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50 Persei

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50 Persei
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Perseus
Right ascension 04h 08m 36.61660s[1]
Declination +38° 02′ 23.0488″[1]
Apparent magnitude (V) 5.52[2]
Characteristics
Spectral type F7 V[3]
U−B color index +0.00[2]
B−V color index +0.54[2]
Variable type RS CVn and BY Dra
Astrometry
Radial velocity (Rv)+26.2[4] km/s
Proper motion (μ) RA: +164.10[1] mas/yr
Dec.: −202.60[1] mas/yr
Parallax (π)47.63 ± 0.26 mas[1]
Distance68.5 ± 0.4 ly
(21.0 ± 0.1 pc)
Absolute magnitude (MV)3.87[5]
Details
Mass1.16[6] M☉
Surface gravity (log g)4.35[6] cgs
Temperature6,147[6] K
Metallicity [Fe/H]−0.11[6] dex
Rotational velocity (v sin i)20.81[7] km/s
Age0.60[8] Gyr
Other designations
50 Per, BD+37° 882, FK5 2297, GJ 9145, HD 25998, HIP 19335, HR 1278, SAO 57006.[9]
Database references
SIMBADdata

50 Persei is a star in the constellation Perseus. Its apparent magnitude is 5.52,[2] which is bright enough to be seen with the naked eye. Located around 21.00 parsecs (68.5 ly) distant, it is a White main-sequence star of spectral type F7V,[3] a star that is currently fusing its core hydrogen. In 1998 the star was named a candidate Gamma Doradus variable with a period of 3.05 days,[5] which would means it displays variations in luminosity due to non-radial pulsations in the photosphere. Subsequently, it was classified as a RS Canum Venaticorum and BY Draconis variable by an automated program.[10]

This is probably a binary system with an unseen companion. It is physically associated with the likely binary system HIP 19255, with the two pairs orbiting each other over a time scale of around a million years. The components of HIP 19255 have an angular separation of 3.87″ and the two components orbit each other every 590 years. 50 Persei may share a gravitational association with Capella, even though the two are separated by nearly 15° − equivalent to a distance of 19 ly (5.9 pc).[11]

50 Persei is emitting an infrared excess at a wavelength of 70 μm, suggesting the presence of a circumstellar debris disk. The disk has a temperature of 96±5 K.[8]

References

  1. ^ a b c d e 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.
  2. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", SIMBAD Astronomical Database, Bibcode:1986EgUBV........0M.
  3. ^ a b Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948.
  4. ^ Nordström, B.; et al. (2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs", Publications of the Astronomical Society of Australia, 21 (2): 129–133, Bibcode:2004PASA...21..129N, doi:10.1071/AS04013.
  5. ^ a b Aerts, C.; Eyer, L., Kestens, E. (September 1998), "The discovery of new gamma Doradus stars from the HIPPARCOS mission", Astronomy and Astrophysics, 337: 790–796, Bibcode:1998A&A...337..790A.{{citation}}: CS1 maint: multiple names: authors list (link)
  6. ^ a b c d Chen, Y. Q.; et al. (February 2000), "Chemical composition of 90 F and G disk dwarfs", Astronomy and Astrophysics Supplement, 141 (3): 491–506, arXiv:astro-ph/9912342, Bibcode:2000A&AS..141..491C, doi:10.1051/aas:2000124.
  7. ^ Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725.
  8. ^ a b Beichman, C. A.; et al. (December 2006), "New Debris Disks around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets", The Astrophysical Journal, 652 (2): 1674–1693, arXiv:astro-ph/0611682, Bibcode:2006ApJ...652.1674B, doi:10.1086/508449.
  9. ^ "* 50 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-07-22.{{cite web}}: CS1 maint: postscript (link)
  10. ^ Dubath, P.; Rimoldini, L.; Süveges, M.; Blomme, J.; López, M.; Sarro, L. M.; et al. (2011), "Random forest automated supervised classification of Hipparcos periodic variable stars", Monthly Notices of the Royal Astronomical Society, 414 (3): 2602–17, arXiv:1101.2406, Bibcode:2011MNRAS.414.2602D, doi:10.1111/j.1365-2966.2011.18575.x.{{citation}}: CS1 maint: unflagged free DOI (link)
  11. ^ Shaya, Ed J.; Olling, Rob P. (January 2011), "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalogue", The Astrophysical Journal Supplement, 192 (1): 17, arXiv:1007.0425, Bibcode:2011ApJS..192....2S, doi:10.1088/0067-0049/192/1/2, 2.
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