V1054 Ophiuchi

An ultraviolet band light curve for a flare on V1054 Ophiuchi, plotted from data published by Dal and Evren (2010)[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ophiuchus
Right ascension 16h 55m 25.2222456607s[2]
Declination −08° 19′ 21.296969682″[2]
Apparent magnitude (V) 9.74/10.34/10.84/11.74/16.80[3]
Characteristics
Spectral type M3 V[4] / M4 Ve[note 1] / M3.5 V[4] / M7.0 V[3]
Astrometry
Proper motion (μ) RA: −817.580±0.052[2] mas/yr
Dec.: −898.595±0.040[2] mas/yr
Parallax (π)153.8754 ± 0.0474 mas[2]
Distance21.196 ± 0.007 ly
(6.499 ± 0.002 pc)
Absolute magnitude (MV)10.69±0.02 / 11.29±0.05 / 11.79±0.05 / 12.69[3][note 2]
VB 8
Proper motion (μ) RA: −813.038±0.063[5] mas/yr
Dec.: −870.609±0.044[5] mas/yr
Parallax (π)153.9659 ± 0.0570 mas[5]
Distance21.184 ± 0.008 ly
(6.495 ± 0.002 pc)
Absolute magnitude (MV)17.75[3]
Orbit[4]
PrimaryV1054 Oph A
CompanionV1054 Oph B
Period (P)1.717267±0.000039[3] yr
Semi-major axis (a)0.2273±0.0004"
(1.46683 AU[note 3])
Eccentricity (e)0.042±0.001
Inclination (i)160.3±0.1°
Longitude of the node (Ω)−10.2±0.2°
Periastron epoch (T)MJD 53943±3
Argument of periastron (ω)
(secondary)		306.0±1.5°
Orbit[4]
PrimaryV1054 Oph Ba
CompanionV1054 Oph Bb
Period (P)2.965509±0.000006 d
Semi-major axis (a)0.00687[note 4]"
(0.04432 AU[note 5])
Eccentricity (e)0.0209±0.0008
Inclination (i)164.18±0.08°
Periastron epoch (T)MJD 50919.48±0.03
Argument of periastron (ω)
(secondary)		150.0±3.0°
Details
V1054 Oph AB
Mass0.4155±0.0057 / 0.3466±0.0047 / 0.3143±0.0040[4] M☉
Gliese 643
Mass0.19[3] M☉
Details
VB 8
Mass0.0914+0.0026
−0.0025[6] M☉
Radius0.1214+0.0060
−0.0057[6] R☉
Luminosity0.000645+0.000004
−0.000005[6] L☉
Temperature2,640+65
−64[6] K
Other designations
V1054 Oph, BD−08°4352, GJ 644, HD 152751, HIP 82817, SAO 141439, Wolf 630[7]
Database references
SIMBADThe system
ABab
A
Bab
GJ 643
C (vB 8)
vB 8B (artifact)

V1054 Ophiuchi, together with the star Gliese 643, is a nearby quintuple star system. In the constellation Ophiuchus at a distance of 21.19 light-years. It consists of five stars, all of which are red dwarfs. The alternative designation of Wolf 630 forms the namesake of a moving group of stars that share a similar motion through space.[8]

Overview

V1054 Ophiuchi/Gliese 643 has the largest number of stars of all star systems located within 10 pc from Earth.[4] It is also the nearest quintuple star system[3] (the next nearest star systems with at least five stars are GJ 2069 (quintuple)[4] at 41.8 light-years, and Castor[3] (sextuple) at 51.6 light-years), and the only quintuple star system within 10 pc.[4][9]

The system consists of three widely separated parts:

  • close triple subsystem V1054 Ophiuchi A-Bab (including very close binary subsystem V1054 Ophiuchi Bab)
  • Gliese 643
  • V1054 Ophiuchi C (vB 8)

Hierarchy of the system:[3]

V1054 Ophiuchi/Gliese 643
V1054 Ophiuchi/Gliese 643 (without V1054 Ophiuchi C)
V1054 Ophiuchi A‑Bab
V1054 Ophiuchi Bab

V1054 Ophiuchi Ba

V1054 Ophiuchi Bb

V1054 Ophiuchi A

Gliese 643

V1054 Ophiuchi C (vB 8)

The brightest and most massive of these five stars is V1054 Ophiuchi A. The close binary subsystem V1054 Ophiuchi B is more massive than V1054 Ophiuchi A, however, its total visual magnitude is 0.1 mag fainter than V1054 Ophiuchi A's visual magnitude.[3]

The total apparent magnitude of the V1054 Ophiuchi A-Bab triple subsystem is 9.02.[3][10]

Despite V1054 Ophiuchi/Gliese 643 consisting of low-mass stars, the system's total mass, due to the large number of components, exceeds the Solar mass,[3] (it is about 1.35 M☉).

Distance

Currently, the most accurate distance estimate of V1054 Ophiuchi/Gliese 643 (apart from weighted mean distance, see below) is a trigonometric parallax of V1054 Ophiuchi AB from Gaia EDR3, published in 2020:[2] 153.8754±0.0474 mas, corresponding to a distance of 6.499±0.002 pc, or 21.196±0.007 ly.

Past V1054 Ophiuchi/Gliese 643 distance estimates

V1054 Ophiuchi A-Bab:

SourcePaperParallax, masDistance, pcDistance, lyRef.
WoolleyWoolley et al. 1970156 ± 46.41 ± 0.1720.9 ± 0.6[11]
GJ, 3rd versionGliese & Jahreiß 1991153.9 ± 2.66.50 ± 0.1121.19 ± 0.36[12]
YPC, 4th editionvan Altena et al. 1995154.8 ± 0.66.460 ± 0.02521.07 ± 0.08[13]
HipparcosPerryman 1997174.23 ± 3.905.74 ± 0.1318.7 ± 0.4[10]
SoederhjelmSoederhjelm 1999155.63 ± 1.816.43 ± 0.0820.96 ± 0.25[14]
Hipparcos2van Leeuwen 2007161.41 ± 5.646.20 ± 0.2220.21 ± 0.73[15]

Gliese 643:

SourcePaperParallax, masDistance, pcDistance, lyRef.
WoolleyWoolley et al. 1970169 ± 55.92 ± 0.1819.3 ± 0.6[11]
GJ, 3rd versionGliese & Jahreiß 1991171.9 ± 7.35.82 ± 0.2619.0 ± 0.8[12]
YPC, 4th editionvan Altena et al. 1995169.8 ± 6.65.89 ± 0.2419.2 ± 0.8[13]
HipparcosPerryman 1997153.96 ± 4.046.50 ± 0.1821.2 ± 0.6[10]
Hipparcos2van Leeuwen 2007148.92 ± 4.006.72 ± 0.1921.9 ± 0.6[15]

V1054 Ophiuchi C (vB 8):

SourcePaperParallax, masDistance, pcDistance, lyRef.
CTIOPI 1.5 mTSN 14 (Costa et al. 2005)155.43 ± 1.336.43 ± 0.0620.98 ± 0.18[16]

Weighted mean distance

Weighted mean parallax,[17] considering YPC (V1054 Ophiuchi A-Bab and Gliese 643), Hipparcos (Soederhjelm — V1054 Ophiuchi A-Bab and van Leeuwen — Gliese 643) and CTIOPI (V1054 Ophiuchi C) data, is 154.96 ± 0.52 mas,[18] corresponding to a distance 6.453 ± 0.022 pc, or 21.05 ± 0.07 ly.

V1054 Ophiuchi A-Bab (inner triple subsystem)

V1054 Ophiuchi A-Bab is a close spectroscopic triple subsystem, consisting of the brighter component V1054 Ophiuchi A and the more massive binary subsystem V1054 Ophiuchi Bab, orbiting each other with a period of 627 days,[4][3] or 1.72 years.[3] V1054 Ophiuchi Bab components are orbiting each other with a period of 2.9655 days.[4][3] Both outer and inner orbits are nearly circular and, probably, coplanar[4][3] (in keeping with a general tendency of close triple systems).[4]

V1054 Ophiuchi A-Bab pair is also visually resolved (for nearly 50 years it was the shortest-period resolved by visual means binary, since its binarity was discovered by G. P. Kuiper in 1934),[3] whereas V1054 Ophiuchi Ba-Bb pair is still unresolved).[4][3][note 6]

Distant components

Gliese 643

The projected separation of Gliese 643 from V1054 Ophiuchi A-Bab is 72 arcsec,[4] corresponding at 21.05 light-years to 465 a.u.

V1054 Ophiuchi C (vB 8)

vB 8 is the smallest, faintest, and most separated component of the V1054 Ophiuchi system. The projected separation of the red dwarf from the primary triple system is about 220 arcsec,[4][3] corresponding at 21.05 light-years to 1420 a.u. Since it is only three times larger than the projected separation between Gliese 643 and V1054 Ophiuchi A-Bab, and such a small ratio should render the triple system dynamically unstable, it was suggested[3] that the real separation of V1054 Ophiuchi C from V1054 Ophiuchi A-Bab is much larger, at least by a factor of two,[3] i. e. at least 2840 a.u.

In 1984, the apparent detection of an infrared source near vB 8 suggested it had a low mass companion. The low mass of this candidate led to speculation that it may be a brown dwarf; the first such to be detected. This discovery was later found to be spurious, but it produced much interest in this class of astronomical object.[19]

Notes

  1. ↑ Referred to entire V1054 Ophiuchi Bab subsystem.
  2. ↑ From apparent magnitude and parallax.
  3. ↑ Assuming weighted mean parallax 154.96 mas.
  4. ↑ From masses, period and parallax.
  5. ↑ From masses and period. According to Mazeh et al. 2001, of order of 0.05 a. u.
  6. ↑ At least it was not resolved by 2001.

References

  1. ↑ Dal, H. A.; Evren, S. (August 2010). "A New Method for Classifying Flares of UV Ceti Type Stars: Differences Between Slow and Fast Flares". The Astronomical Journal. 140 (2): 483–489. arXiv:1206.5791. Bibcode:2010AJ....140..483D. doi:10.1088/0004-6256/140/2/483. S2CID 119308060. Retrieved 4 February 2022.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 Mazeh, Tsevi; Latham, David W.; Goldberg, Elad; Torres, Guillermo; Stefanik, Robert P.; Henry, Todd J.; Zucker, Shay; Gnat, Orly; Ofek, Eran O. (2001). "Studies of multiple stellar systems - IV. The triple-lined spectroscopic system V1054 Ophiuchi". Monthly Notices of the Royal Astronomical Society. 325 (1): 343–357. arXiv:astro-ph/0102451. Bibcode:2001MNRAS.325..343M. doi:10.1046/j.1365-8711.2001.04419.x. S2CID 16472347.
  4. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 Ségransan, Damien; Delfosse, Xavier; Forveille, Thierry; Beuzit, Jean-Luc; Udry, Stéphane; Perrier, Christian; Mayor, Michel (2000). "Accurate masses of very low mass stars. III. 16 new or improved masses". Astronomy and Astrophysics. 364: 665–673. arXiv:astro-ph/0010585. Bibcode:2000A&A...364..665S.
  5. 1 2 3 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.
  6. 1 2 3 4 Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv:2106.07656. Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID 235435757. 40.
  7. ↑ "HD 152751". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-25.
  8. ↑ Bubar, Eric J.; King, Jeremy R. (August 2010). "Spectroscopic Abundances and Membership in the Wolf 630 Moving Group". The Astronomical Journal. 140 (2): 293–318. arXiv:1005.1205. Bibcode:2010AJ....140..293B. doi:10.1088/0004-6256/140/2/293. S2CID 118455341.
  9. ↑ RECONS CENSUS OF OBJECTS NEARER THAN 10 PARSECS
  10. 1 2 3 Vizier, The Hipparcos and Tycho Catalogues (ESA 1997)
  11. 1 2 Vizier, Stars within 25 pc of the Sun (Woolley+ 1970)
  12. 1 2 Vizier, Nearby Stars, Preliminary 3rd Version (Gliese+ 1991)
  13. 1 2 VizieR, Yale Trigonometric Parallaxes, Fourth Edition (van Altena+ 1995)
  14. ↑ Vizier, Visual binary orbits and masses (Soederhjelm 1999)
  15. 1 2 Vizier, Hipparcos, the New Reduction (van Leeuwen 2007)
  16. ↑ Costa, Edgardo; Méndez, René A.; Jao, W.-C.; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Ianna, Philip A.; Bartlett, Jennifer (2005). "The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation-First Results from the 1.5 m Telescope Program". The Astronomical Journal. 130 (1): 337–349. Bibcode:2005AJ....130..337C. CiteSeerX 10.1.1.573.7563. doi:10.1086/430473. S2CID 12213270.
  17. ↑ DENSE Project. 25 pc White Dwarf Sample (see formulae below)
  18. ↑ THE ONE HUNDRED NEAREST STAR SYSTEMS brought to you by RECONS (Research Consortium On Nearby Stars)
  19. ↑ Reid, Neill I.; Hawley, Suzanne L. (27 November 2013), New Light on Dark Stars: Red Dwarfs, Low-Mass Stars, Brown Dwarfs, Astronomy and Planetary Sciences, Springer Science & Business Media, 2013, p. 344, ISBN 978-1447136637.
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