Astronomy:Iota Persei

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Short description: F-type or G-type main sequence star in the constellation Perseus
Iota Persei
Perseus constellation map.svg
Red circle.svg
Location of ι Persei (circled)
Observation data
Equinox J2000.0]] (ICRS)
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[1] mas
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. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.  Vizier catalog entry
  2. ↑ 2.0 2.1 2.2 2.3 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, doi:10.1093/mnras/172.3.667, Bibcode: 1975MNRAS.172..667J. 
  3. ↑ 3.0 3.1 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, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K 
  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, doi:10.1086/504637, Bibcode: 2006AJ....132..161G. 
  5. ↑ 5.0 5.1 Nidever, David L. et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series 141 (2): 503–522, doi:10.1086/340570, Bibcode: 2002ApJS..141..503N. 
  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, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 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. doi:10.1086/430500. Bibcode: 2005ApJS..159..141V.  Note: see VizieR catalogie J/ApJS/159/141 .
  8. ↑ 8.0 8.1 8.2 8.3 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, doi:10.1088/0004-637X/746/1/101, Bibcode: 2012ApJ...746..101B . See Table 10.
  9. ↑ 9.0 9.1 Kovtyukh, V. V. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics 411 (3): 559–564. doi:10.1051/0004-6361:20031378. Bibcode: 2003A&A...411..559K. 
  10. ↑ 10.0 10.1 10.2 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. doi:10.1086/591785. Bibcode: 2008ApJ...687.1264M. 
  11. ↑ "iot Per". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=iot+Per. 
  12. ↑ 12.0 12.1 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  13. ↑ Mason, B. D. et al. (2014), The Washington Visual Double Star Catalog, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M 
  14. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日

External links



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