Details | |
| 13 Sco A | |
| Mass | 7.80[6] M☉ |
| Luminosity | 3020[7] L☉ |
| Rotational velocity (v sin i) | 165[8] km/s |
| Age | 11[6] Myr |
| 13 Sco B | |
| Mass | 1.12[6] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
13 Scorpii, also known by its Bayer designation c2 Scorpii, is a binary star in the constellation Scorpius. Its apparent magnitude is 4.57,[2] meaning it can be faintly seen with the naked eye. Based on parallax estimates made by the Hipparcos spacecraft, the system is located about 480 light-years (147 parsecs) away.[1] It is located within the Upper Scorpius subgroup of the Scorpius–Centaurus association.[6]
13 Scorpii is a spectroscopic binary, meaning the two stars are too close to be individually resolved, but periodic Doppler shifts in the star's spectrum indicate there must be orbital motion. In this case, light from only one of its stars can be detected and it is a double-lined spectroscopic binary.[3] The two have an orbital period of 5.7805 days and an eccentricity of 0.19.[3] The primary star, at 11 million years old,[6] is a B-type main-sequence star with a spectral type of B2V.[3] While the primary's mass is estimated to be about 7.8 M☉, its companion is thought to have a mass of 1.12 M☉.[6]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL.
- ↑ 2.0 2.1 Høg, E. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. Bibcode: 2000A&A...355L..27H.
- ↑ 3.0 3.1 3.2 3.3 3.4 Pourbaix, D. et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics 424 (2): 727–732. doi:10.1051/0004-6361:20041213. Bibcode: 2004A&A...424..727P.
- ↑ 4.0 4.1 Johnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory 4: 99. Bibcode: 1966CoLPL...4...99J.
- ↑ Evans, D. S. (1967). "The Revision of the General Catalogue of Radial Velocities". in Alan Henry Batten. 30. London: Academic Press. p. 57. Bibcode: 1967IAUS...30...57E.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Bonavita, M. (2016). "SPOTS: The Search for Planets Orbiting Two Stars. II. First constraints on the frequency of sub-stellar companions on wide circumbinary orbits". Astronomy & Astrophysics 593: A38. doi:10.1051/0004-6361/201628231. Bibcode: 2016A&A...593A..38B.
- ↑ Cite error: Invalid
<ref>tag; no text was provided for refs namedHernandez - ↑ Strom, S. E.; Wolff, S. C.; Dror, D. H. A. (2005). "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?". The Astronomical Journal 129 (2): 809–828. doi:10.1086/426748. Bibcode: 2005AJ....129..809S.
- ↑ "* c02 Sco". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+c02+Sco.
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