13 Scorpii

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13 Scorpii
Observation data
Epoch J2000        Equinox J2000
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  mas [1]
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☉
Temperature 24000 [7]   K
Rotational velocity (v sin i)165 [8]  km/s
Age 11 [6]   Myr
13 Sco B
Mass 1.12 [6]   M☉
Other designations
c2 Sco, 13 Sco, CD −27° 10841, HD  145482, HIP  79404, HR  6028, SAO  184221 [9]
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]

Related Research Articles

<span class="mw-page-title-main">Beta Scorpii</span> Multi-star system in the constellation of Scorpius

Beta Scorpii is a multiple star system in the southern zodiac constellation of Scorpius. It bore the traditional proper name of Acrab, though the International Astronomical Union now regards that name as applying only to the β Scorpii Aa component.

<span class="mw-page-title-main">Sigma Scorpii</span> Multiple star system in the constellation of Scorpius

Sigma Scorpii, is a multiple star system in the constellation of Scorpius, located near the red supergiant Antares, which outshines it. This system has a combined apparent visual magnitude of +2.88, making it one of the brighter members of the constellation. Based upon parallax measurements made during the Hipparcos mission, the distance to Sigma Scorpii is roughly 696 light-years (214 parsecs). North et al. (2007) computed a more accurate estimate of 568+75
−59 light years.

<span class="mw-page-title-main">Rho Scorpii</span>

Rho Scorpii is a double star in the constellation of Scorpius. It has an apparent visual magnitude of +3.87, which is bright enough to be seen with the naked eye. Based upon parallax measurements, it is located approximately 472 light years from the Sun. At that distance, the visual magnitude of the system is reduced by 0.07 due to extinction from interstellar dust. It is a member of the Upper Scorpius OB association.

Omicron Scorpii is a star in the zodiac constellation of Scorpius. With an apparent visual magnitude of +4.57, it is visible to the naked eye. Parallax measurements indicate a distance of roughly 900 light years. It is located in the proximity of the Rho Ophiuchi dark cloud.

Psi Scorpii, which is Latinized from ψ Scorpii, is a star in the zodiac constellation of Scorpius. It is white in hue and has an apparent visual magnitude of 4.94, which is bright enough to be faintly visible to the naked eye. Based upon parallax measurements, it is located at a distance of around 162 light years from the Sun. Data collected during the Hipparcos mission suggests it is an astrometric binary, although nothing is known about the companion. The system is drifting closer to the Sun with a radial velocity of −5 km/s.

<span class="mw-page-title-main">Pi Virginis</span> Binary star in the constellation Virgo

Pi Virginis is a binary star in the zodiac constellation of Virgo. It is visible to the naked eye with an apparent visual magnitude of 4.64. The distance to this star, based upon parallax measurements, is roughly 380 light years.

39 Boötis is a triple star system located around 224 light years away from the Sun in the northern constellation of Boötes. It is visible to the naked eye as a faint, yellow-white hued star with a combined apparent magnitude of 5.68. The system is moving closer to the Earth with a heliocentric radial velocity of −31 km/s.

Pi1 Cygni (π1 Cygni, abbreviated Pi1 Cyg, π1 Cyg) is a binary star in the northern constellation of Cygnus. It is visible to the naked eye, having a combined apparent visual magnitude of 4.66. The distance to this system can be roughly gauged by its annual parallax shift of 1.89 mas, which yields a separation of around 1,700 light years from the Sun, give or take a hundred light years.

<span class="mw-page-title-main">HD 129116</span> Binary star in the constellation Centaurus

HD 129116 is a binary star in the northeastern part of Centaurus, east of Menkent. It is also known by its Bayer designation of b Centauri, while HD 129116 is the star's identifier in the Henry Draper catalogue. This object has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.01. It is located at a distance of approximately 325 light years from the Sun based on parallax, and has an absolute magnitude of −1.07.

3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

Tau Librae, Latinized from τ Librae, is the Bayer designation for a binary star system at the southern edge of the zodiac constellation of Libra. It can be seen with the naked eye, having an apparent visual magnitude of 3.68. The distance to this system is around 367 light years, as determined from an annual parallax shift of 8.89 mas.

HD 176051 is a spectroscopic binary star system approximately 49 light years away from Earth in the constellation Lyra. The pair orbit with a period of 22,423 days and an eccentricity of 0.25. Compared to the Sun, they have a somewhat lower proportion of elements more massive than helium. Their individual masses are estimated at 1.07 and 0.71 solar masses (M☉). The system is moving closer to the Sun with a radial velocity of −47 km/s and will reach perihelion in about 269,000 years when it comes within roughly 17 ly (5.1 pc) of the Sun.

<span class="mw-page-title-main">V636 Scorpii</span> Spectroscopic binary star system in the constellation Scorpius

V636 Scorpii is a multiple star system in the constellation Scorpius, 3,000 light years away. The primary is a Classical Cepheid variable and its visual magnitude varies from 6.4 to 6.9.

<span class="mw-page-title-main">ET Andromedae</span> Star in the constellation Andromeda

ET Andromedae is a binary star system star in the northern constellation of Andromeda. It has an apparent visual magnitude of 6.48, placing it at the nominal limit for visibility with the naked eye. The distance to this system can be estimated from its annual parallax shift of 5.42 mas, which yields a value of 602 light years.

1 Scorpii, or b Scorpii, is a single star in the southern zodiac constellation of Scorpius. It has an apparent magnitude of 4.63, 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 member of the Sco OB2 moving group.

<span class="mw-page-title-main">Epsilon Herculis</span> Multiple star systen in the constellation Hercules

Epsilon Herculis, Latinized from ε Herculis, is a fourth-magnitude multiple star system in the northern constellation of Hercules. The combined apparent visual magnitude of 3.9111 is bright enough to make this system visible to the naked eye. Based upon an annual parallax shift of 21.04 mas as seen from Earth, it is located 155 light years from the Sun. The system is moving closer to the Sun with a radial velocity of −25 km/s.

HR 7955 is a binary star system in the northern circumpolar constellation of Cepheus, near the constellation border with Cygnus. It has a yellow-white hue and is faintly visible to the naked eye with a combined apparent visual magnitude of 4.51. The system is located at a distance of 89 light-years from the Sun, based on parallax. It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.243 arc seconds per annum, and is drifting closer to the Sun with a radial velocity of -33 km/s.

HD 134687 is a binary star system in the southern constellation Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.81. The distance to HD 134687 can be estimated from its annual parallax shift of 7.6 mas, yielding roughly 430 light years. It is a member of the ~11 million year old Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association, the closest OB association to the Sun.

<span class="mw-page-title-main">Q Scorpii</span> High proper motion binary star system in the constellation of Scorpius

Q Scorpii, also designated as HD 159433, is an astrometric binary located in the southern zodiac constellation Scorpius. It has an apparent magnitude of 4.27, making it readily visible to the naked eye under ideal conditions. It lies in the tail of Scorpius, between the stars λ Scorpii and μ Scorpii and is located 7′ away from the faint globular cluster Tonantzintla 2. Based on parallax measurements from Gaia DR3, the system is estimated to be 158 light years distant, but is approaching the Solar System with a heliocentric radial velocity of −49 km/s.

38 Leonis Minoris is a binary star system in the northern constellation of Leo Minor. It shines with a combined light of apparent magnitude 5.84, which indicates it a dimly visible to the naked eye under good viewing conditions. An annual parallax shift of 19.11 mas provides a distance estimate of around 171 light years. It has a relatively high proper motion, traversing the celestial sphere at a rate of 0.226 arcseconds per year, and is moving away from the Sun with a radial velocity of +31 km/s.

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 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.
  3. 1 2 3 4 5 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.
  4. 1 2 Johnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
  5. ↑ 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.
  6. 1 2 3 4 5 6 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.
  7. 1 2 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.
  8. ↑ 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.
  9. ↑ "* c02 Sco". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 10 April 2017.
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