| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 14m 15.14594s [1] |
| Declination | –59° 06′ 11.6528″ [1] |
| Apparent magnitude (V) | 4.90 [2] + 10.2 [3] |
| Characteristics | |
| Spectral type | F6 V Fe-0.4 [4] |
| B−V color index | 0.489±0.020 [2] |
| Astrometry | |
| Radial velocity (Rv) | −64.0±0.3 [5] km/s |
| Proper motion (μ) |
RA: −249.254
[1]
mas/
yr Dec.: −153.256 [1] mas/ yr |
| Parallax (π) | 55.0143 ± 0.2644 mas [1] |
| Distance | 59.3 ± 0.3
ly (18.18 ± 0.09 pc) |
| Absolute magnitude (MV) | 3.73 [6] |
| Details | |
| HD 114837 A | |
| Mass | 1.14 [7] M☉ |
| Radius | 1.3 [8] R☉ |
| Luminosity | 3.12 [2] L☉ |
| Surface gravity (log g) | 4.21 [9] cgs |
| Temperature | 6,346±80 [9] K |
| Metallicity [Fe/H] | −0.27 [9] dex |
| Rotational velocity (v sin i) | 8.8±3.0 [6] km/s |
| Age | 3.40 [9] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 114837 is a suspected binary star [7] [3] system in the southern constellation of Centaurus. The brighter star is faintly visible to the naked eye with an apparent visual magnitude of 4.90. [2] It has a magnitude 10.2 candidate common proper motion companion at an angular separation of 4.2 ″, as of 2014. [3] The distance to this system, based on an annual parallax shift of 55.0143 ″ as seen from Earth's orbit, [1] is 59.3 light years. It is moving closer with a heliocentric radial velocity of −64 km/s, [5] and will approach to within 21.8 ly in around 240,600 years. [11]
The primary component is an F-type main-sequence star with a stellar classification of F6 V Fe-0.4, [4] showing a mild underabundance of iron in its spectrum. It is about 3.4 [9] billion years old with 1.14 [7] times the mass of the Sun and about 1.3 [8] times the Sun's radius. This star is radiating 3.12 [2] times the Sun's luminosity from its photosphere at an effective temperature of 6,346 K. [9]
- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051.
- ^ 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.
- ^ a b c Chini, R.; et al. (January 2014), "New visual companions of solar-type stars within 25 pc", Monthly Notices of the Royal Astronomical Society, 437 (1): 879–886, arXiv: 1310.2684, Bibcode: 2014MNRAS.437..879C, doi: 10.1093/mnras/stt1953.
- ^ a b Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv: astro-ph/0603770, Bibcode: 2006AJ....132..161G, doi: 10.1086/504637, S2CID 119476992.
- ^ a b 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.
- ^ a b Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv: 1204.2459, Bibcode: 2012A&A...542A.116A, doi: 10.1051/0004-6361/201118724, S2CID 53666672.
- ^ a b c Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z. (2017), "Multiplicity among Solar-type Stars", The Astrophysical Journal, 836: 139, Bibcode: 2017ApJ...836..139F, doi: 10.3847/1538-4357/836/1/139.
- ^ a b Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition", Astronomy and Astrophysics, 367 (2): 521–524, arXiv: astro-ph/0012289, Bibcode: 2001A&A...367..521P, doi: 10.1051/0004-6361:20000451, S2CID 425754.
- ^ a b c d e f Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, arXiv: 1103.4651, Bibcode: 2011A&A...530A.138C, doi: 10.1051/0004-6361/201016276, S2CID 56118016.
- ^ "HD 114837". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-05.
- ^ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv: 1412.3648, Bibcode: 2015A&A...575A..35B, doi: 10.1051/0004-6361/201425221, S2CID 59039482, A35.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 14m 15.14594s [1] |
| Declination | –59° 06′ 11.6528″ [1] |
| Apparent magnitude (V) | 4.90 [2] + 10.2 [3] |
| Characteristics | |
| Spectral type | F6 V Fe-0.4 [4] |
| B−V color index | 0.489±0.020 [2] |
| Astrometry | |
| Radial velocity (Rv) | −64.0±0.3 [5] km/s |
| Proper motion (μ) |
RA: −249.254
[1]
mas/
yr Dec.: −153.256 [1] mas/ yr |
| Parallax (π) | 55.0143 ± 0.2644 mas [1] |
| Distance | 59.3 ± 0.3
ly (18.18 ± 0.09 pc) |
| Absolute magnitude (MV) | 3.73 [6] |
| Details | |
| HD 114837 A | |
| Mass | 1.14 [7] M☉ |
| Radius | 1.3 [8] R☉ |
| Luminosity | 3.12 [2] L☉ |
| Surface gravity (log g) | 4.21 [9] cgs |
| Temperature | 6,346±80 [9] K |
| Metallicity [Fe/H] | −0.27 [9] dex |
| Rotational velocity (v sin i) | 8.8±3.0 [6] km/s |
| Age | 3.40 [9] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 114837 is a suspected binary star [7] [3] system in the southern constellation of Centaurus. The brighter star is faintly visible to the naked eye with an apparent visual magnitude of 4.90. [2] It has a magnitude 10.2 candidate common proper motion companion at an angular separation of 4.2 ″, as of 2014. [3] The distance to this system, based on an annual parallax shift of 55.0143 ″ as seen from Earth's orbit, [1] is 59.3 light years. It is moving closer with a heliocentric radial velocity of −64 km/s, [5] and will approach to within 21.8 ly in around 240,600 years. [11]
The primary component is an F-type main-sequence star with a stellar classification of F6 V Fe-0.4, [4] showing a mild underabundance of iron in its spectrum. It is about 3.4 [9] billion years old with 1.14 [7] times the mass of the Sun and about 1.3 [8] times the Sun's radius. This star is radiating 3.12 [2] times the Sun's luminosity from its photosphere at an effective temperature of 6,346 K. [9]
- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051.
- ^ 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.
- ^ a b c Chini, R.; et al. (January 2014), "New visual companions of solar-type stars within 25 pc", Monthly Notices of the Royal Astronomical Society, 437 (1): 879–886, arXiv: 1310.2684, Bibcode: 2014MNRAS.437..879C, doi: 10.1093/mnras/stt1953.
- ^ a b Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv: astro-ph/0603770, Bibcode: 2006AJ....132..161G, doi: 10.1086/504637, S2CID 119476992.
- ^ a b 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.
- ^ a b Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv: 1204.2459, Bibcode: 2012A&A...542A.116A, doi: 10.1051/0004-6361/201118724, S2CID 53666672.
- ^ a b c Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z. (2017), "Multiplicity among Solar-type Stars", The Astrophysical Journal, 836: 139, Bibcode: 2017ApJ...836..139F, doi: 10.3847/1538-4357/836/1/139.
- ^ a b Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition", Astronomy and Astrophysics, 367 (2): 521–524, arXiv: astro-ph/0012289, Bibcode: 2001A&A...367..521P, doi: 10.1051/0004-6361:20000451, S2CID 425754.
- ^ a b c d e f Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, arXiv: 1103.4651, Bibcode: 2011A&A...530A.138C, doi: 10.1051/0004-6361/201016276, S2CID 56118016.
- ^ "HD 114837". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-07-05.
- ^ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv: 1412.3648, Bibcode: 2015A&A...575A..35B, doi: 10.1051/0004-6361/201425221, S2CID 59039482, A35.
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