Iota Persei
Location of ι Persei (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 03h 09m 04.02s[1]
Declination +49° 36′ 47.8″[1]
Apparent magnitude (V) 4.062[2]
Characteristics
Spectral type G0V[3] or F9.5 V[4]
U−B color index +0.119[2]
B−V color index +0.595[2]
Astrometry
Radial velocity (Rv)+49.22±0.08[5] km/s
Proper motion (μ) RA: +1262.41[1] mas/yr
Dec.: −91.50[1] mas/yr
Parallax (π)94.87 ± 0.23 mas[1]
Distance34.38 ± 0.08 ly
(10.54 ± 0.03 pc)
Absolute magnitude (MV)3.94[6]
Details
Mass1.35±0.08[7] M☉
Radius1.412±0.009[8] R☉
Luminosity2.181±0.032[8] L☉
Surface gravity (log g)4.31[7] cgs
Temperature5,963±5.1[9] K
Metallicity [Fe/H]+0.09[10] dex
Rotational velocity (v sin i)4.1[7] km/s
Age3.2–4.1[7][10] Gyr
Other designations
ι Per, BD+49°857, FK5 112, GC 3740, HD 19373, HIP 14632, HR 937, SAO 38597, PPM 45875, CCDM J03091+4936A, WDS J03091+4937A[11]
Database references
SIMBADdata

ι Persei, Latinized as Iota Persei, is a single[12] star in the northern constellation Perseus. This object is visible to the naked eye as a faint, yellow-white hued point of light with an apparent visual magnitude of 4.1.[2] It is located 34 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +49 km/s.[5] Iota Persei has a relatively high proper motion across the sky.[1]

ι Persei in optical light

This is a late F- or early G-type main-sequence star with a stellar classification of around G0V.[3] It is about 3–4[7][10] billion years old and is spinning slowly with a projected rotational velocity of 4 km/s.[7] The star has 1.4[7] times the mass of the Sun and 1.4[8] times the Sun's radius. It is radiating more than double[8] the luminosity of the Sun from its photosphere at an effective temperature of 5,963 K.[9]

There is a 12.4-magnitude line-of-sight companion star that is not believed to be gravitationally associated with Iota Persei.[12] This object is located at an angular separation of 154.4″ from the primary along a position angle of 125°, as of 2014.[13]

Naming

In Chinese, 大陵 (Dà Líng), meaning Mausoleum, refers to an asterism consisting of ι Persei, 9 Persei, τ Persei, κ Persei, β Persei, ρ Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for ι Persei itself is 大陵三 (Dà Líng sān, English: the Third Star of Mausoleum).[14]

References

  1. 1 2 3 4 5 6 7 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. Vizier catalog entry
  2. 1 2 3 4 Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants", Monthly Notices of the Royal Astronomical Society, 172 (3): 667–679, Bibcode:1975MNRAS.172..667J, doi:10.1093/mnras/172.3.667.
  3. 1 2 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", The Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373
  4. ↑ 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.
  5. 1 2 Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID 51814894.
  6. ↑ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
  7. 1 2 3 4 5 6 7 Valenti, Jeff A.; Fischer, Debra A. (July 2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi:10.1086/430500. Note: see VizieR catalogie J/ApJS/159/141 Archived 2016-08-06 at the Wayback Machine.
  8. 1 2 3 4 Boyajian, Tabetha S.; et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal, 746 (1): 101, arXiv:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101, S2CID 18993744. See Table 10.
  9. 1 2 Kovtyukh, V. V.; et al. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics. 411 (3): 559–564. arXiv:astro-ph/0308429. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. S2CID 18478960.
  10. 1 2 3 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
  11. ↑ "iot Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-06.
  12. 1 2 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.
  13. ↑ Mason, B. D.; et al. (2014), The Washington Visual Double Star Catalog, Bibcode:2001AJ....122.3466M, doi:10.1086/323920
  14. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.