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56 Persei
Observation data
Epoch J2000       Equinox J2000
Constellation Perseus
Right ascension 04h 24m 37.46102s [1]
Declination +33° 57′ 35.2908″ [1]
Apparent magnitude (V) 5.77 [2] (5.80 + 15.00 [3] + 9.16 [4] + 11.30 [5])
Characteristics
Spectral type F4V + DA3.1 [3] + F4 [6] + ?
B−V color index 0.400±0.019 [2]
Astrometry
Radial velocity (Rv)−31.8±2.9 [2] km/s
Proper motion (μ) RA: +43.818 [1]  mas/ yr
Dec.: −90.502 [1]  mas/ yr
Parallax (π)23.5093 ± 0.0909  mas [1]
Distance138.7 ± 0.5  ly
(42.5 ± 0.2  pc)
Absolute magnitude (MV)2.73 [2]
Details
56 Per Aa
Mass1.53 [7]  M☉
Radius1.97+0.05
−0.11 [1]  R☉
Luminosity7.166±0.034 [8]  L☉
Surface gravity (log g)4.32±0.14 [8]  cgs
Temperature6,629±225 [8]  K
Metallicity [Fe/H]−0.11±0.08 [9]  dex
Age1.811 [8]  Gyr
56 Per Ab
Mass0.90±0.12 [10]  M☉
Surface gravity (log g)8.46±0.2 [10]  cgs
Temperature16,420±420 [10]  K
Other designations
56 Per, BD+33° 854, HD 27786, HIP 20591, HR 1379, SAO 57216 [11]
Database references
SIMBAD data

56 Persei is at least a triple star [10] and possibly a quadruple star [3] system in the northern constellation of Perseus. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.77. [2] The system is located 139 light-years (42.5 pc) distant from the Sun based on parallax, [1] but is drifting closer with a radial velocity of −32 km/s. [2]

The main component is a binary system [12] with an orbital period of 47.3 years and a semimajor axis of 17.60  AU. The primary, designated component Aa, is an F-type main-sequence star with a stellar classification of F4V, a star that is currently fusing its core hydrogen. [7] It is 1.8 [8] billion years old with 1.5 [7] times the mass of the Sun and twice [1] the Sun's radius. It is radiating 7 [8] times the luminosity of the Sun from its photosphere at an effective temperature of 6,629 K. [8]

The companion, component Ab, is a hydrogen–rich white dwarf star with a class of DA3.1, [3] having begun its main sequence life with more mass than the current primary and thus evolved into a compact star more rapidly. It now has 90% of the Sun's mass – much higher than the 0.6 M☉ for an average white dwarf – and an effective temperature of 16,420 K; [10] contributing an ultraviolet excess to the system. [3]

Component B shares a common linear motion through space with the primary, and thus may form a third member of the system. This star has 0.84 times the mass of the Sun and a projected separation of 178.2  AU from the primary. [7] The Washington Double Star Catalogue has it classified as a double star, with a magnitude 11.30 companion at an angular separation of 0.60″ along a position angle of 292°, as of 2002. [5]

References

  1. ^ a b c d e f g h 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. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e f 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.
  3. ^ a b c d e Holberg, J. B.; et al. (2013), "Where are all the Sirius-like binary systems?", Monthly Notices of the Royal Astronomical Society, 435 (3): 2077, arXiv: 1307.8047, Bibcode: 2013MNRAS.435.2077H, doi: 10.1093/mnras/stt1433.
  4. ^ Fabricius, C.; et al. (2002), "The Tycho double star catalogue", Astronomy and Astrophysics, 384: 180–189, Bibcode: 2002A&A...384..180F, doi: 10.1051/0004-6361:20011822.
  5. ^ a b Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920
  6. ^ Cannon, Annie J.; Mayall, Margaret Walton (1949), "The Henry Draper extension. II", Annals of Harvard College Observatory, 112: 1–295, Bibcode: 1949AnHar.112....1C.
  7. ^ a b c d Tokovinin, A.; Kiyaeva, O. (2015), "Eccentricity distribution of wide binaries", Monthly Notices of the Royal Astronomical Society, 456 (2): 2070, arXiv: 1512.00278, Bibcode: 2016MNRAS.456.2070T, doi: 10.1093/mnras/stv2825.
  8. ^ a b c d e f g David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv: 1501.03154, Bibcode: 2015ApJ...804..146D, doi: 10.1088/0004-637X/804/2/146, S2CID  33401607.
  9. ^ Gáspár, András; Rieke, George H.; Ballering, Nicholas (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 171, arXiv: 1604.07403, Bibcode: 2016ApJ...826..171G, doi: 10.3847/0004-637X/826/2/171, S2CID  119241004.
  10. ^ a b c d e Landsman, Wayne; et al. (March 1996), "The White-Dwarf Companions of 56 Persei and HR 3643", Publications of the Astronomical Society of the Pacific, 108: 250, arXiv: astro-ph/9512117, Bibcode: 1996PASP..108..250L, doi: 10.1086/133718, S2CID  14398914.
  11. ^ "54 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-21.
  12. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID  14878976.
Retrieved from " https://en.wikipedia.org/?title=56_Persei&oldid=1235041753"
From Wikipedia, the free encyclopedia
56 Persei
Observation data
Epoch J2000       Equinox J2000
Constellation Perseus
Right ascension 04h 24m 37.46102s [1]
Declination +33° 57′ 35.2908″ [1]
Apparent magnitude (V) 5.77 [2] (5.80 + 15.00 [3] + 9.16 [4] + 11.30 [5])
Characteristics
Spectral type F4V + DA3.1 [3] + F4 [6] + ?
B−V color index 0.400±0.019 [2]
Astrometry
Radial velocity (Rv)−31.8±2.9 [2] km/s
Proper motion (μ) RA: +43.818 [1]  mas/ yr
Dec.: −90.502 [1]  mas/ yr
Parallax (π)23.5093 ± 0.0909  mas [1]
Distance138.7 ± 0.5  ly
(42.5 ± 0.2  pc)
Absolute magnitude (MV)2.73 [2]
Details
56 Per Aa
Mass1.53 [7]  M☉
Radius1.97+0.05
−0.11 [1]  R☉
Luminosity7.166±0.034 [8]  L☉
Surface gravity (log g)4.32±0.14 [8]  cgs
Temperature6,629±225 [8]  K
Metallicity [Fe/H]−0.11±0.08 [9]  dex
Age1.811 [8]  Gyr
56 Per Ab
Mass0.90±0.12 [10]  M☉
Surface gravity (log g)8.46±0.2 [10]  cgs
Temperature16,420±420 [10]  K
Other designations
56 Per, BD+33° 854, HD 27786, HIP 20591, HR 1379, SAO 57216 [11]
Database references
SIMBAD data

56 Persei is at least a triple star [10] and possibly a quadruple star [3] system in the northern constellation of Perseus. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.77. [2] The system is located 139 light-years (42.5 pc) distant from the Sun based on parallax, [1] but is drifting closer with a radial velocity of −32 km/s. [2]

The main component is a binary system [12] with an orbital period of 47.3 years and a semimajor axis of 17.60  AU. The primary, designated component Aa, is an F-type main-sequence star with a stellar classification of F4V, a star that is currently fusing its core hydrogen. [7] It is 1.8 [8] billion years old with 1.5 [7] times the mass of the Sun and twice [1] the Sun's radius. It is radiating 7 [8] times the luminosity of the Sun from its photosphere at an effective temperature of 6,629 K. [8]

The companion, component Ab, is a hydrogen–rich white dwarf star with a class of DA3.1, [3] having begun its main sequence life with more mass than the current primary and thus evolved into a compact star more rapidly. It now has 90% of the Sun's mass – much higher than the 0.6 M☉ for an average white dwarf – and an effective temperature of 16,420 K; [10] contributing an ultraviolet excess to the system. [3]

Component B shares a common linear motion through space with the primary, and thus may form a third member of the system. This star has 0.84 times the mass of the Sun and a projected separation of 178.2  AU from the primary. [7] The Washington Double Star Catalogue has it classified as a double star, with a magnitude 11.30 companion at an angular separation of 0.60″ along a position angle of 292°, as of 2002. [5]

References

  1. ^ a b c d e f g h 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. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e f 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.
  3. ^ a b c d e Holberg, J. B.; et al. (2013), "Where are all the Sirius-like binary systems?", Monthly Notices of the Royal Astronomical Society, 435 (3): 2077, arXiv: 1307.8047, Bibcode: 2013MNRAS.435.2077H, doi: 10.1093/mnras/stt1433.
  4. ^ Fabricius, C.; et al. (2002), "The Tycho double star catalogue", Astronomy and Astrophysics, 384: 180–189, Bibcode: 2002A&A...384..180F, doi: 10.1051/0004-6361:20011822.
  5. ^ a b Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920
  6. ^ Cannon, Annie J.; Mayall, Margaret Walton (1949), "The Henry Draper extension. II", Annals of Harvard College Observatory, 112: 1–295, Bibcode: 1949AnHar.112....1C.
  7. ^ a b c d Tokovinin, A.; Kiyaeva, O. (2015), "Eccentricity distribution of wide binaries", Monthly Notices of the Royal Astronomical Society, 456 (2): 2070, arXiv: 1512.00278, Bibcode: 2016MNRAS.456.2070T, doi: 10.1093/mnras/stv2825.
  8. ^ a b c d e f g David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv: 1501.03154, Bibcode: 2015ApJ...804..146D, doi: 10.1088/0004-637X/804/2/146, S2CID  33401607.
  9. ^ Gáspár, András; Rieke, George H.; Ballering, Nicholas (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 171, arXiv: 1604.07403, Bibcode: 2016ApJ...826..171G, doi: 10.3847/0004-637X/826/2/171, S2CID  119241004.
  10. ^ a b c d e Landsman, Wayne; et al. (March 1996), "The White-Dwarf Companions of 56 Persei and HR 3643", Publications of the Astronomical Society of the Pacific, 108: 250, arXiv: astro-ph/9512117, Bibcode: 1996PASP..108..250L, doi: 10.1086/133718, S2CID  14398914.
  11. ^ "54 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-21.
  12. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID  14878976.
Retrieved from " https://en.wikipedia.org/?title=56_Persei&oldid=1235041753"

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