  | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 42m 14.91569s [1] |
| Declination | +40° 11′ 38.1898″ [1] |
| Apparent magnitude (V) | 4.94 [2] |
| Characteristics | |
| Spectral type | F9 V [3] |
| U−B color index | +0.08 [2] |
| B−V color index | +0.56 [2] |
| Astrometry | |
| Radial velocity (Rv) | 5.20 [4] km/s |
| Proper motion (μ) |
RA: −17.20
[1]
mas/
yr Dec.: −183.30 [1] mas/ yr |
| Parallax (π) | 41.34 ± 0.43 mas [1] |
| Distance | 78.9 ± 0.8
ly (24.2 ± 0.3 pc) |
| Orbit | |
| Period (P) | 330.98 [5] d |
| Semi-major axis (a) | 53.18 [6] mas |
| Eccentricity (e) | 0.663 [5] |
| Inclination (i) | 127.17 [6]° |
| Details | |
| 12 Per A | |
| Mass | 1.382±0.019 [5] M☉ |
| Radius | 1.55 [5] R☉ |
| Luminosity | 3.02 [5] L☉ |
| Surface gravity (log g) | 4.20±0.10 [5] cgs |
| Temperature | 6195±200 [5] K |
| Metallicity [Fe/H] | ≥0.35 [5] dex |
| Rotational velocity (v sin i) | 13 [7] km/s |
| Age | 1.12 [5] Gyr |
| 12 Per B | |
| Mass | 1.240±0.017 [5] M☉ |
| Radius | 1.31 [5] R☉ |
| Luminosity | 1.86 [5] L☉ |
| Surface gravity (log g) | 4.30±0.10 [5] cgs |
| Temperature | 6000±200 [5] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
12 Persei (12 Per) is a double-lined spectroscopic binary star system in the northern constellation Perseus. Its combined apparent magnitude is 4.94, [2] which means it can be viewed with the naked eye. Based upon parallax measurements, this system is about 79 light years away from the Sun. [1]
The magnitude difference between the two components is estimated to be 0.51. Based upon this, the primary has a mass around 138% of the Sun, 155% of the Sun's radius, and shines with three times the Sun's luminosity. The smaller secondary component is also larger than the Sun, with 124% of the Sun's mass, 131% of the radius of the Sun, and has 186% of the Sun's luminosity. [5] The stellar classification of the primary is F9 V, [3] which suggests it is an F-type main sequence star. The pair have an estimated age of just over a billion years. [5]
The pair orbit each other with a period of 331 days and an eccentricity of 0.663. [5] The semimajor axis of their orbit is 1.27 AU, which means the inner stability radius for a hypothetical planet orbiting the pair would be at 4.35 AU. This lies outside the habitability zone for this system. [9]
- ^ a b c d e f 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.
- ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", SIMBAD Astronomical Database, Bibcode: 1986EgUBV........0M.
- ^ a b Abt, Helmut A. (2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–118, Bibcode: 2009ApJS..180..117A, doi: 10.1088/0067-0049/180/1/117, S2CID 122811461.
- ^ Pourbaix, D.; et al. (September 2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424: 727–732, arXiv: astro-ph/0406573, Bibcode: 2004A&A...424..727P, doi: 10.1051/0004-6361:20041213, S2CID 119387088.
- ^ a b c d e f g h i j k l m n o p q Leushin, V. V.; Kuznetsov, M. K. (2008), "Chemical Composition and Evolutionary Status of Spectral Binary Star 12 Per", Odessa Astronomical Publications, 21: 57, Bibcode: 2008OAP....21...57L.
- ^ a b Bagnuolo, William G. Jr.; et al. (June 2006), "The star 12 Persei and separated fringe packet binaries (SFPB)", in Monnier, John D.; Schöller, Markus; Danchi, William C. (eds.), Advances in Stellar Interferometry, Proceedings of the SPIE, vol. 6268, pp. 62682T, Bibcode: 2006SPIE.6268E..2TB, doi: 10.1117/12.672275, S2CID 124256072, 62682T.
- ^ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1): 1, Bibcode: 1970CoAsi.239....1B.
- ^ "* 12 Per", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2016-07-21
- ^ Jaime, Luisa G.; et al. (September 2014), "Habitable zones with stable orbits for planets around binary systems", Monthly Notices of the Royal Astronomical Society, 443 (1): 260–274, arXiv: 1401.1006, Bibcode: 2014MNRAS.443..260J, doi: 10.1093/mnras/stu1052.
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 42m 14.91569s [1] |
| Declination | +40° 11′ 38.1898″ [1] |
| Apparent magnitude (V) | 4.94 [2] |
| Characteristics | |
| Spectral type | F9 V [3] |
| U−B color index | +0.08 [2] |
| B−V color index | +0.56 [2] |
| Astrometry | |
| Radial velocity (Rv) | 5.20 [4] km/s |
| Proper motion (μ) |
RA: −17.20
[1]
mas/
yr Dec.: −183.30 [1] mas/ yr |
| Parallax (π) | 41.34 ± 0.43 mas [1] |
| Distance | 78.9 ± 0.8
ly (24.2 ± 0.3 pc) |
| Orbit | |
| Period (P) | 330.98 [5] d |
| Semi-major axis (a) | 53.18 [6] mas |
| Eccentricity (e) | 0.663 [5] |
| Inclination (i) | 127.17 [6]° |
| Details | |
| 12 Per A | |
| Mass | 1.382±0.019 [5] M☉ |
| Radius | 1.55 [5] R☉ |
| Luminosity | 3.02 [5] L☉ |
| Surface gravity (log g) | 4.20±0.10 [5] cgs |
| Temperature | 6195±200 [5] K |
| Metallicity [Fe/H] | ≥0.35 [5] dex |
| Rotational velocity (v sin i) | 13 [7] km/s |
| Age | 1.12 [5] Gyr |
| 12 Per B | |
| Mass | 1.240±0.017 [5] M☉ |
| Radius | 1.31 [5] R☉ |
| Luminosity | 1.86 [5] L☉ |
| Surface gravity (log g) | 4.30±0.10 [5] cgs |
| Temperature | 6000±200 [5] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
12 Persei (12 Per) is a double-lined spectroscopic binary star system in the northern constellation Perseus. Its combined apparent magnitude is 4.94, [2] which means it can be viewed with the naked eye. Based upon parallax measurements, this system is about 79 light years away from the Sun. [1]
The magnitude difference between the two components is estimated to be 0.51. Based upon this, the primary has a mass around 138% of the Sun, 155% of the Sun's radius, and shines with three times the Sun's luminosity. The smaller secondary component is also larger than the Sun, with 124% of the Sun's mass, 131% of the radius of the Sun, and has 186% of the Sun's luminosity. [5] The stellar classification of the primary is F9 V, [3] which suggests it is an F-type main sequence star. The pair have an estimated age of just over a billion years. [5]
The pair orbit each other with a period of 331 days and an eccentricity of 0.663. [5] The semimajor axis of their orbit is 1.27 AU, which means the inner stability radius for a hypothetical planet orbiting the pair would be at 4.35 AU. This lies outside the habitability zone for this system. [9]
- ^ a b c d e f 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.
- ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", SIMBAD Astronomical Database, Bibcode: 1986EgUBV........0M.
- ^ a b Abt, Helmut A. (2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–118, Bibcode: 2009ApJS..180..117A, doi: 10.1088/0067-0049/180/1/117, S2CID 122811461.
- ^ Pourbaix, D.; et al. (September 2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424: 727–732, arXiv: astro-ph/0406573, Bibcode: 2004A&A...424..727P, doi: 10.1051/0004-6361:20041213, S2CID 119387088.
- ^ a b c d e f g h i j k l m n o p q Leushin, V. V.; Kuznetsov, M. K. (2008), "Chemical Composition and Evolutionary Status of Spectral Binary Star 12 Per", Odessa Astronomical Publications, 21: 57, Bibcode: 2008OAP....21...57L.
- ^ a b Bagnuolo, William G. Jr.; et al. (June 2006), "The star 12 Persei and separated fringe packet binaries (SFPB)", in Monnier, John D.; Schöller, Markus; Danchi, William C. (eds.), Advances in Stellar Interferometry, Proceedings of the SPIE, vol. 6268, pp. 62682T, Bibcode: 2006SPIE.6268E..2TB, doi: 10.1117/12.672275, S2CID 124256072, 62682T.
- ^ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1): 1, Bibcode: 1970CoAsi.239....1B.
- ^ "* 12 Per", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2016-07-21
- ^ Jaime, Luisa G.; et al. (September 2014), "Habitable zones with stable orbits for planets around binary systems", Monthly Notices of the Royal Astronomical Society, 443 (1): 260–274, arXiv: 1401.1006, Bibcode: 2014MNRAS.443..260J, doi: 10.1093/mnras/stu1052.
| Stars |
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|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
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Star clusters |
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| Nebulae |
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| Galaxies |
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