47 Ophiuchi

Last updated
47 Ophiuchi
Observation data
Epoch J2000        Equinox J2000
Constellation Ophiuchus [1]
Right ascension 17h 26m 37.88094s [2]
Declination −05° 05′ 11.7500″ [2]
Apparent magnitude  (V)4.54 [3] (4.93 / 5.83) [4]
Characteristics
Spectral type F3V [5]
U−B color index -0.03 [6]
B−V color index +0.39 [6]
Astrometry
Radial velocity (Rv)1.67 ± 0.13 [4]  km/s
Proper motion (μ)RA: -92.50 [2]   mas/yr
Dec.: -43.29 [2]   mas/yr
Parallax (π)33.25 ± 0.25  mas [2]
Distance 98.1 ± 0.7  ly
(30.1 ± 0.2  pc)
Orbit [4]
Period (P)26.27565 ± 0.00004 d
Semi-major axis (a)7.99 ± 0.10 mas
Eccentricity (e)0.481 ± 0.002
Inclination (i)59.5 ± 1.3°
Longitude of the node (Ω)121.8 ± 1.0°
Periastron epoch (T)JD 2448103.380 ± 0.026
Argument of periastron (ω)
(secondary)		27.04 ± 0.54°
Semi-amplitude (K1)
(primary)		46.92 ± 0.40 km/s
Semi-amplitude (K2)
(secondary)		52.80 ± 0.39 km/s
Details [4]
47 Oph A
Mass 1.50 ± 0.06  M☉
Radius 2.06 ± 0.07  R☉
Luminosity 7.80 ± 0.36  L☉
47 Oph B
Mass 1.34 ± 0.06  M☉
Radius 1.36 ± 0.06  R☉
Luminosity3.41 ± 0.25  L☉
C
Mass 70±1 [7]   MJup
Radius 0.93±0.01 [7]   RJup
Surface gravity (log g)5.32±0.01 [7]   cgs
Temperature 1,580±10 [7]   K
Other designations
BD−04° 4275, FK5  647, HD  157950, HIP  85365, HR  6493, SAO  141665
Database references
SIMBAD data

47 Ophiuchi (47 Oph) is a binary star in the constellation Ophiuchus. The combined apparent magnitude of the system is 4.54. [3] The system is located about 98.1 light-years, or 30.1 parsecs away, based on its parallax as measured by Hipparcos. [2]

47 Ophiuchi is a spectroscopic binary: that is, the two stars move fast enough that periodic Doppler shifts in the stars' spectra can be detected. In this case, the two stars have also been resolved using interferometry. [4] The primary star is an F-type main-sequence star, [5] that is 1.5 times the mass of the Sun and around twice as wide. [4] Its companion star is 1.34 times the mass of the Sun, and 1.36 times the radius of the Sun. [4] The two stars orbit each other every 26.3 days, and its orbital eccentricity is 0.481. [4]

The designation 47 Ophiuchi was originally used for the star HR 6496. [8] However, when constellation borders were redrawn, the star fell into the constellation Serpens, and the designation became used for this star, HR 6493, instead. [9]

There is also a wider companion, a brown dwarf which has a projected separation of 8850 astronomical units from 47 Ophiuchi. It is a L-type brown dwarf with a spectral type of L5.5, [10] This object is 70 times more massive than Jupiter and is close to the hydrogen burning limit —dividing line between brown dwarfs and stars— while its radius is only 0.93 that of Jupiter. [7]

Related Research Articles

<span class="mw-page-title-main">70 Ophiuchi</span> Star in the constellation Ophiuchus

70 Ophiuchi is a binary star system located 16.6 light years away from the Earth. It is in the constellation Ophiuchus. At magnitude 4 it appears as a dim star visible to the unaided eye away from city lights.

<span class="mw-page-title-main">Epsilon Sculptoris</span> Binary star system in the constellation Sculptor

Epsilon Sculptoris is a binary star in the constellation Sculptor. It is approximately 91.7 light years from Earth.

<span class="mw-page-title-main">1 Aurigae</span> Star in the constellation Perseus

1 Aurigae is the original name for a star now in the constellation Perseus. It was the first entry in John Flamsteed's catalogue of stars in Auriga. When Eugène Joseph Delporte drew up simplified boundaries for the constellations on behalf of the International Astronomical Union in 1930, 1 Aurigae ended up over the border in Perseus. To avoid confusion, the star may instead be referred to by its Harvard Revised catalogue number, HR 1533.

<span class="mw-page-title-main">67 Ophiuchi</span> Star in the constellation Ophiuchus

67 Ophiuchi is a class B5 Ib star in the constellation Ophiuchus. Its apparent magnitude is 3.93 and it is approximately 2,000 light years away based on spectroscopy. It is considered to be a member of the open cluster Collinder 359.

<span class="mw-page-title-main">Gamma Monocerotis</span> Star in the constellation of Monoceros

γ Monocerotis, Latinised as Gamma Monocerotis, is a binary star system in the equatorial constellation of Monoceros. Based upon an annual parallax shift of 6.55 mas, it is located roughly 500 light years from the Sun. It can be viewed with the naked eye, having an apparent visual magnitude of 3.96. Gamma Monocerotis is moving away from the Sun with a radial velocity of −5 km/s.

20 Ceti is a single star located around 590 light years away in the equatorial constellation of Cetus. It is faintly visible to the naked eye with apparent magnitude is 4.76. The Bright Star Catalogue has this star classified as M0III, matching an aging red giant star that has consumed the hydrogen at its core and expanded. Houk and Swift (1999) listed an earlier class of K5 III. It has around 60 times the Sun's radius and is radiating about 800 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 3,700 K.

<span class="mw-page-title-main">Upsilon Ophiuchi</span> Multiple star in the constellation Ophiuchus

Upsilon Ophiuchi is a triple star system in the equatorial constellation of Ophiuchus. It has a white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.62. The distance to this system is approximately 134 light years based on parallax. It is drifting closer with a radial velocity of −30.6 km/s.

<span class="mw-page-title-main">41 Ophiuchi</span> Binary star system in the constellation Ophiuchus

41 Ophiuchi is a binary star system in the zodiac constellation of Ophiuchus, and is positioned less than half a degree to the south of the celestial equator. It is visible to the naked eye as a faint, orange-hued point of light with a combined apparent visual magnitude of 4.72. The distance to this system is approximately 202 light years based on parallax.

<span class="mw-page-title-main">Tau Ophiuchi</span> Multiple star in the constellation Ophiuchus

Tau Ophiuchi is a multiple star in the constellation Ophiuchus, approximately 167 light years away based on parallax. Its two main components are two yellow-white main sequence stars, A, of magnitude 5.24 and class F2V, and B, of magnitude 5.94 and class F5V, orbiting each other with a period of 257 years and eccentricity around 0.77. A is reported as a spectroscopic binary with a smaller star of 0.29 solar masses orbiting it every 186 days. An additional component, C, has a separation of 100.8" and magnitude 11.28.

<span class="mw-page-title-main">66 Ophiuchi</span> Star in the constellation Ophiuchus

66 Ophiuchi is a binary variable star in the equatorial constellation of Ophiuchus. It has the variable star designation V2048 Ophiuchi, while 66 Ophiuchi is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued point of light with a baseline apparent visual magnitude of 4.60. It is located approximately 650 light years away from the Sun based on parallax, but is drifting closer with a radial velocity of −13 km/s. The star has a peculiar velocity of 13.1±3.2 km/s relative to its neighbors.

<span class="mw-page-title-main">22 Orionis</span> Binary star system in the constellation Orion

22 Orionis is a binary star in the equatorial constellation of Orion. It has the Bayer designation o Orionis, while 22 Orionis is the Flamsteed designation. This system is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.74. It is located approximately 1,100 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +28.80

<span class="mw-page-title-main">51 Orionis</span> Star in the constellation of Orion

51 Orionis is a single star in the equatorial constellation of Orion. It has the Bayer designation b Orionis, while 51 Orionis is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.90. It is located approximately 299 light-years away from the Sun based on parallax, and is drifting further away with a radial velocity of +88 km/s.

<span class="mw-page-title-main">72 Pegasi</span> Binary star system in the constellation Pegasus

72 Pegasi is a binary star system in the northern constellation of Pegasus. It is visible to the naked eye as a faint, orange-hued point of light with a combined apparent visual magnitude of 4.97. The system is located approximately 550 light years away from the Sun, based on parallax, but is drifting closer with a radial velocity of −25 km/s.

<span class="mw-page-title-main">HD 20468</span> K-type bright giant star in the constellation Perseus

HD 20468 is a class K2II star in the constellation Perseus. Its apparent magnitude is 4.82 and it is approximately 1180 light years away based on parallax.

<span class="mw-page-title-main">HD 69142</span> Star in the constellation Puppis

HD 69142 is a class K1II-III star in the constellation Puppis. Its apparent magnitude is 4.44 and it is approximately 298 light years away based on parallax.

<span class="mw-page-title-main">V Puppis</span> Variable star in the constellation Puppis

V Puppis is a star system in the constellation Puppis. Its apparent magnitude is 4.41. There is a binary star system at the center with a B1 dwarf orbiting a B3 subgiant star. They have an orbital period of 1.45 days and a distance of only 15 solar radii apart. However, the system moves back and forth, indicating that there is a massive object orbiting them with a period around 5.47 years. Based on the mass of the object, its lack of a visible spectrum, and circumstellar matter in the system with many heavy elements, it is probably a black hole. However, a follow-up study could not confirm this object, but found signs that there may be a third object which is fainter than the other components.

<span class="mw-page-title-main">HD 65810</span> Star in the constellation Puppis

HD 65810 is a class A2V star in the constellation Puppis. Its apparent magnitude is 4.61 and it is approximately 241 light years away based on parallax.

<span class="mw-page-title-main">HD 59890</span> Star in the constellation Puppis

HD 59890 is a class G3Ib yellow supergiant star in the constellation Puppis. Its apparent magnitude is 4.65 and it is approximately 1,360 light years away based on parallax.

<span class="mw-page-title-main">HD 61831</span> Star in the constellation Puppis

HD 61831 is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.84 and it is approximately 556 light years away based on parallax.

<span class="mw-page-title-main">42 Persei</span> Binary star system in the constellation Perseus

42 Persei is a binary star system in the northern constellation of Perseus. It has the Bayer designation n Persei, while 42 Persei is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.11. It is located around 93 parsecs (302 ly) distant from the Sun, but is drifting closer with a radial velocity of −12.4 km/s.

References

  1. ↑ "Finding the constellation which contains given sky coordinates". djm.cc. 2 August 2008. Archived from the original on 15 August 2019. Retrieved 23 May 2024.
  2. 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.
  3. 1 2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  4. 1 2 3 4 5 6 7 8 Wang, Xiaoli; Hummel, Christian A.; Ren, Shulin; Fu, Yanning (2015). "The Three-Dimensional Orbit and Physical Parameters of 47 Oph". The Astronomical Journal. 149 (3): 110. Bibcode:2015AJ....149..110W. doi: 10.1088/0004-6256/149/3/110 . S2CID   54767546.
  5. 1 2 Abt, H. A. (2009). "MK Classifications of Spectroscopic Binaries". The Astrophysical Journal Supplement Series. 180 (1): 117–118. Bibcode:2009ApJS..180..117A. doi:10.1088/0067-0049/180/1/117. S2CID   122811461.
  6. 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  7. 1 2 3 4 5 Sanghi, Aniket; Liu, Michael C.; Best, William M. J.; Dupuy, Trent J.; Siverd, Robert J.; Zhang, Zhoujian; Hurt, Spencer A.; Magnier, Eugene A.; Aller, Kimberly M.; Deacon, Niall R. (2023-11-08). "Table of Ultracool Fundamental Properties". Zenodo. doi:10.5281/zenodo.10086810.
  8. ↑ Wagman, M. (August 1987). "Flamsteed's Missing Stars". Journal for the History of Astronomy. 18 (3): 212. Bibcode:1987JHA....18..209W. doi:10.1177/002182868701800305. S2CID   118445625.
  9. ↑ Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050. Bibcode:1995yCat.5050....0H.
  10. ↑ Deacon, Niall R.; Liu, Michael C.; Magnier, Eugene A.; Aller, Kimberly M.; Best, William M. J.; Dupuy, Trent; Bowler, Brendan P.; Mann, Andrew W.; Redstone, Joshua A.; Burgett, William S.; Chambers, Kenneth C.; Draper, Peter W.; Flewelling, H.; Hodapp, Klaus W.; Kaiser, Nick (2014-09-01). "Wide Cool and Ultracool Companions to Nearby Stars from Pan-STARRS 1". The Astrophysical Journal. 792 (2): 119. arXiv: 1407.2938 . Bibcode:2014ApJ...792..119D. doi:10.1088/0004-637X/792/2/119. ISSN   0004-637X.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.