13 Scorpii

In this article we will address 13 Scorpii, a topic that has captured the attention and interest of people from various areas and profiles. 13 Scorpii is a widely debated topic that has given rise to conflicting opinions, generating a wide spectrum of analysis, discussions and reflections. Since its inception, 13 Scorpii has been the object of study, research and speculation, arousing curiosity and concern in those who seek to understand, deepen and understand its implications and consequences. Over the years, 13 Scorpii has evolved and has positioned itself as a relevant topic in various contexts, covering social, political, economic, scientific and cultural aspects. In this article, we will explore different perspectives, approaches and debates related to 13 Scorpii, with the aim of offering a comprehensive and enriching vision of this exciting topic.

This article is about c2 Scorpii. For other stars with this Bayer designation, see c Scorpii.
13 Scorpii
Observation data
Epoch J2000      Equinox J2000
Constellation Scorpius[1]
Right ascension 16h 12m 18.20490s[2]
Declination −27° 55′ 34.9457″[2]
Apparent magnitude (V) +4.568[3]
Characteristics
Spectral type B2V[4]
U−B color index −0.74[5]
B−V color index −0.16[5]
Astrometry
Radial velocity (Rv)0 ± 5[6] km/s
Proper motion (μ) RA: −10.38[2] mas/yr
Dec.: −23.94[2] mas/yr
Parallax (π)6.81±0.16 mas[2]
Distance480 ± 10 ly
(147 ± 3 pc)
Absolute magnitude (MV)−1.25[1]
Orbit[4]
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
Mass7.80[7] M☉
Luminosity3020[8] L☉
Temperature24000[8] K
Rotational velocity (v sin i)165[9] km/s
Age11[7] Myr
13 Sco B
Mass1.12[7] M☉
Other designations
c2 Sco, 13 Sco, CD−27° 10841, HD 145482, HIP 79404, HR 6028, SAO 184221[10]
Database references
SIMBADdata

13 Scorpii, also known by its Bayer designation c2 Scorpii, is a binary star in the constellation Scorpius. Its apparent magnitude is 4.57,[3] 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.[2] It is located within the Upper Scorpius subgroup of the Scorpius–Centaurus association.[7]

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.[4] The two have an orbital period of 5.7805 days and an eccentricity of 0.19.[4] The primary star, at 11 million years old,[7] is a B-type main-sequence star with a spectral type of B2V.[4] 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☉.[7]

References

  1. ^ a b Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  2. ^ a b c d e f van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  3. ^ a b Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27 – L30. Bibcode:2000A&A...355L..27H.
  4. ^ a b c d e Pourbaix, D.; et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727–732. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID 119387088.
  5. ^ a b Johnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
  6. ^ Evans, D. S. (1967). "The Revision of the General Catalogue of Radial Velocities". In Alan Henry Batten; John Frederick Heard (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30 held at the University of Toronto 20-24 June, 1966. International Astronomical Union. Vol. 30. London: Academic Press. p. 57. Bibcode:1967IAUS...30...57E.
  7. ^ a b c d e f Bonavita, M.; et al. (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. arXiv:1605.03962. Bibcode:2016A&A...593A..38B. doi:10.1051/0004-6361/201628231. S2CID 55950739.
  8. ^ a b Hernández, J.; Calvet, N.; Hartmann, L.; Briceño, C.; Sicilia-Aguilar, A.; Berlind, P. (2005). "Herbig Ae/Be Stars in nearby OB Associations". The Astronomical Journal. 129 (2): 856–871. arXiv:astro-ph/0410494. Bibcode:2005AJ....129..856H. doi:10.1086/426918. S2CID 17672346.
  9. ^ 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. arXiv:astro-ph/0410337. Bibcode:2005AJ....129..809S. doi:10.1086/426748. S2CID 15059129.
  10. ^ "* c02 Sco". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 10 April 2017.