1 Scorpii

In today's article we will explore 1 Scorpii, a topic that has captured the attention of many people in recent years. With a focus on 1 Scorpii, we will analyze its impact on various aspects of everyday life, from health to technology. As we delve into this topic, we will cover its history, its current applications, and its potential for the future. With interviews with 1 Scorpii experts and analysis of relevant data, this article seeks to shed light on a particular aspect of 1 Scorpii that is often overlooked. Additionally, we will explore how 1 Scorpii has evolved over time, and how it continues to change the world we live in. Get ready for an exciting journey into the world of 1 Scorpii.

This article is about b Scorpii. Not to be confused with β Scorpii.
1 Scorpii
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Scorpius[1]
Right ascension 15h 50m 58.74452s[2]
Declination −25° 45′ 04.6649″[2]
Apparent magnitude (V) 4.63[1]
Characteristics
Spectral type B1.5 Vn[3]
B−V color index −0.072±0.003[1]
Astrometry
Radial velocity (Rv)−3.0±4.7[4] km/s
Proper motion (μ) RA: −14.20[2] mas/yr
Dec.: −25.12[2] mas/yr
Parallax (π)6.59±0.27 mas[2]
Distance490 ± 20 ly
(152 ± 6 pc)
Absolute magnitude (MV)−1.27[1]
Details
Mass8.3±0.2[5] M☉
Radius3.7[6] R☉
Luminosity3,890[6] L☉
Temperature24,000[6] K
Rotational velocity (v sin i)310[7] km/s
Age10.3±5.3[5] Myr
Other designations
b Sco, 1 Sco, CD−25°11131, HD 141637, HIP 77635, HR 5885, SAO 183854[8]
Database references
SIMBADdata

1 Scorpii, or b Scorpii, is a single[9] star in the southern zodiac constellation of Scorpius. It has an apparent magnitude of 4.63,[1] which is bright enough to be faintly visible to the naked eye on a dark night. The star shows an annual parallax shift of 6.59 mas from Earth's orbit, which equates to a distance of roughly 490 light years. It is a probable (89% chance) member of the Sco OB2 moving group.[10][9]

This is a B-type main-sequence star with a stellar classification of B1.5 Vn,[3] where the 'n' suffix indicates "nebulous" absorption lines being induced by rapid rotation. It has a projected rotational velocity of 310 km/s, which is giving the star an oblate shape with an equatorial bulge that is 13% wider than the polar radius.[7] There is some weak evidence that this is a Be star with a gaseous disk that is being viewed edge-on.[11]

1 Scorpii is a young star at around 10[5] million years old, with 8.3[5] times the mass of the Sun and 3.7 times the Sun's radius.[6] The star is radiating 3,890 times the Sun's luminosity from its photosphere at an effective temperature of about 24,000 K.[6]

References

  1. ^ a b c d e Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  2. ^ a b c d e van Leeuwen, F. (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 Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1988mcts.book.....H.
  4. ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  5. ^ a b c d Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  6. ^ a b c d e Hernández, J. S.; et al. (2005), "Herbig Ae/Be Stars in nearby OB Associations", The Astronomical Journal, 129 (2): 856, arXiv:astro-ph/0410494, Bibcode:2005AJ....129..856H, doi:10.1086/426918, S2CID 17672346.
  7. ^ a b Belle, G. T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
  8. ^ "b Sco". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-21.
  9. ^ a b Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  10. ^ Rizzuto, Aaron; et al. (October 2011), "Multidimensional Bayesian membership analysis of the Sco OB2 moving group", Monthly Notices of the Royal Astronomical Society, 416 (4): 3108–3117, arXiv:1106.2857, Bibcode:2011MNRAS.416.3108R, doi:10.1111/j.1365-2966.2011.19256.x, S2CID 54510608.
  11. ^ Rivinius, Th.; et al. (November 2006), "Bright Be-shell stars", Astronomy and Astrophysics, 459 (1): 137−145, Bibcode:2006A&A...459..137R, doi:10.1051/0004-6361:20053008.